研究者データベース

高橋 幸弘(タカハシ ユキヒロ)
理学研究院 地球惑星科学部門 宇宙惑星科学分野
教授

基本情報

所属

  • 理学研究院 地球惑星科学部門 宇宙惑星科学分野

職名

  • 教授

学位

  • 博士(理学)(東北大学)

ホームページURL

J-Global ID

研究キーワード

  • 雷放電   スプライト   エルブス   電離圏   TLE   ELF   地球ガンマ線   超高層大気   中間圏   TGF   中層大気   北欧   地上観測   磁気圏   リモートセンシング   台風   ISUAL   大学衛星   ダウンバースト   インドネシア   ブラジル   超小型衛星   スウェーデン   豪雨災害   発光現象   北欧観測   マイクロサテライト   人工衛星   ミャンマー   大気化学   

研究分野

  • 自然科学一般 / 宇宙惑星科学
  • 環境・農学 / 環境動態解析
  • 社会基盤(土木・建築・防災) / 防災工学
  • 社会基盤(土木・建築・防災) / 防災工学
  • 自然科学一般 / 大気水圏科学
  • 自然科学一般 / 固体地球科学
  • 人文・社会 / 地理学

職歴

  • 2009年 - 2015年 北海道大学 理学(系)研究科(研究院) 教授

研究活動情報

論文

  • Masataka Imai, Junichi Kurihara, Toru Kouyama, Toshinori Kuwahara, Shinya Fujita, Yuji Sakamoto, Yuji Sato, Sei-Ichi Saitoh, Takafumi Hirata, Hirokazu Yamamoto, Yukihiro Takahashi
    Sensors 21 7 2429 - 2429 2021年04月01日 
    Radiometric calibration utilizing the Moon as a reference source is termed as lunar calibration. It is a useful method for evaluating the performance of optical sensors onboard satellites orbiting the Earth. Lunar calibration provides sufficient radiometric calibration opportunities without requiring any special equipment, and is suitable for nano/microsatellites. This study applies lunar calibration to a multispectral sensor, Ocean Observation Camera (OOC), on board a microsatellite named Rapid International Scientific Experiment Satellite. Simulating the brightness of the Moon based on the RObotic Lunar Observatory and SELENE/Spectrum Profiler models, sensitivity degradation was proven to be negligible in any of the four spectral bands of the OOC with the sensor temperature correction. A bluing trend in the OOC’s sensor sensitivity was revealed, indicating a shorter observation wavelength shows larger irradiance. Comparing the top-of-atmosphere reflectance of Railroad Valley Playa with the Radiometric Calibration Network dataset revealed that the derived calibration parameter from the lunar calibration was valid for correcting the bluing trend in the visible range. Although the lunar and vicarious calibration parameters for the infrared band were unexpectedly inconsistent, lunar calibration could potentially contribute toward estimating the contaminated background radiance in the Earth observation images.
  • 高橋 幸弘, 今井 正尭, 佐藤 光輝
    日本惑星科学会誌遊星人 30 2 72 - 73 日本惑星科学会 2021年 

    ⾦星に雷放電の有無に決着をつけるべく,世界初の惑星雷放電発光観測装置LACは⾦星周回軌道で観測を継続してきました.観測開始から約4年になる2020年3月1日に,最初にして唯一(2021年4月末日現在)の突発的な発光現象を記録しました.果たして雷はあったのでしょうか?

  • K. Bandholnopparat, M. Sato, T. Adachi, T. Ushio, Y. Takahashi
    Journal of Geophysical Research: Atmospheres 125 23 2020年12月16日
  • Masataka Imai, Toru Kouyama, Junichi Kurihara, Toshinori Kuwahara, Shinya Fujita, Yuji Sakamoto, Sei Ichi Saitoh, Takafumi Hirata, Yukihiro Takahashi
    International Geoscience and Remote Sensing Symposium (IGARSS) 6222 - 6225 2020年09月26日 
    Radiometric calibration with the Moon (called the lunar calibration) is a promising method for evaluating the performance of instruments onboard satellites orbiting around the Earth. In particular, the lunar calibration can provide inflight radiometric calibration opportunities for nano/microsatellites whose priorities are technical demonstrations and scientific observations during rather a short lifetime. In this study, we have applied the lunar calibration to a recently launched microsatellite named RISESAT. RISESAT had observed the Moon every month for a half year after the launch with an onboard instrument OOC. By simulating the Moon brightness for each observation based on the ROLO and SELENE/SP Moon models, we succeeded to measure < 2 % of a small degradation in four months. Further comparison of the observation and the simulation irradiance of the Moon revealed the bluing trend in the OOC's inter-band ratio.
  • T. Yamada, T. O. Sato, T. Adachi, H. Winkler, K. Kuribayashi, R. Larsson, N. Yoshida, Y. Takahashi, M. Sato, A. B. Chen, R. R. Hsu, Y. Nakano, T. Fujinawa, S. Nara, Y. Uchiyama, Y. Kasai
    Geophysical Research Letters 47 3 2020年02月16日
  • Tetsuya Fukuhara, Yuji Sakamoto, Toshinori Kuwahara, Nobuo Sugimura, Kazuya Yoshida, Yukihiro Takahashi
    IEEE GEOSCIENCE AND REMOTE SENSING LETTERS 17 2 332 - 336 2020年02月 
    The commercial thermal infrared camera mounting the uncooled microbolometer array (UMBA), which detects thermal wavelengths from 8 to 14 mu m , was modified for space use and applied to the small earth-observing satellite called Rising-2. The satellite was launched in 2014, and the camera successfully took 17 of the cloud top and 3 of the land images from the sun-synchronous orbit. Observed brightness temperatures based on the reference data acquired in the laboratory before the launch have been compared with verified products derived from the Japanese meteorological satellite called MTSAT-2, and we confirmed that the UMBA could sense brightness temperature distribution of the target. The demonstration of the commercial thermal infrared camera in orbit would innovate in the development of space instruments as a new approach.
  • KURIHARA Junichi, IP Wing-Huen, KUWAHARA Toshinori, FUJITA Shinya, SATO Yuji, HANYU Kosuke, SAKAL Morokot, MURATA Yu, TOMIO Hannah, TAKAHASHI Yukihiro
    TRANSACTIONS OF THE JAPAN SOCIETY FOR AERONAUTICAL AND SPACE SCIENCES, AEROSPACE TECHNOLOGY JAPAN 18 5 186 - 191 一般社団法人 日本航空宇宙学会 2020年 

    Nano/microsatellites play a significant role in Earth observation with the emerging constellation of high spatial resolution satellites. However, there are technological limitations in their spectral resolution. In this paper, we present an overview of a high spatial resolution multispectral sensor, the High-Precision Telescope (HPT), which was developed originally for the RISING-2 microsatellite and subsequently improved for the Rapid International Scientific Experiment Satellite (RISESAT) microsatellite. The HPTs were also installed on the DIWATA-1 and DIWATA-2 microsatellites, but they are different from those in the RISING-2 and RISESAT microsatellites in terms of number of spectral bands. The HPT on the RISESAT has the largest number of spectral bands in a series of the high spatial resolution multispectral sensors. The RISESAT was successfully launched by the Epsilon-4 launch vehicle on 18 January 2019. The preliminary results obtained in the commissioning phase of the operation demonstrate the expected performance of the HPT.

  • Junichi Kurihara, Tetsuro Ishida, Yukihiro Takahashi
    Unmanned Aerial Vehicle: Applications in Agriculture and Environment 25 - 38 2020年
  • Masataka Imai, Toru Kouyama, Yukihiro Takahashi, Atsushi Yamazaki, Shigeto Watanabe, Manabu Yamada, Takeshi Imamura, Takehiko Satoh, Masato Nakamura, Shin‐ya Murakami, Kazunori Ogohara, Takeshi Horinouchi
    Journal of Geophysical Research: Planets 2019年10月31日 [査読有り][通常論文]
  • Ralph D. Lorenz, Masataka Imai, Yukihiro Takahashi, Mitsuteru Sato, Atsushi Yamazaki, Takao M. Sato, Takeshi Imamura, Takehiko Satoh, Masato Nakamura
    Geophysical Research Letters 46 14 7955 - 7961 American Geophysical Union ({AGU}) 2019年07月 [査読有り][通常論文]
  • Toshihiko NAKANO, Makoto TAGUCHI, Yasuhiro SHOJI, Mao TAKAMURA, Daiki SUNAGUCHI, Masataka IMAI, Makoto WATANABE, Yukihiro TAKAHASHI, Yuji SAKAMOTO, Kazuya YOSHIDA
    TRANSACTIONS OF THE JAPAN SOCIETY FOR AERONAUTICAL AND SPACE SCIENCES, AEROSPACE TECHNOLOGY JAPAN 17 1 51 - 56 2019年
  • Yukihiro Takahashi, Mitsuteru Sato, Masataka Imai, Ralph Lorenz, Yoav Yair, Karen Aplin, Georg Fischer, Masato Nakamura, Nobuaki Ishii, Takumi Abe, Takehiko Satoh, Takeshi Imamura, Chikako Hirose, Makoto Suzuki, George L. Hashimoto, Naru Hirata, Atsushi Yamazaki, Takao M. Sato, Manabu Yamada, Shin-ya Murakami, Yukio Yamamoto, Tetsuya Fukuhara, Kazunori Ogohara, Hiroki Ando, Ko-ichiro Sugiyama, Hiroki Kashimura, Shoko Ohtsuki
    Earth, Planets and Space 70 1 2018年12月01日 [査読有り][通常論文]
     
    The existence of lightning discharges in the Venus atmosphere has been controversial for more than 30 years, with many positive and negative reports published. The lightning and airglow camera (LAC) onboard the Venus orbiter, Akatsuki, was designed to observe the light curve of possible flashes at a sufficiently high sampling rate to discriminate lightning from other sources and can thereby perform a more definitive search for optical emissions. Akatsuki arrived at Venus during December 2016, 5 years following its launch. The initial operations of LAC through November 2016 have included a progressive increase in the high voltage applied to the avalanche photodiode detector. LAC began lightning survey observations in December 2016. It was confirmed that the operational high voltage was achieved and that the triggering system functions correctly. LAC lightning search observations are planned to continue for several years.
  • Start of lightning hunting by LAC / Akatsuki
    Takahashi, Y, M. Sato, M. Imai, R. Lorenz, Y. Yair, K. Aplin, G. Fischer, M. Nakamura, N. Ishii, T. Abe, T. Satoh, T. Imamura, C. Hirose, M. Suzuki, G. L. Hashimoto, N. Hitrata, A. Yamazaki, T. M. Sato, M. Yamada, S. Murakami, Y. Yamamoto, T. Fukuhara, K. Ogohara, H. Ando, K. Sugiyama, H. Kashimura, S. Ohtsuki
    Earth, Planets and Space 70:88 2018年05月 [査読有り][通常論文]
  • Junichi Kurihara, Yukihiro Takahashi, Yuji Sakamoto, Toshinori Kuwahara, Kazuya Yoshida
    Sensors 18 2 619 - 619 2018年02月18日 
    Although nano/microsatellites have great potential as remote sensing platforms, the spatial and spectral resolutions of an optical payload instrument are limited. In this study, a high spatial resolution multispectral sensor, the High-Precision Telescope (HPT), was developed for the RISING-2 microsatellite. The HPT has four image sensors: three in the visible region of the spectrum used for the composition of true color images, and a fourth in the near-infrared region, which employs liquid crystal tunable filter (LCTF) technology for wavelength scanning. Band-to-band image registration methods have also been developed for the HPT and implemented in the image processing procedure. The processed images were compared with other satellite images, and proven to be useful in various remote sensing applications. Thus, LCTF technology can be considered an innovative tool that is suitable for future multi/hyperspectral remote sensing by nano/microsatellites.
  • HPT: A High Spatial Resolution Multispectral Sensor for Microsatellite Remote Sensing
    Kurihara Junichi, Takahashi Yukihiro, Sakamoto Yuji, KUWAHARA Toshinori, Kazuya Yoshida
    Sensors 619 18 1 - 11 2018年02月 [査読有り][通常論文]
  • Tsurushima, D, N. Honma, F. Tsuchiya, M. Sato, Y. Takahashi
    電気学会論文誌B(電力・エネルギー部門誌) 138 5 339 - 345 2018年 [査読有り][通常論文]
  • Katsuhama, N, M. Imai, N. Naruse, Y. Takahashi
    J. Remote Sensing Letters 9 1186 - 1194 2018年 [査読有り][通常論文]
  • Tetsuya Fukuhara, Toru Kouyama, Soushi Kato, Ryosuke Nakamura, Yukihiro Takahashi, Hiroaki Akiyama
    IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING 55 8 4314 - 4324 2017年08月 [査読有り][通常論文]
     
    The thermal infrared camera with the uncooled microbolometer array based on commercial products has been developed in a laboratory of a Japanese university and mounted to a 50-kg class small satellite specialized for discovering wildfire. It has been launched in 2014 and successfully detected considerable hotspots not only wildfire but also volcanoes. Brightness temperature derived from observation has been verified, and the scale of observed wildfire has been provisionally presumed; the smallest wildfire ever detected has a flame zone less than similar to 300 m(2) and the fire radiative power = similar to 35.4 mW. It is 1/30th the size of the initial requirement estimated in the design process. Our thermal infrared camera developed in a short time with low cost has attained enough ability to discover small wildfire which is suppressive at initial attack.
  • Mitsuteru Sato, Toru Adachi, Tomoo Ushio, Takeshi Morimoto, Masayuki Kikuchi, Hiroshi Kikuchi, Makoto Suzuki, Atsushi Yamazaki, Yukihiro Takahashi, Ryohei Ishida, Yuji Sakamoto, Kazuya Yoshida, Yasuhide Hobara
    TERRESTRIAL ATMOSPHERIC AND OCEANIC SCIENCES 28 4 545 - 561 2017年08月 [査読有り][通常論文]
     
    The Global Lightning and Sprite Measurements on the Japanese Experiment Module (JEM-GLIMS) started continuous nadir observations of lightning and transient luminous events (TLEs) at the International Space Station (ISS) in November 2012 and completed the observations in August 2015. As JEM-GLIMS uses the nadir observation technique, the JEM-GLIMS optical instruments simultaneously measure both incomparably intense lightning emissions and weak sprite emissions. We adopted combined data analytical methods to distinguish between these two types of emissions: (1) a subtraction of the wideband LSI-1 image from the narrowband LSI-2 image, (2) a calculation of the intensity ratio between different photometer channels, and (3) an estimation of the charge moment change (CMC) of the suspected sprite-producing CG discharge. This report presents as a case study one sprite event detected at 19: 50: 40.30580 UT on 28 September 2013 and identified using the above analytical methods. From the results derived from detailed data analyses, we judged that the optical emission measured by LSI-2 is a sprite emission. We carried out the geometry conversion toward the LSI-1 and subtracted images and found that the sprite emission location shifts by 3.5 km from the peak lightning emission location, which agree with the previous reports. The detailed horizontal distributions of sprites and the relationship between the sprite location and the parent lightning location are quantitatively revealed for the first time.
  • Identification of sprites in JEM-GLIMS nadir observations and their spatial distributions
    Sato, M, T. Adachi, T. Ushio, T. Morimoto, M. Kikuchi, H. Kikuchi, M. Suzuki, A. Yamazaki, Y. Takahashi, R. Ishida, Y. Sakamoto, K. Yoshida, Y. Hobara
    Terrestrial, Atmospheric and Oceanic Sciences 28 545 - 561 2017年08月 [査読有り][通常論文]
  • Hiroko Miyahara, Chika Higuchi, Toshio Terasawa, Ryuho Kataoka, Mitsuteru Sato, Yukihiro Takahashi
    ANNALES GEOPHYSICAE 35 3 2017年04月 [査読有り][通常論文]
     
    A signal of the 27-day solar rotational period is often observed in cloud and lightning activities over the globe. Here we provide evidence of the 27-day periodicity of lightning activity in Japan using daily observational records of lightning for AD1989-2015. The 27-day period is detected with 4.2 standard deviations, but only in wide-area lightning activity covering more than a 10(5) km(2). The 27-day signal is more prominent around the maxima of solar decadal cycles.
  • Yoshitaka Uchida, Kawawa Banda, Toru Hamamoto, Yui Yoshii, Kabenuka Munthali, Mukuka Mwansa, Moses Mukuka, Mubanga Mutale, Nobuyasu Naruse, Yukihiro Takahashi
    bioRxiv 2017年01月 [査読無し][通常論文]
  • Studies of dust and discharges around a Martian rover with onboard hazard analyses using electromagnetic and acoustic wave measurements
    Yamamoto, M, M. Sato, K. Ishisaka, Y. Takahashi, K. Ogohara, M. Kamogawa, H. Miyamoto
    Ttansactions of the Japan Society for Aeronatical and Space Sciences 14 30 41 - 45 2016年10月 [査読有り][通常論文]
  • H. U. Frey, S. B. Mende, S. E. Harris, H. Heetderks, Y. Takahashi, H. -T. Su, R. -R. Hsu, A. B. Chen, H. Fukunishi, Y. -S. Chang, L. -C. Lee
    JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS 121 8 8134 - 8145 2016年08月 [査読有り][通常論文]
     
    The Imager for Sprites and Upper Atmospheric Lightning (ISUAL) was the first specifically dedicated instrument to observe lightning-induced transient luminous events (TLE): sprites, elves, halos, and gigantic jets from space. The Imager is an intensified CCD system operating in the visible wavelength region with a filter wheel to select from six positions with filters. The Imager has a 5 degrees x 20 degrees (vertical times horizontal) field of view. The spectrophotometer (SP) is populated with six photometers with individual filters for emissions from the far ultraviolet to the near infrared. An array photometer with two channels operating in the blue and red provides altitude profiles of the emission over 16 altitude bins each. The Associated Electronics Package (AEP) controls instrument functions and interfaces with the spacecraft. ISUAL was launched 21 May 2004 into a Sun-synchronous 890 km orbit on the Formosat-2 satellite and has successfully been collecting data ever since. ISUAL is running on the nightside of the orbit and is pointed to the east of the orbit down toward the limb. The instrument runs continuously and writes data to a circular buffer. Whenever the SP detects a sudden signal increase above a preset threshold, a trigger signal is generated that commands the system to keep the data for about 400 ms starting from similar to 50 ms before the trigger. Over its lifetime of similar to 11 years the system recorded thousands of TLE and also successfully observed aurora and airglow.
  • Adachi Toru, Sato Mitsuteru, Ushio Tomoo, Yamazaki Atsushi, Suzuki Makoto, Kikuchi Masayuki, Takahashi Yukihiro, Inan Umran S, Linscott Ivan, Hobara Yasuhide, Frey Harald U, Mende Stephen B, Chen Alfred B, Hsu Rue-Ron, Kusunoki Kenichi
    JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS 145 85 - 97 2016年07月 [査読有り][通常論文]
     
    © 2016 Elsevier Ltd. We propose a new technique to identify the occurrence of lightning and transient luminous events (TLEs) using multicolor photometric data obtained by space borne nadir measurements. We estimate the spectral characteristics of lightning and TLEs by converting the optical data obtained by the ISUAL limb experiment to the GLIMS nadir geometry. We find that the estimated spectral shapes of TLE-accompanied lightning are clearly different from those of pure lightning. The obtained results show that (1) the intensity of FUV signals and (2) the ratio of 337/red (609-753 nm) spectral irradiance are useful to identify the occurrence of TLEs. The occurrence probabilities of TLEs are 10%, 40%, 80%, in the case of lightning events having the 337/red spectral irradiance ratio of 0.95, 2.95, 14.79, respectively. By using the 60% criterion of the 337/red ratio and the existence of FUV emissions, we classify the 1039 GLIMS-observed lightning events into 828 pure lightning and 211 TLE-accompanied lightning. Since the GLIMS trigger level is adjusted to observe extremely-bright events, the occurrence probability of TLEs obtained here most probably reflects the characteristics of energetic lightning. The estimated global map is consistent with previously determined distributions: the highest activities of lightning and TLEs are found over the North/South American continents, African continent, and Asian maritime regions. While the absolute occurrence number of pure lightning and TLE-accompanied lightning are found to maximize in the equatorial region, the occurrence probability of TLEs possibly increase somewhat in the mid-latitude region. Since the occurrence probabilities of TLEs are higher over the ocean than over land, it is likely that the GLIMS-observed TLEs are due primarily to elves which tends to occur more frequently over the ocean.
  • Masato Nakamura, Takeshi Imamura, Nobuaki Ishii, Takumi Abe, Yasuhiro Kawakatsu, Chikako Hirose, Takehiko Satoh, Makoto Suzuki, Munetaka Ueno, Atsushi Yamazaki, Naomoto Iwagami, Shigeto Watanabe, Makoto Taguchi, Tetsuya Fukuhara, Yukihiro Takahashi, Manabu Yamada, Masataka Imai, Shoko Ohtsuki, Kazunori Uemizu, George L. Hashimoto, Masahiro Takagi, Yoshihisa Matsuda, Kazunori Ogohara, Naoki Sato, Yasumasa Kasaba, Toru Kouyama, Naru Hirata, Ryosuke Nakamura, Yukio Yamamoto, Takeshi Horinouchi, Masaru Yamamoto, Yoshi-Yuki Hayashi, Hiroki Kashimura, Ko-ichiro Sugiyama, Takeshi Sakanoi, Hiroki Ando, Shin-ya Murakami, Takao M. Sato, Seiko Takagi, Kensuke Nakajima, Javier Peralta, Yeon Joo Lee, Junichi Nakatsuka, Tsutomu Ichikawa, Kozaburo Inoue, Tomoaki Toda, Hiroyuki Toyota, Sumitaka Tachikawa, Shinichiro Narita, Tomoko Hayashiyama, Akiko Hasegawa, Yukio Kamata
    Earth, Planets and Space 68 1 Springer Science $\mathplus$ Business Media 2016年05月 [査読有り][通常論文]
     
    AKATSUKI is the Japanese Venus Climate Orbiter that was designed to investigate the climate system of Venus. The orbiter was launched on May 21, 2010, and it reached Venus on December 7, 2010. Thrust was applied by the orbital maneuver engine in an attempt to put AKATSUKI into a westward equatorial orbit around Venus with a 30-h orbital period. However, this operation failed because of a malfunction in the propulsion system. After this failure, the spacecraft orbited the Sun for 5 years. On December 7, 2015, AKATSUKI once again approached Venus and the Venus orbit insertion was successful, whereby a westward equatorial orbit with apoapsis of similar to 440,000 km and orbital period of 14 days was initiated. Now that AKATSUKI's long journey to Venus has ended, it will provide scientific data on the Venusian climate system for two or more years. For the purpose of both decreasing the apoapsis altitude and avoiding a long eclipse during the orbit, a trim maneuver was performed at the first periapsis. The apoapsis altitude is now similar to 360,000 km with a periapsis altitude of 1000-8000 km, and the period is 10 days and 12 h. In this paper, we describe the details of the Venus orbit insertion-revenge 1 (VOI-R1) and the new orbit, the expected scientific information to be obtained at this orbit, and the Venus images captured by the onboard 1-mu m infrared camera, ultraviolet imager, and long-wave infrared camera 2 h after the successful initiation of the VOI-R1.
  • M. Sato, M. Mihara, T. Adachi, T. Ushio, T. Morimoto, M. Kikuchi, H. Kikuchi, M. Suzuki, A. Yamazaki, Y. Takahashi, U. Inan, I. Linscott, R. Ishida, Y. Sakamoto, K. Yoshida, Y. Hobara
    JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES 121 7 3171 - 3194 2016年04月 [査読有り][通常論文]
     
    Global Lightning and Sprite Measurements on Japanese Experiment Module (JEM-GLIMS) started the nadir observations of lightning discharges and transient luminous events (TLEs) from the International Space Station (ISS) since November 2012. In the nadir observations, JEM-GLIMS optical instruments have to simultaneously detect incomparably intense lightning emissions and weak TLE emissions. To distinguish TLEs, especially sprite events, from lightning events, combined data analytical methods are adopted: (1) a subtraction of the wideband camera image from the narrowband camera image, (2) a calculation of the intensity ratio between different photometer channels, and (3) an estimation of the polarization and charge moment changes for the TLE-producing lightning discharges. We succeeded in identifying numbers of sprite events using the combined analytical methods, and here we report three sprite events detected by JEM-GLIMS as a case study. In the subtracted images, sprite emissions are located over the area of the sprite-producing lightning emissions. However, these sprites and sprite-producing lightning discharges did not occur at the nadir point of the ISS. For this reason, the geometry conversion of the sprite and sprite-producing lightning emissions as observed from the point just over the sprite-producing lightning discharges is performed. In the geometry-converted images, the locations of the sprite emissions are clearly displaced by 8-20km from the peak positions of the sprite-producing lightning emissions. Thus, the first quantitative spatial distributions of sprites and sprite-producing lightning discharges from the JEM-GLIMS nadir observations are revealed.
  • 成瀬 延康, 池田 文人, 山田 邦雅, 飯田 直弘, 高橋 幸弘, 鈴木 誠
    高等教育ジャーナル-高等教育と生涯学習- 23 23 101 - 107 北海道大学高等教育推進機構 2016年03月 [査読有り][通常論文]
  • 高橋 幸弘
    計測と制御 55 9 792 - 796 公益社団法人 計測自動制御学会 2016年
  • Yasuhiro SHOJI, Makoto TAGUCHI, Toshihiko NAKANO, Atsunori MAEDA, Masataka IMAI, Yuya GOUDA, Makoto WATANABE, Yukihiro TAKAHASHI, Yuji SAKAMOTO, Kazuya YOSHIDA
    TRANSACTIONS OF THE JAPAN SOCIETY FOR AERONAUTICAL AND SPACE SCIENCES, AEROSPACE TECHNOLOGY JAPAN 14 ists30 Pk_95 - Pk_102 2016年
  • Imai Masataka, Takahashi Yukihiro, Watanabe Makoto, Kouyama Toru, Watanabe Shigeto, Gouda Shuhei, Gouda Yuya
    Icarus 278 204 - 214 2016年 [査読有り][通常論文]
     
    A planetary-scale bright and dark UV feature, known as the "Y-feature," rotates around Venus with a period of 4-5 days and has been long-time interpreted as planetary waves. When assuming this, its rotation period and spatial structure might help to understand the propagation of the planetary-scale waves and find out their role in the acceleration-deceleration of the zonal wind speed, which is essential for understanding the super-rotation of the planet. The rotation period of the UV feature varied over the course of observation by the Pioneer Venus orbiter. However, in previous explorations of Venus such as Pioneer Venus and Venus Express, the spacecraft were operated in nearly fixed inertial space. As a result, the periodicity variations on sub-yearly timescales (one Venusian year is 224 Earth days) were obscured by the limitations of continuous dayside observations. We newly conducted six periods of ground -based Venus imaging observations at 365 nm from mid-August 2013 to the end of June 2014. Each observation period spanned over half or one month, enabling long-term monitoring of Venus' atmosphere above the equator region. Distributions of the relative brightness were obtained from the equatorial (EQ) to mid-latitudinal regions in both hemispheres, and from the cyclical variations of these distributions we deduced the rotation periods of the UV features of the cloud tops brightness. The relative brightness exhibited periods of 5.2 and 3.5 days above 90% of significance. The relative intensities of these two significant components also seemed subject to temporal variations. Although the 3.5-day component considered persists throughout the observation periods, its dominance over the longer period varied in a cyclic fashion. The prevailing first significant mode seems to change from 5.2-day waves to 3.5-day waves in about nine months, which is clearly inconsistent with the Venusian year. Clear periodic perturbations, indicating stability of the planetary-scale UV-feature, were observed only in the presence of single longer or shorter periodic waves. During the transition periods of dominant-wave changing, the amplitude of the relative brightness was largely changed. This can be explained by the deformation of the Y-shaped UV feature as observed by Pioneer Venus in 1979. (C) 2016 Elsevier Inc. All rights reserved.
  • 清水千春, 佐藤光輝, 本郷保二, 土屋史紀, 高橋幸弘
    電気学会論文誌 2016年 [査読有り][通常論文]
     
    in press
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    EXPERIMENTAL ASTRONOMY 40 1 315 - 326 2015年11月 [査読有り][通常論文]
     
    Space-based detectors for the study of extreme energy cosmic rays (EECR) are being prepared as a promising new method for detecting highest energy cosmic rays. A pioneering space device - the "tracking ultraviolet set-up" (TUS) - is in the last stage of its construction and testing. The TUS detector will collect preliminary data on EECR in the conditions of a space environment, which will be extremely useful for planning the major JEM-EUSO detector operation.
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. de Donato, C. de la Taille, C. de Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    EXPERIMENTAL ASTRONOMY 40 1 91 - 116 2015年11月 [査読有り][通常論文]
     
    The JEM-EUSO telescope will be, after calibration, a very accurate instrument which yields the number of received photons from the number of measured photo-electrons. The project is in phase A (demonstration of the concept) including already operating prototype instruments, i.e. many parts of the instrument have been constructed and tested. Calibration is a crucial part of the instrument and its use. The focal surface (FS) of the JEM-EUSO telescope will consist of about 5000 photo-multiplier tubes (PMTs), which have to be well calibrated to reach the required accuracy in reconstructing the air-shower parameters. The optics system consists of 3 plastic Fresnel (double-sided) lenses of 2.5 m diameter. The aim of the calibration system is to measure the efficiencies (transmittances) of the optics and absolute efficiencies of the entire focal surface detector. The system consists of 3 main components: (i) Pre-flight calibration devices on ground, where the efficiency and gain of the PMTs will be measured absolutely and also the transmittance of the optics will be. (ii) On-board relative calibration system applying two methods: a) operating during the day when the JEM-EUSO lid will be closed with small light sources on board. b) operating during the night, together with data taking: the monitoring of the background rate over identical sites. (iii) Absolute in-flight calibration, again, applying two methods: a) measurement of the moon light, reflected on high altitude, high albedo clouds. b) measurements of calibrated flashes and tracks produced by the Global Light System (GLS). Some details of each calibration method will be described in this paper.
  • The JEM-EUSO collaboration, including, M. Sato
    Experimental Astronomy 40 1 183 - 214 2015年11月 [査読有り][通常論文]
     
    The Extreme Universe Space Observatory (EUSO) on-board the Japanese Experimental Module (JEM) of the International Space Station aims at the detection of ultra high energy cosmic rays from space. The mission consists of a UV telescope which will detect the fluorescence light emitted by cosmic ray showers in the atmosphere. The mission, currently developed by a large international collaboration, is designed to be launched within this decade. In this article, we present the reconstruction of the energy of the observed events and we also address the X (max) reconstruction. After discussing the algorithms developed for the energy and X (max) reconstruction, we present several estimates of the energy resolution, as a function of the incident angle, and energy of the event. Similarly, estimates of the X (max) resolution for various conditions are presented.
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashini, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotovi, A. Zuccaro Marchi
    EXPERIMENTAL ASTRONOMY 40 1 61 - 89 2015年11月 [査読有り][通常論文]
     
    The Extreme Universe Space Observatory on the Japanese Experiment Module (JEM-EUSO) on board the International Space Station (ISS) is the first space-based mission worldwide in the field of Ultra High-Energy Cosmic Rays (UHECR). For UHECR experiments, the atmosphere is not only the showering calorimeter for the primary cosmic rays, it is an essential part of the readout system, as well. Moreover, the atmosphere must be calibrated and has to be considered as input for the analysis of the fluorescence signals. Therefore, the JEM-EUSO Space Observatory is implementing an Atmospheric Monitoring System (AMS) that will include an IR-Camera and a LIDAR. The AMS Infrared Camera is an infrared, wide FoV, imaging system designed to provide the cloud coverage along the JEM-EUSO track and the cloud top height to properly achieve the UHECR reconstruction in cloudy conditions. In this paper, an updated preliminary design status, the results from the calibration tests of the first prototype, the simulation of the instrument, and preliminary cloud top height retrieval algorithms are presented.
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, D. Finco, M. Flamini, C. Fornarodo, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircakja, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    EXPERIMENTAL ASTRONOMY 40 1 135 - 152 2015年11月 [査読有り][通常論文]
     
    The JEM-EUSO (Extreme Universe Space Observatory on-board the Japanese Experiment Module) mission will conduct extensive air shower (EAS) observations on the International Space Station (ISS). Following the ISS orbit, JEM-EUSO will experience continuous changes in the atmospheric conditions, including cloud presence. The influence of clouds on space-based observation is, therefore, an important topic to investigate from both EAS property and cloud climatology points of view. In the present work, the impact of clouds on the apparent profile of EAS is demonstrated through the simulation studies, taking into account the JEM-EUSO instrument and properties of the clouds. These results show a dependence on the cloud-top altitude and optical depth of the cloud. The analyses of satellite measurements on the cloud distribution indicate that more than 60 % of the cases allow for conventional EAS observation, and an additional similar to 20 % with reduced quality. The combination of the relevant factors results in an effective trigger aperture of EAS observation similar to 72 %, compared to the one in the clear atmosphere condition.
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchari, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itowen, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wl Odarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    EXPERIMENTAL ASTRONOMY 40 1 281 - 299 2015年11月 [査読有り][通常論文]
     
    EUSO-Balloon is a pathfinder for JEM-EUSO, the Extreme Universe Space Observatory which is to be hosted on-board the International Space Station. As JEM-EUSO is designed to observe Ultra-High Energy Cosmic Rays (UHECR)-induced Extensive Air Showers (EAS) by detecting their ultraviolet light tracks "from above", EUSO-Balloon is a nadir-pointing UV telescope too. With its Fresnel Optics and Photo-Detector Module, the instrument monitors a 50 km(2) ground surface area in a wavelength band of 290-430 nm, collecting series of images at a rate of 400,000 frames/sec. The objectives of the balloon demonstrator are threefold: a) perform a full end-to-end test of a JEM-EUSO prototype consisting of all the main subsystems of the space experiment, b) measure the effective terrestrial UV background, with a spatial and temporal resolution relevant for JEM-EUSO. c) detect tracks of ultraviolet light from near space for the first time. The latter is a milestone in the development of UHECR science, paving the way for any future space-based UHECR observatory. On August 25, 2014, EUSO-Balloon was launched from Timmins Stratospheric Balloon Base (Ontario, Canada) by the balloon division of the French Space Agency CNES. From a float altitude of 38 km, the instrument operated during the entire astronomical night, observing UV-light from a variety of ground-covers and from hundreds of simulated EASs, produced by flashers and a laser during a two-hour helicopter under-flight.
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. de Donato, C. de la Taille, C. de Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de Los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    EXPERIMENTAL ASTRONOMY 40 1 3 - 17 2015年11月 [査読有り][通常論文]
     
    The Extreme Universe Space Observatory on board the Japanese Experiment Module of the International Space Station, JEM-EUSO, is being designed to search from space ultra-high energy cosmic rays. These are charged particles with energies from a few 10(19) eV to beyond 10(20) eV, at the very end of the known cosmic ray energy spectrum. JEM-EUSO will also search for extreme energy neutrinos, photons, and exotic particles, providing a unique opportunity to explore largely unknown phenomena in our Universe. The mission, principally based on a wide field of view (60 degrees) near-UV telescope with a diameter of similar to 2.5 m, will monitor the earth's atmosphere at night, pioneering the observation from space of the ultraviolet tracks (290-430 nm) associated with giant extensive air showers produced by ultra-high energy primaries propagating in the earth's atmosphere. Observing from an orbital altitude of similar to 400 km, the mission is expected to reach an instantaneous geometrical aperture of A (g e o) a parts per thousand yen 2 x 10(5) km(2) sr with an estimated duty cycle of similar to 20 %. Such a geometrical aperture allows unprecedented exposures, significantly larger than can be obtained with ground-based experiments. In this paper we briefly review the history of space-based search for ultra-high energy cosmic rays. We then introduce the special issue of Experimental Astronomy devoted to the various aspects of such a challenging enterprise. We also summarise the activities of the on-going JEM-EUSO program.
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csoma, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fern'andez-G'omez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. Gonz'alez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hern'andez Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgr'o, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. L'opez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los R'ios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orlea'nski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Pr'evot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodr'iguez, M. D. Rodr'iguez Fr'ias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczy'nski, M. D. Sabau, G. S'aez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. S'anchez, A. Santangelo, L. Santiago Cr'uz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva L'opez, J. Sledd, K. Slomi'nska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Vald'es-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov
    EXPERIMENTAL ASTRONOMY 40 1 179 - 181 2015年11月 [査読有り][通常論文]
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galiciaga, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    EXPERIMENTAL ASTRONOMY 40 1 239 - 251 2015年11月 [査読有り][通常論文]
     
    The main goal of the JEM-EUSO experiment is the study of Ultra High Energy Cosmic Rays (UHECR, 10(19)-10(21) e V), but the method which will be used (detection of the secondary light emissions induced by cosmic rays in the atmosphere) allows to study other luminous phenomena. The UHECRs will be detected through the measurement of the emission in the range between 290 and 430 m, where some part of Transient Luminous Events (TLEs) emission also appears. This work discusses the possibility of using the JEM-EUSO Telescope to get new scientific results on TLEs. The high time resolution of this instrument allows to observe the evolution of TLEs with great precision just at the moment of their origin. The paper consists of four parts: review of the present knowledge on the TLE, presentation of the results of the simulations of the TLE images in the JEM-EUSO telescope, results of the Russian experiment Tatiana-2 and discussion of the possible progress achievable in this field with JEM-EUSO as well as possible cooperation with other space projects devoted to the study of TLE - TARANIS and ASIM. In atmospheric physics, the study of TLEs became one of the main physical subjects of interest after their discovery in 1989. In the years 1992 - 1994 detection was performed from satellite, aircraft and space shuttle and recently from the International Space Station. These events have short duration (milliseconds) and small scales (km to tens of km) and appear at altitudes 50 - 100 km. Their nature is still not clear and each new experimental data can be useful for a better understanding of these mysterious phenomena.
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, L. Anchordoqui, V. Andreev, A. Anzalone, Y. Arai, K. Asano, M. Ave Pernas, P. Baragatti, P. Barrillon, T. Batsch, J. Bayer, R. Bechini, T. Belenguer, R. Bellotti, K. Belov, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, N. Blanc, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, C. Catalano, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, D. Cline, V. Connaughton, L. Conti, G. Cordero, H. J. Crawford, R. Cremonini, S. Csorna, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, C. De Santis, L. del Peral, A. Dell'Oro, N. De Simone, M. Di Martino, G. Distratis, F. Dulucq, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, D. Finco, M. Flamini, C. Fornaro, A. Franceschi, J. Fujimoto, M. Fukushima, P. Galeotti, G. Garipov, J. Geary, G. Gelmini, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, D. Ikeda, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, M. Karus, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, A. Kusenko, E. Kuznetsov, M. Lacombe, C. Lachaud, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, D. Maravilla, L. Marcelli, A. Marini, O. Martinez, G. Masciantonio, K. Mase, R. Matev, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, A. Monaco, D. Monnier-Ragaigne, J. A. Morales de los Rios, C. Moretto, V. S. Morozenko, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, T. Napolitano, D. Naumov, R. Nava, A. Neronov, K. Nomoto, T. Nonaka, T. Ogawa, S. Ogio, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, M. I. Panasyuk, E. Parizot, I. H. Park, H. W. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, S. Perez Cano, T. Peter, P. Picozza, T. Pierog, L. W. Piotrowski, S. Piraino, Z. Plebaniak, A. Pollini, P. Prat, G. Prevot, H. Prieto, M. Putis, P. Reardon, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, M. Roth, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, H. Sagawa, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, H. Tokuno, T. Tomida, N. Tone, S. Toscano, F. Trillaud, R. Tsenov, Y. Tsunesada, K. Tsuno, T. Tymieniecka, Y. Uchihori, M. Unger, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, M. Yu. Zotov, A. Zuccaro Marchi
    EXPERIMENTAL ASTRONOMY 40 1 45 - 60 2015年11月 [査読有り][通常論文]
     
    The JEM-EUSO telescope will detect Ultra-High Energy Cosmic Rays (UHECRs) from space, detecting the UV Fluorescence Light produced by Extensive Air Showers (EAS) induced by the interaction of the cosmic rays with the earth's atmosphere. The capability to reconstruct the properties of the primary cosmic ray depends on the accurate measurement of the atmospheric conditions in the region of EAS development. The Atmospheric Monitoring (AM) system of JEM-EUSO will host a LIDAR, operating in the UV band, and an Infrared camera to monitor the cloud cover in the JEM-EUSO Field of View, in order to be sensitive to clouds with an optical depth tau a parts per thousand yen 0.15 and to measure the cloud top altitude with an accuracy of 500 m and an altitude resolution of 500 m.
  • Imai, M, Takahashi, Y, Watanabe, S, Watanabe, M. an
    European Planetary Science Congress EPSC2015 - 523 2015年10月 [査読無し][通常論文]
  • M. Sato, T. Ushio, T. Morimoto, M. Kikuchi, H. Kikuchi, T. Adachi, M. Suzuki, A. Yamazaki, Y. Takahashi, U. Inan, I. Linscott, R. Ishida, Y. Sakamoto, K. Yoshida, Y. Hobara, T. Sano, T. Abe, M. Nakamura, H. Oda, Z. -I. Kawasaki
    JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES 120 9 3822 - 3851 2015年05月 [査読有り][通常論文]
     
    Global Lightning and Sprite Measurements on Japanese Experiment Module (JEM-GLIMS) is a space mission to conduct the nadir observations of lightning discharges and transient luminous events (TLEs). The main objectives of this mission are to identify the horizontal distribution of TLEs and to solve the occurrence conditions determining the spatial distribution. JEM-GLIMS was successfully launched and started continuous nadir observations in 2012. The global distribution of the detected lightning events shows that most of the events occurred over continental regions in the local summer hemisphere. In some events, strong far-ultraviolet emissions have been simultaneously detected with N-2 1P and 2P emissions by the spectrophotometers, which strongly suggest the occurrence of TLEs. Especially, in some of these events, no significant optical emission was measured by the narrowband filter camera, which suggests the occurrence of elves, not sprites. The VLF receiver also succeeded in detecting lightning whistlers, which show clear falling-tone frequency dispersion. Based on the optical data, the time delay from the detected lightning emission to the whistlers was identified as approximate to 10ms, which can be reasonably explained by the wave propagation with the group velocity of whistlers. The VHF interferometer conducted the spaceborne interferometric observations and succeeded in detecting VHF pulses. We observed that the VHF pulses are likely to be excited by the lightning discharge possibly related with in-cloud discharges and measured with the JEM-GLIMS optical instruments. Thus, JEM-GLIMS provides the first full set of optical and electromagnetic data of lightning and TLEs obtained by nadir observations from space.
  • M. Sato, T. Ushio, T. Morimoto, M. Kikuchi, H. Kikuchi, T. Adachi, M. Suzuki, A. Yamazaki, Y. Takahashi, U. Inan, I. Linscott, R. Ishida, Y. Sakamoto, K. Yoshida, Y. Hobara, T. Sano, T. Abe, M. Nakamura, H. Oda, Z. I. Kawasaki
    Journal of Geophysical Research 120 9 3822 - 3851 2015年 [査読有り][通常論文]
     
    © 2015. American Geophysical Union. All Rights Reserved. Global Lightning and Sprite Measurements on Japanese Experiment Module (JEM-GLIMS) is a space mission to conduct the nadir observations of lightning discharges and transient luminous events (TLEs). The main objectives of this mission are to identify the horizontal distribution of TLEs and to solve the occurrence conditions determining the spatial distribution. JEM-GLIMS was successfully launched and started continuous nadir observations in 2012. The global distribution of the detected lightning events shows that most of the events occurred over continental regions in the local summer hemisphere. In some events, strong far-ultraviolet emissions have been simultaneously detected with N2 1P and 2P emissions by the spectrophotometers, which strongly suggest the occurrence of TLEs. Especially, in some of these events, no significant optical emission was measured by the narrowband filter camera, which suggests the occurrence of elves, not sprites. The VLF receiver also succeeded in detecting lightning whistlers, which show clear falling-tone frequency dispersion. Based on the optical data, the time delay from the detected lightning emission to the whistlers was identified as ~10 ms, which can be reasonably explained by the wave propagation with the group velocity of whistlers. The VHF interferometer conducted the spaceborne interferometric observations and succeeded in detecting VHF pulses. We observed that the VHF pulses are likely to be excited by the lightning discharge possibly related with in-cloud discharges and measured with the JEM-GLIMS optical instruments. Thus, JEM-GLIMS provides the first full set of optical and electromagnetic data of lightning and TLEs obtained by nadir observations from space.
  • Masato Nakamura, Yasuhiro Kawakatsu, Chikako Hirose, Takeshi Imamura, Nobuaki Ishii, Takumi Abe, Atsushi Yamazaki, Manabu Yamada, Kazunori Ogohara, Kazunori Uemizu, Tetsuya Fukuhara, Shoko Ohtsuki, Takehiko Satoh, Makoto Suzuki, Munetaka Ueno, Junichi Nakatsuka, Naomoto Iwagami, Makoto Taguchi, Shigeto Watanabe, Yukihiro Takahashi, George L. Hashimoto, Hiroki Yamamoto
    Acta Astronautica 93 384 - 389 2014年 
    Japanese Venus Climate Orbiter/AKATSUKI was proposed in 2001 with strong support by international Venus science community and approved as an ISAS (The Institute of Space and Astronautical Science) mission soon after the proposal. The mission life we expected was more than two Earth years in Venus orbit. AKATSUKI was successfully launched at 06:58:22JST on May 21, 2010, by H-IIA F17. After the separation from H-IIA, the telemetry from AKATSUKI was normally detected by DSN Goldstone station (10:00JST) and the solar cell paddles' deployment was confirmed. After a successful cruise, the malfunction happened on the propulsion system during the Venus orbit insertion (VOI) on Dec. 7, 2010. The engine shut down before the planned reduction in speed to achieve. The spacecraft did not enter the Venus orbit but entered an orbit around the Sun with a period of 203 days. Most of the fuel still had remained, but the orbital maneuvering engine was found to be broken and unusable. However, we have found an alternate way of achieving orbit by using only the reaction control system (RSC). We had adopted the alternate way for orbital maneuver and three minor maneuvers in Nov. 2011 were successfully done so that AKATSUKI would meet Venus in 2015. We are considering several scenarios for VOI using only RCS. © 2013 IAA.
  • Tomoo Ushio, Mitsuteru Sato, Takeshi Morimoto, Makoto Suzuki, Atsushi Yamazaki, Yasuhide Hobara, Masayuki Kikuchi, Umran Inan, Ivan Linscott, Hiroshi Kikuchi, Ryohei Ishida, Yukihiro Takahashi, Toru Adachi, Yuji Sakamoto, Zen Ichiro Kawasaki
    International Conference on Atmospheric Electricity, ICAE 2014 2014年 [査読有り][通常論文]
     
    © International Conference on Atmospheric Electricity, ICAE 2014 The Global Lightning and sprIte MeasurementS (GLIMS) on the International Space Station (ISS) is a mission to detect and locate optical transient luminous events (TLEs) and its associated lightning simultaneously from the non-sun synchronous orbit, and was launched successfully in July, 2012 as part of the multi-mission consolidated equipment on Japanese Exposure Module (JEM). Our mission goals are to identify temporal and spatial evolutions of lightning and TLEs and to clarify the occurrence conditions of TLEs and global occurrence locations and rates of TLEs from the nadir observation. To achieve these goals, two CMOS cameras, six Photometers, VLF receiver, and VHF interferometer with two antennas, are installed at the bottom of the module to observe the TLEs as well as causative lighting discharges at nadir direction during day and night time. Though the luminous events so-called sprite, elves and jets have been investigated by numerous researchers all over the world based mainly on the ground observations, some important problems have not been fully understood yet such as generation mechanisms of columniform fine structure and horizontal offset of some sprites from the parent lightning discharges. In the JEM-GLIMS mission, observations from our synchronized sensors are going to shed light on above-mentioned unsolved problems regarding TLEs as well as causative lighting discharges. JEM-GIMS was successfully launched and transported to the ISS by the H-II Transfer Vehicle (HTV) No.3 cargo transporter at the end of July 2012, and started its operation from December 2012. So far, more than one thousand events were recorded. In this paper, we present on the mission overview, examples of the observation results, and several initial analysis for the observed events such as on the identification of the intra-cloud and ground flashes from optical measurements and lightning location from the broad band interferometry at VHF band.
  • Yukihiro Takahashi, Mitsuteru Sato, Kozo Yamashita
    2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) 2014年 [査読有り][通常論文]
  • An ELF Signal Associated with a Positive GC Lightning Event in Winter
    Honma. N, Y. Hongo, D. Tsurushima, F. Tsuchiya, M. Sato, Y. Takahashi
    Proc. 23nd International Lightning Detection Conf. 2014年 [査読無し][通常論文]
  • J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, M. Ambrosio, L. Anchordoqui, A. Anzalone, Y. Arai, C. Aramo, K. Asano, M. Ave, P. Barrillon, T. Batsch, J. Bayer, T. Belenguer, R. Bellotti, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, J. Biccki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J. -N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, O. Catalano, A. Cellino, M. Chikawa, M. J. Christi, V. Connaughton, J. F. Cortes, H. J. Crawford, R. Cremonini, S. Csorna, J. C. D'Olivo, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, L. del Peral, A. Dell'Oro, M. P. De Pascale, M. Di Martino, G. Distratis, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, A. Franceschi, J. Fujimoto, P. Galeotti, G. Garipov, J. Geary, U. G. Giaccari, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, T. Iguchi, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, S. H. Ko, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, E. Kuznetsov, G. La Rosa, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, L. Marcelli, A. Marini, G. Martin-Chassard, O. Martinez, G. Masciantonio, K. Mase, R. Matev, A. Maurissen, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, D. Monnier-Ragaigne, J. A. Morales de los Rios, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, J. W. Nam, S. Nam, K. Nam, T. Napolitano, D. Naumov, A. Neronov, K. Nomoto, T. Ogawa, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, N. Pacheco, M. I. Panasyuk, E. Parizot, I. H. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, T. Peter, P. Picozza, A. Pollini, H. Prieto, P. Reardon, M. Reinabi, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, M. Scuderi, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozigbio, H. H. Silva Lopez, J. Sledd, K. Slomiriska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, T. Tomida, N. Tone, F. Trillaud, R. Tsenov, K. Tsuno, T. Tymieniecka, Y. Uchihori, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, A. Zamora, A. Zuccaro Marchi
    ASTROPARTICLE PHYSICS 44 76 - 90 2013年04月 [査読有り][通常論文]
     
    We evaluate the exposure during nadir observations with JEM-EUSO, the Extreme Universe Space Observatory, on-board the Japanese Experiment Module of the International Space Station. Designed as a mission to explore the extreme energy Universe from space, JEM-EUSO will monitor the Earth's nighttime atmosphere to record the ultraviolet light from tracks generated by extensive air showers initiated by ultra-high energy cosmic rays. In the present work, we discuss the particularities of space-based observation and we compute the annual exposure in nadir observation. The results are based on studies of the expected trigger aperture and observational duty cycle, as well as, on the investigations of the effects of clouds and different types of background light. We show that the annual exposure is about one order of magnitude higher than those of the presently operating ground-based observatories. (C) 2013 Elsevier B.V. All rights reserved.
  • Nadir Observations of Lightning and TLEs by JEM-GLIMS
    M. Sato, T. Ushio, T. Morimoto, M. Suzuki, A. Yamazaki, M. Kikuchi, Y. Takahashi, I. Umran, L. Ivan, Y. Hobara
    EGU General Assembly 2013 --  2013年04月 [査読有り][通常論文]
  • Hiroo Kunimori, Toshihiro Kubooka, Tetsuharu Fuse, Hideki Takenaka, Morio Toyoshima, Toshinori Kuwahara, Kazuya Yoshida, Yoshihiro Tomioka, Kazufumi Fukuda, Junichi Kurihara, Yukihiro Takahashi
    Proceedings of the International Astronautical Congress, IAC 4 3132 - 3136 2013年 
    The laser communication terminal called VSOTA and a 5m GSD multi-spectral high-resolution Cassegrain telescope called HPT will be equipped on a 50kg-class micro satellite RISESAT. VSOTA aims to demonstrate satellite-to-ground laser communication by means of accurate attitude control of the satellite body itself. The HPT is designed to be able to send the coordinate information of the light spot from laser on ground to the attitude control system with a frequency of 10 Hz. RISESAT also carries a single retro-reflector which serves to make sure to keep acquisition and pointing for ground station. Link analysis between HPT and ground station as well as laser ranging laser as a pilot signal in initial acquisition scenario is discussed. ©2013 by the International Astronautical Federation. All rights reserved.
  • Hiroyo Ohya, Fuminori Tsuchiya, Hiroyuki Nakata, Kazuo Shiokawa, Yoshizumi Miyoshi, Kozo Yamashita, Yukihiro Takahashi
    JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS 117 2012年11月 [査読有り][通常論文]
     
    We report multipoint observations of daytime tweek atmospherics during the solar eclipse of 22 July 2009. Sixteen and sixty-three tweek atmospherics were observed at Moshiri and Kagoshima, Japan, where the magnitudes of the solar eclipse were 0.458 and 0.966, respectively. This was the first observation of tweek atmospherics during a low-magnitude eclipse (0.458). The average and standard deviation of the reflection height were 94.9 +/- 13.7 km at Moshiri and 87.2 +/- 12.9 km at Kagoshima. The reflection height at Moshiri was almost the same as that for normal nighttime conditions in July (96.7 +/- 12.6 km) in spite of the low magnitude of the eclipse. The reflection height at Kagoshima seems be divided into two parts: propagation across the total solar eclipse path and propagation in the partial solar eclipse path. During the eclipse, we also observed the phase variation in the LF transmitter signals. The average change in the phase delay of the LF signals was 109 degrees for the paths that crossed the eclipse path and 27 degrees for the paths that did not cross the eclipse path. Assuming a normal daytime height for LF waves of 65 km, a ray tracing analysis indicates that the variations in phase correspond to a height increase of 5-6 km for the paths across the eclipse and 1-2 km for partial eclipse paths. The wide range of estimated tweek reflection heights at Kagoshima also suggests a difference in electron density in the lower ionosphere between total and partial solar eclipses.
  • FUKUDA Kazufumi, SUGIMURA Nobuo, SAKAMOTO Yuji, KUWAHARA Toshinori, YOSHIDA Kazuya, TAKAHASHI Yukihiro
    TRANSACTIONS OF THE JAPAN SOCIETY FOR AERONAUTICAL AND SPACE SCIENCES, AEROSPACE TECHNOLOGY JAPAN 10 28 Td_11 - Td_16 THE JAPAN SOCIETY FOR AERONAUTICAL AND SPACE SCIENCES 2012年 
    The 50-kg class micro satellite RISING-2 is now under development by Tohoku University and Hokkaido University. The development is at Flight Model phase and some components are tested to evaluate its specifications. In this paper, the endurance tests using vacuum chamber and thermal test chamber in Tohoku University are described. There was no problem in those tests. In addition, the attitude control accuracy of the RISING-2 was analyzed in the simulation. This simulation based on component specifications and also included noise data. The results show the pointing error angle was less than required error angle.
  • Masato Nakamura, Yasuhiro Kawakatsu, Chikako Hirose, Takeshi Imamura, Nobuaki Ishii, Takumi Abe, Atsushi Yamazaki, Manabu Yamada, Kazunori Ogohara, Kazunori Uemizu, Tetsuya Fukuhara, Shoko Ohtsuki, Takehiko Satoh, Makoto Suzuki, Munetaka Ueno, Naomoto Iwagami, Makoto Taguchi, Shigeto Watanabe, Yukihiro Takahashi, George L. Hashimoto, Hiroki Yamamoto
    Proceedings of the International Astronautical Congress, IAC 3 1727 - 1732 2012年 
    Japanese Venus Climate Orbiter/AKATSUKI was proposed in 2001 with strong support by international Venus science community and approved as an ISAS (Institute of Space and Astronautical Science) mission soon after the proposal. The mission life we expected was more than two Earth years in Venus orbit. AKATSUKI was successfully launched at 06:58:22JST on May 21, 2010, by H-IIA F17. After the separation from H-IIA, the telemetry from AKATSUKI was normally detected by DSN Goldstone station (10:00JST) and the solar cell paddles' expansion was confirmed. The malfunction happened on the propulsion system during the Venus orbit insertion (VOI) on Dec 7, 2010. We failed to make the spacecraft become a Venus orbiter, and the spacecraft entered an orbit around the Sun with a period of 203 days. Most of the fuel still had remained, but the orbital maneuvering engine was found to be broken. We decided to use only the reaction control system (RCS) for orbital maneuver and three minor maneuvers in Nov 2011 were successfully done so that AKATSUKI will meet Venus in 2015. We are considering several scenarios for VOI using only RCS. Copyright © (2012) by the International Astronautical Federation.
  • Makoto Watanabe, Yukihiro Takahashi, Mitsuteru Sato, Shigeto Watanabe, Tetsuya Fukuhara, Ko Hamamoto, Akihito Ozaki
    GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY IV 8446 84462O  2012年 [査読無し][通常論文]
     
    We have built a visible multi-spectral imager (MSI) for the 1.6-m Pirka telescope of the Hokkaido University in Hokkaido, Japan. The instrument is equipped with two liquid crystal tunable filters and a 512 x 512 pixel EMCCD camera. One of the major purposes of this instrument is to obtain multi-spectral images (series of narrow-band images at many different wavelengths) of the solar planets rapidly. These tunable filters are a Lyot filter with liquid crystal variable retarders and thus can tune the transmitting wavelength rapidly without moving parts. Their spectral ranges are 400-720 nm and 650-1100 nm and the bandwidth is typically 10 nm on both filters. The EMCCD camera can obtain images at a frame rate of about 32 Hz, which also enables us to improve the spatial resolution with the shift-and-add or the Lucky imaging techniques. The field of view is 3.3 x 3.3 arcmin with a pixel scale of 0.39 arcsec pixel(-1). The instrument also has UBV RI-band broad-band filters and several narrow-band filters. MSI is mounted at the f/12 Cassegrain focus of the telescope. It had the first light on February 2011, and then have been used for several astronomical and planetary science programs as a major facility instrument at this telescope. We describe the design, construction, integration, and performance of this multi-spectral imager.
  • Nakano Toshihiko, Shoji Yasuhiro, Yamamoto Mutsumi, Hamamoto Ko, Nakamoto Jumpei, Imai Masataka, Sakamoto Yuji, Kuwahara Toshinori, Watanabe Makoto, Takahashi Yukihiro, Yoshida Kazuya, Taguchi Makoto, IEEE
    2012 Ieee/sice International Symposium on System Integration (Sii) 313 - 318 2012年 [査読有り][通常論文]
  • Ushio, T, M. Sato, T. Morimoto, M. Suzuki, H. Kikuchi, A. Yamazaki, Y. Takahashi, Y. Hobara, U. Inan, I. Linscott, Y. Sakamoto, R. Ishida, M. Kikuchi, K. Yoshida, Z. Kawasaki
    IEEJ Transactions on Fundamentals and Materials 131 12 971 - 976 The Institute of Electrical Engineers of Japan 2011年12月 [査読有り][通常論文]
     
    Global Lightning and sprIte MeasurementS (GLIMS) is a mission on the International Space Station (ISS) to detect and locate optical transient luminous events (TLEs) and associated lightning simultaneously from the non-sun-synchronous orbit. It is scheduled to be launched from Japan in January, 2012 as part of the multi-mission consolidated equipment on the Japanese Exposure Module (JEM). Our mission's goals are (1) to detect and locate lightning and sprites within storm scale resolution over a large region of the Earth's surface along the orbital track of the ISS without any bias, (2) to clarify the mechanism by which sprites are generated, and (3) to identify the conditions under which TLEs occur. To achieve these goals, two CMOS cameras, six Photometers, a VLF receiver and VHF interferometer with two antennas are installed at the bottom of the module to observe the TLEs, as well as causative lightning discharges at nadir direction during day and night time. Though the luminous events' so-called sprites, elves and jets have been investigated by numerous researchers all over the world based mainly on ground observations, some important problems have not been fully understood yet. These include the generation mechanisms of columniform fine structures and horizontal offset of some sprites from the parent lightning discharges. In the JEM-GLIMS mission, observations from our synchronized sensors will shed light on the unsolved problems mentioned above regarding TLEs and causative lightning discharges. In this presentation scientific background, instrumentation, and project summaries are given.
  • Development Status and Operation Plan of 50-kg Microsatellite RISING-2 for Earth Observations by Multi-Spectrum Instruments
    Yuji Sakamoto, Toshinori Kuwahara, Yoshihiro Tomioka, Kazufumi Fukuda, Steve Battazzo, Kazuya Yoshida, Tetsuya Fukuhara, Junichi Kurihara, Yukihiro Takahashi
    The 28th International Symposium on Space Technology and Science (ISTS), Naha, Japan, June 2011, No.2011-f-25. 2011年06月 [査読無し][通常論文]
  • Y. T. Tanaka, M. Hayakawa, Y. Hobara, A. P. Nickolaenko, K. Yamashita, M. Sato, Y. Takahashi, T. Terasawa, T. Takahashi
    GEOPHYSICAL RESEARCH LETTERS 38 L08805  2011年04月 [査読有り][通常論文]
     
    We report on the first clear detection of transient Extremely-Low-Frequency (ELF) signal caused by an extremely intense cosmic gamma-ray flare. On 2004 December 27, the brightest gamma-ray flare ever recorded was observed by numerous satellites. A transient ELF emission observed at Moshiri and Onagawa in Japan exactly coincided with the peak time of the flare, and its wide pulse width of similar to 40 ms disfavors the possibility of lightning origin. Furthermore, the two horizontal components of ELF magnetic field data recorded at Esrange in Sweden showed clear transient Schumann resonance waveforms. The source direction determined by the Lissajous method roughly corresponds to the subflare point. The chance probability that a sprite occurs within 30 ms of the peak flare time is similar to 0.025%, which again clearly excludes the sprite origin. Thus, a bright cosmic gamma-ray flare is a new source of transient ELF radio signals observed on the Earth, although the emission mechanism needs to be clarified in future. Citation: Tanaka, Y. T., M. Hayakawa, Y. Hobara, A. P. Nickolaenko, K. Yamashita, M. Sato, Y. Takahashi, T. Terasawa, and T. Takahashi (2011), Detection of transient ELF emission caused by the extremely intense cosmic gamma-ray flare of 27 December 2004, Geophys. Res. Lett., 38, L08805, doi: 10.1029/2011GL047008.
  • Hong Peng K, Miyahara Hiroko, Yokoyama Yusuke, Takahashi Yukihiro, Sato Mitsuteru
    JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS 73 5月6日 587 - 591 2011年04月 [査読有り][通常論文]
  • Kozo Yamashita, Yukihiro Takahashi, Mitsuteru Sato, Hiromi Kase
    JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS 116 2011年02月 [査読有り][通常論文]
     
    The global observation of cloud-to-ground (CG) discharges based on ELF measurements provides essential information, including vertical charge moment (Qdl) for investigations of global-scale thunderstorm activity. However, the geolocating method by direction finding of sferics in the frequency range of 1-100 Hz has a rather large error, on the order of 1000 km, even for the CGs with relatively large Qdl (>1000 C-km). Here we improve the methods for geolocation and estimation of Qdl, which are applicable to smaller CGs with Qdl down to 470 C-km, making use of the time-of-arrival method and the high correlation between Qdl and the peak amplitude of ELF sferics. The evaluated average error in geolocation, comparing with World Wide Lightning Location Network data, is 680 km. By this improved method, CGs with Qdl of <470 C-km can be detected at any location in the world. In the preliminary analysis for the year of 2004, the number of CGs whose location and Qdl are determined is about a million events per month, roughly 10-30 times compared to previous studies by ELF measurement, enabling an investigation of the day-to-day variations of the global CG distribution with transferred charge amount. The combination of accurate geolocation and the uniformity of detection show active regions in the three main areas: Africa, South America, and the Maritime Continent. In addition, minor thunderstorm areas in Japan, the Mediterranean Sea, and the Pacific Ocean can be monitored.
  • Toshinori Kuwahara, Kazuya Yoshida, Yuji Sakamoto, Yukihiro Takahashi, Junichi Kurihara, Hiroshi Yamakawa, Atsushi Takada
    62nd International Astronautical Congress 2011, IAC 2011 5 3699 - 3706 2011年 
    Professor Shinichi Nakasuka of University of Tokyo is now leading a small satellite development activity within the scope of a Japanese FIRST (Funding Program for World-Leading Innovative R&D on Science and Technology) program. In this program several 50-kg class micro-satellites are going to be developed and launched by the end of Japanese fiscal year of 2013, including one scientific micro-satellite under international cooperation. This program as whole shall contribute to enhance the activities of world's small satellite research societies and industries, and to build the basis of new paradigm for the future, where cost-effective and reliable small satellites are widely utilized for both research and business purposes. Tohoku University has been assigned as the project leader of the above mentioned international scientific micro-satellite, named as RISESAT (Rapid International Scientific Experiment Satellite), and is developing the bus system as well as organizing scientific payload instruments from all over the world together with Hokkaido University and Kyoto University. This satellite shall demonstrate the performance of its bus system which is supposed to be offered as a common bus system for international scientific missions in the future. The selection of scientific instruments is almost finished. The orbit of me RISESAT is planned to be a sun-synchronous orbit with an altitude of between 500km and 800km. In order to accommodate as many payload instruments as possible, the satellite is equipped with two deployable side solar panels enabling a maximum power consumption of up to about 100 W. Many of the attitude determination and control components are going to be developed by the Space Robotics Laboratory of the Tohoku University achieving an attitude control accuracy of better than 0.1 deg. It is also equipped with an X-band transmitter for mission data downlink. The electrical interface between the payload instruments and the bus system is based on a space plug and play avionics standard. The development of engineering model of the RISESAT will be completed by March 2012. This paper summarizes the system design of the satellite and progress report of the development activities, as well as the brief description of selected scientific instruments. Copyright ©2011 by the International Astronautical Federation. All rights reserved.
  • Kozo Yamashita, Yukihiro Takahashi, Mitsuteru Sato, Hiromi Kase
    Journal of Geophysical Research: Space Physics 116 2 2011年 [査読有り][通常論文]
     
    The global observation of cloud-to-ground (CG) discharges based on ELF measurements provides essential information, including vertical charge moment (Qdl) for investigations of global-scale thunderstorm activity. However, the geolocating method by direction finding of sferics in the frequency range of 1-100 Hz has a rather large error, on the order of 1000 km, even for the CGs with relatively large Qdl (> 1000 C-km). Here we improve the methods for geolocation and estimation of Qdl, which are applicable to smaller CGs with Qdl down to 470 C-km, making use of the time-of-arrival method and the high correlation between Qdl and the peak amplitude of ELF sferics. The evaluated average error in geolocation, comparing with World Wide Lightning Location Network data, is 680 km. By this improved method, CGs with Qdl of < 470 C-km can be detected at any location in the world. In the preliminary analysis for the year of 2004, the number of CGs whose location and Qdl are determined is about a million events per month, roughly 10-30 times compared to previous studies by ELF measurement, enabling an investigation of the day-to-day variations of the global CG distribution with transferred charge amount. The combination of accurate geolocation and the uniformity of detection show active regions in the three main areas: Africa, South America, and the Maritime Continent. In addition, minor thunderstorm areas in Japan, the Mediterranean Sea, and the Pacific Ocean can be monitored. Copyright 2011 by the American Geophysical Union.
  • 「月惑星探査の来たる10年」検討・第一段階報告
    大谷栄治, 倉本圭, 今村剛, 寺田直樹, 渡部重十, 荒川政彦, 伊藤孝士, 圦本尚義, 渡部潤一, 木村淳, 高橋幸弘, 中島健介, 中本泰史, 三好由純, 小林憲正, 山岸明彦, 並木則行, 小林直樹, 出村裕英, 大槻圭史
    日本惑星科学会誌 20 350 - 366 2011年 [査読有り][通常論文]
  • Y. Takahashi, A. Yoshida, M. Sato, T. Adachi, S. Kondo, R. -R. Hsu, H. -T. Su, A. B. Chen, S. B. Mende, H. U. Frey, L. -C. Lee
    JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS 115 2010年09月 [査読有り][通常論文]
     
    Although the Quasi-electrostatic (QE) model has been considered a basic mechanism for describing sprite generation, the relationship between sprite luminosity and the charge moment change (CMC) value, caused by the sprites' parent lightning has not been examined quantitatively. CMC value represents the energy of cloud-to-ground discharge (CG) and the electric field intensity above the thunderstorm. We focused on the data obtained in 2004, in which both ISUAL on board the FORMOSAT-2 satellite and the Tohoku ELF network were operated throughout one year. We could estimate the absolute luminous intensity of sprites free from atmospheric influence with the ISUAL/Array Photometer (AP) and investigated its relationship to the charge moment of parent lightning. Absolute optical energies emitted from sprites were estimated for 14 streamer-type sprites for the first time. The averages of the time-integrated optical energies are 176 kJ and 119 kJ for the N2 1PG and N2 2PG bands, respectively. Furthermore, the optical energies and the charge moments of their parent lightning estimated with ELF data show a high correlation (correlation coefficient = 0.93), that is consistent, qualitatively, with the QE model. This relationship predicts that the 50% occurrence probability is located at similar to 600 C km, which coincides with previous statistical studies.
  • S. C. Chang, C. L. Kuo, L. J. Lee, A. B. Chen, H. T. Su, R. R. Hsu, H. U. Frey, S. B. Mende, Y. Takahashi, L. C. Lee
    JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS 115 2010年07月 [査読有り][通常論文]
     
    The Imager of Sprites and Upper Atmospheric Lightnings (ISUAL) often recorded events that have significant far-ultraviolet (FUV) emissions in the spectrophotometer but have no discernible transient luminous events (TLEs) in the imager. These FUV events likely are dim TLEs. To confirm the conjecture, lightning emissions were simulated and proved to be completely absorbed by the atmosphere. The FUV emission of the FUV events follows the lightning OI emission within 1 ms, similar to the characteristics of elves. After analyzing the imager-N(2)1P brightness of the elves and their FUV intensity, a linear correlation was found, which is consistent with the work of Kuo et al. (2007). The intensity of the FUV events ranks among the dimmest elves and is less than 1 x 10(4) photons/cm(2). Combining all the information, the FUV events are identified as dim elves that eluded the detection of the ISUAL imager. Also from the detection limits of the ISUAL spectrophotometer (SP) and the imager, for the before-the-limb elves the detection number of SP is found to be nearly 16 times higher than that of the imager. This result is consistent with a related factor of similar to 13 that was inferred from the U. S. National Lightning Detection Network (NLDN) peak current distribution for the negative cloud-to-ground lightning. Hence the ISUAL spectrophotometer can be used to perform elve survey, to infer the peak current of the elve-producing lightning, and possibly to be used to deduce other lightning parameters. Evidence is also found for the existence of multielves, which are FUV events from the M-components or the multiple strokes in lightning flashes.
  • Yukihiro Takahashi, Kazuya Yoshida, Yuji Sakamoto, Takeshi Sakamoi
    SMALL SATELLITE MISSIONS FOR EARTH OBSERVATION 197 - + 2010年 [査読有り][通常論文]
     
    SPRITE-SAT is a micro satellite in the size of 50 cm cube and weighing 45-kg, designed and developed by Tohoku University. Its mission objective is to conduct scientific observation of atmospheric luminous emissions called "sprites" and terrestrial Gamma-ray flushes. Both are recently discovered phenomena and their mechanisms are still under the veil. SPRITE-SAT was developed to achieve significant observations to determine clear models of these mysterious phenomena. On January 23rd, 2009, SPRITE-SAT was successfully launched by JAXA's H-IIA rocket as a piggyback payload of Greenhouse Gas Observation Satellite (GOSAT). The spacecraft is now in a sun-synchronous polar orbit with 670 km altitude form the Earth's surface.
  • Yuji Sakamoto, Yukihiro Takahashi, Kazuya Yoshida, Kazufumi Fukuda, Toshihiko Nakano, Steve Battazzo, Tetsuya Fukuhara, Junichi Kurihara
    61st International Astronautical Congress 2010, IAC 2010 1 469 - 473 2010年 
    Tohoku University and Hokkaido University started the development of a new 41-kg microsatellite RISING-2 at July 2009. This satellite inherits the development technique of RISING (SPRITE-SAT) launched on January 2009. The progress of RISING-2 project is shown in this paper. Using a Cassegrain telescope with 10-cm diameter and 1-m focal length, earth surface is observed with 5-m resolution from 700-km-alt sun synchronous orbit. By 3-axis attitude stabilization using reaction wheels and star sensors, the designated area on earth surface can be observed. In addition to color images, multi-spectrum images of cumulonimbus are observed by using a liquid crystal tunable filter. As a secondary mission, transient luminous events such as sprite are observed, which is same mission as SPRITE-SAT. Copyright ©2010 by the International Astronautical Federation. All rights reserved.
  • 坂本 祐二, 吉田 和哉, 高橋 幸弘
    年次大会講演論文集 2010 371 - 372 一般社団法人日本機械学会 2010年 
    Tohoku University and Hokkaido University started the development of a new 50-kg microsatellite RISING-2 at July 2009. This satellite inherits the development technique of RISING (SPRITE-SAT) launched on January 2009. The progress is shown in this paper. Using a Cassegrain telescope with 10-cm diameter and 1-m focal length, earth surface is observed with 5-m resolution from 700-km-alt sun synchronous orbit. By 3-axis attitude stabilization using reaction wheels and star sensors, the designated area on earth surface can be observed. In addition to color images, multi-spectrum images of cumulonimbus are observed by using a liquid crystal tunable filter. As a secondary mission, transient luminous events such as sprite are observed, which is same mission as SPRITE-SAT.
  • SHOJI Yasuhiro, ONISHI Tomoya, BATTAZZO Steve, TERAGUCHI Tomoko, YOSHIMURA Atsushi, SAKAMOTO Yuji, TAKAHASHI Yukihiro, YOSHIDA Kazuya, TAGUCHI Makoto
    TRANSACTIONS OF THE JAPAN SOCIETY FOR AERONAUTICAL AND SPACE SCIENCES, AEROSPACE TECHNOLOGY JAPAN 8 27 Pm_15 - Pm_20 THE JAPAN SOCIETY FOR AERONAUTICAL AND SPACE SCIENCES 2010年 
    A balloon borne telescope is one of the space observation methods by carrying a telescope to the stratosphere with a huge balloon in order to be free from the atmospheric influences on observations. The authors have been developing a balloon borne telescope system for optical observations of other planets in the solar system. The observation aimed to achieve finer images of the planets than those taken by ground telescopes, which required the balloon borne telescope to hold the target star with subarcsec precision during the exposure of the camera. To meet the requirement, the system is equipped three stage pointing system. This article introduces the overview of the flight campaign and the flight system, and reports the pointing performance verified in ground experiments.
  • SAKAMOTO Yuji, NAKAZATO Yasuhiro, SAWAKAMI Tomoki, YOSHIDA Kazuya, TAKAHASHI Yukihiro
    TRANSACTIONS OF THE JAPAN SOCIETY FOR AERONAUTICAL AND SPACE SCIENCES, AEROSPACE TECHNOLOGY JAPAN 8 27 Tf_1 - Tf_6 THE JAPAN SOCIETY FOR AERONAUTICAL AND SPACE SCIENCES 2010年 
    The microsatellite SPRITE-SAT developed by Tohoku University was launched in January 2009. Regarding the thermal system of SPRITE-SAT, the mathematical model, the parameter determination for the heat transfer coefficients, and the comparison between the estimate and real temperature in flight mode are shown in this paper. The precision of thermal analysis using the simple 7-node model was solved. The estimate error of temperature in orbit is less than 5 degrees Celsius in panels with most of instruments.
  • Y. Takahashi, Y. Okazaki, M. Sato, H. Miyahara, K. Sakanoi, P. K. Hong, N. Hoshino
    ATMOSPHERIC CHEMISTRY AND PHYSICS 10 4 1577 - 1584 2010年 [査読有り][通常論文]
     
    Although linkages between solar activity and the earth's climate have been suggested and the 11-year cycle in solar activity evident in sunspot numbers is the most examined example of periodicity in previous studies, no quantitative evidence indicating a relationship for tropospheric phenomena has been found for a short period. Based on FFT analysis for OLR (Outgoing Longwave Radiation) compared with the F10.7 index, we clearly demonstrate a 27-day variation in the cloud amount in the region of the Western Pacific warm pool, which is only seen in the maximum years of 11-year solar activity. The average spectrum in such years also shows an enhancement in the range of the MJO (Madden-Julian Oscillation) period. Although there exist some explanations for possible mechanisms, the exact cause is unknown. Therefore, the proposed connection between 27-day cloud variation and solar cycle in the WPWP region is still a hypothesis and various kinds of varification based on other meteorological and solar parameters are strongly required.
  • Williams, E, W.A. Lyons, Y. Hobara, V. Mushtak, N. Asencio, R. Boldi, J. Bo r, S. Cummer, E. Greenberg, M. Hayakawa, R. Holzworth, V. Kotroni, J. Li, C. Morales, T. Nelson, C. Price, B. Russell, M. Sato, G. Satori, K. Shirahata, Y. Takahashi, K. Yamashita
    Q. J. R. Meteorol. Soc. 136 257 - 271 2009年12月 [査読有り][通常論文]
  • 高橋 幸弘
    電気学会論文誌. A, 基礎・材料・共通部門誌 = The transactions of the Institute of Electrical Engineers of Japan. A, A publication of Fundamentals and Materials Society 129 4 163 - 167 The Institute of Electrical Engineers of Japan 2009年04月01日 
    Lightning is discharge phenomenon between thunderclouds and the ground, or inside/between thunderclouds. However, a new type of atmospheric discharge was found in 1989 by chance: a discharge between thundercloud and ionosphere, named "sprites". After this discovery, similar types of transient luminous events in the middle and upper atmosphere, called TLEs, have been reported. On the other hand, gamma-ray flash radiated from the thundercloud, called TGF, was found in 1994 by satellite observation. Detail characteristics, mechanisms and effects on the atmosphere are not well understood both for TLE and TGF, although the extensive investigations have been carried out experimentally and theoretically for more than a decade. Here we review these phenomena and introduce the latest projects to solve the fundamental scientific problems.
  • SHOJI Yasuhiro, YOSHIKAWA Takashi, SAKAMOTO Yuji, TAKAHASHI Yukihiro, YOSHIDA Kazuya
    TRANSACTIONS OF THE JAPAN SOCIETY FOR AERONAUTICAL AND SPACE SCIENCES, SPACE TECHNOLOGY JAPAN 7 26 Tn_7 - Tn_12 THE JAPAN SOCIETY FOR AERONAUTICAL AND SPACE SCIENCES 2009年 
    An S-520 sounding rocket was launched in the summer of 2007 in order to observe magneto electric phenomena in high sky and to verify a new spectroscopic observation method. A Multi-Spectrum Imager (MSI) was developed for the latter aim. The observation device is equipped a spectroscopic camera with a liquid crystal tunable filter and a pointing system to control the pointing direction to take spectroscopic images of a target against the spin of the rocket body. With the successful flight of the sounding rocket, the MSI succeeded in taking and sending approximately 30 pictures and the house keeping data.
  • SAKAMOTO Yuji, KANAZAWA Tomoaki, SHOUJI Yasuhiro, TAKAHASHI Yukihiro, YOSHIDA Kazuya, TAGUCHI Makoto
    TRANSACTIONS OF THE JAPAN SOCIETY FOR AERONAUTICAL AND SPACE SCIENCES, SPACE TECHNOLOGY JAPAN 7 26 Pd_23 - Pd_28 THE JAPAN SOCIETY FOR AERONAUTICAL AND SPACE SCIENCES 2009年 
    Tohoku University and Rikkyo University are carrying out the project of Venus observation with high precision using a balloon-borne telescope. In this paper, the outline of Balloon-Borne Telescope for the optical remote sensing of Venus is introduced, and the simulation model of three-stage control method is constructed. For this observation, the pointing technology with high precision to restrain the slight moving of image is necessary. The target precision is only 0.1 arc seconds. The dynamics and control model is defined firstly, and the model parameters are determined by the experimental verification. By developing the numerical simulation tool, the motion can be estimated in the simulator, and the control strategy can be more easily optimized compared to the gain adjustment only based on experiments.
  • 坂本 祐二, 吉田 和哉, 澤上 友貴, 坂野井 健, 高橋 幸弘
    年次大会講演論文集 2009 245 - 246 一般社団法人日本機械学会 2009年 
    The microsatellite SPRITE-SAT developed by Tohoku University was launched in January 2009. The mission is the observation of Sprite phenomena and Terrestrial Gamma-ray Flashes incidental on lightning discharges. In the 12 days after launch, the satellite is normally operated. But because it is damaged by a serious trouble at February 4, 2009, the data communication including uplink and downlink is not successful now. This paper shows the outlines of satellite system, flight operation results, and the reason of trouble.
  • Y. Takahashi, J. Yoshida, Y. Yair, T. Imamura, M. Nakamura
    SPACE SCIENCE REVIEWS 137 1-4 317 - 334 2008年06月 [査読有り][通常論文]
     
    Lightning activity in Venus has been a mystery for a long period, although many studies based on observations both by spacecraft and by ground-based telescope have been carried out. This situation may be attributed to the ambiguity of these evidential measurements. In order to conclude this controversial subject, we are developing a new type of lightning detector, LAC (Lightning and Airglow Camera), which will be onboard Planet-C (Venus Climate Orbiter: VCO). Planet-C will be launched in 2010 by JAXA. To distinguish an optical lightning flash from other pulsing noises, high-speed sampling at 50 kHz for each pixel, that enables us to investigate the time variation of each lightning flash phenomenon, is adopted. On the other hand, spatial resolution is not the first priority. For this purpose we developed a new type of APD (avalanche photo diode) array with a format of 8x8. A narrow band interference filter at wavelength of 777.4 nm (OI), which is the expected lightning color based on laboratory discharge experiment, is chosen for lightning measurement. LAC detects lightning flash with an optical intensity of average of Earth's lightning or less at a distance of 3 Rv. In this paper, firstly we describe the background of the Venus lightning study to locate our spacecraft project, and then introduce the mission details.
  • 気球搭載望遠鏡による金星観測
    田口 真, 吉田 和哉, 坂本 祐二, 荘司 泰弘, 高橋 幸弘, 坂野井 健
    平成20年度大気球シンポジウム集録 2008年 [査読無し][通常論文]
  • Development of the sprite and lightning imaging system onboard the SPRITE-SAT
    Sato, M, Y. Takahashi, T. Sakanoi, S. Ueda, S. Kondo, K. Yoshida, Y. Sakamoto, T. Takashima
    EOS Trans, AGU 88 52 2008年 [査読無し][通常論文]
  • N. Sakaki, Y. Takizawa, Y. Kawasaki, M. Sato, T. Sawabe, M. Nagano, T. Tsunoda, T. Kamioka, K. Hayasaka, M. Kamimura, A. K. Yoshida, T. Shibata, T. Ebisuzaki, K. Inoue, F. Kajino, Y. Takahashi, Y. Saito, K. Yamada, T. Kawasaki
    Proceedings of the 30th International Cosmic Ray Conference, ICRC 2007 5 HE PART 2 965 - 968 2007年 [査読有り][通常論文]
     
    Ultra-high energy cosmic rays (UHECRs) above 100 EeV have been observed with several experiments. Their origin and propagation mechanism are still in mystery mainly due to the low statistics. In order to observe UHECRs with sufficient statistics, the JEM-EUSO mission is going on. In the JEMEUSO mission, fluorescence and ̌Cerenkov light from the extensive air showers induced by UHECRs are observed with a telescope attached to the International Space Station. It is important to study the background (BG) intensity in near UV region (300-400nm) seen from the JEM-EUSO telescope. We launched a balloon at Sanriku Balloon Center of JAXA to investigate the nightglow and the clouds on August 29, 2005. The upward and downward nightglow were measured in the eight near UV bands and the cloud images were recorded with an infrared thermography. In this paper, the detail of the experiment and the results will be reported.
  • Nakamura, M, Imamura, T, Ueno, M, Iwagami, N, Satoh, T, Watanabe, S, Taguchi, M, Takahashi, Y, Suzuki, M, Abe, T, Hashimoto, G. L, Sakanoi, T, Okano, S, Kasaba, Y, Yoshida, J, Yamada, M, Ishii, N, Yamada, T, Uemizu, K, Fukuhara, T, Oyama, K
    Planet. Space Sci. 55 12 1831 - 1842 2007年01月01日 [査読有り][通常論文]
     
    The Venus Climate Orbiter mission (PLANET-C), one of the future planetary missions of Japan, aims at understanding the atmospheric circulation of Venus. Meteorological information will be obtained by globally mapping clouds and minor constituents successively with four cameras at ultraviolet and infrared wavelengths, detecting lightning with a high-speed imager, and observing the vertical structure of the atmosphere with radio science technique. The equatorial elongated orbit with westward revolution fits the observation of the movement and temporal variation of the atmosphere which as a whole rotates westward. The systematic, continuous imaging observations will provide us with an unprecedented large data set of the Venusian atmospheric dynamics. Additional targets of the mission are the exploration of the ground surface and the observation of zodiacal light. The mission will complement the ESA's Venus Express, which also explores the Venusian environment with different approaches. (C) 2007 Elsevier Ltd. All rights reserved.
  • Y Kawasaki, M Bertaina, T Ebisuzaki, F Kajino, Y Miyazaki, M Nagano, N Sakaki, M Sato, HM Shimizu, Y Takizawa, M Ameri, O Catalano, S Cuneo, F Fontanelli, Gracco, V, P Musico, M Pallavicini, A Petrolini, R Pratolongo, M Sannino, N Bleurvacq, F Cadoux, C Chapron, P Gorodetzky, P Nedelec, T Patzak, E Plagnol, Y Takahashi
    INTERNATIONAL JOURNAL OF MODERN PHYSICS A 20 29 6890 - 6893 2005年11月 [査読有り][通常論文]
     
    The Extreme Universe Space Observatory (EUSO) is a space mission to study extremely high-energy cosmic rays. The EUSO instrument is a wide-angle refractive telescope in near-ultraviolet wavelength region to observe time-resolved atmospheric fluorescence images of the extensive air showers from the International Space Station. The Focal surface is an aspherical curved surface, and its area amounts to about 4.5 m(2). The focal surface detector is designed as a mosaic of multianode photomultipliers (MAPMT) for the single photoelectron counting capability. The strongest requirement for the focal surface detector is the maximization of the photon detection efficiency together with the uniformity over the focal surface. We have developed a new type of MAPMT. It is modified from the ordinary one and has a grid between the photocathode and the first dynode to electrostatically demagnify the photoelectron image on the dynode. We are also developing the HV supply system for a great number of MAPMTs. EUSO experiments the day-time and night-time every 90 minutes. The heat flow must be considered to stabilize the PMT characteristics, in parallel with the heat dissipation of the electronics attached on the focal surface supporting structure.
  • Cheng-Ling Kuo, R. R. Hsu, A. B. Chen, H. T. Su, L. C. Lee, S. B. Mende, H. U. Frey, H. Fukunishi, Y. Takahashi
    Geophysical Research Letters 32 19 1 - 4 2005年10月16日 [査読有り][通常論文]
     
    Electron energies and the strenght of electric fields in sprites are deduced for five selected events, which were recorded by the space-borne instrument called ISUAL (Imager of Sprites and Upper Atmospheric Lightning a payload on the FORMOSAT-2 satellite). From the derived peak intensity ratios of spectrophotometer channel 2 (centered at 337 nm) and channel 3 (centered at 391.4 nm) of these sprites, the average and characteristic electron energies were found to be in the range of 6.2-9.2 eV and 4.5-6.5 eV, respectively. The estimated E/N at 40-60 km is 243-443 Td and the strength of the electric field is 2.1 - 3.7 times that of the atmosphere breakdown E-field at these altitudes. The inferred electron energies and the strength of electric fields are about two times higher than those inferred from ground campaigns. However, they are consistent with the prediction of the sprite streamer model. Copyright 2005 by the American Geophysical Union.
  • Y Okazaki, H Fukunishi, Y Takahashi, M Taguchi, S Watanabe
    JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS 110 A3 2005年03月 [査読有り][通常論文]
     
    [1] Interplanetary hydrogen atoms that penetrate into the heliosphere are illuminated by enhanced hydrogen Lyman alpha emission from solar active regions. Using the data obtained by the Solar Wind Anisotropies ( SWAN) instrument on board the Solar and Heliospheric Observatory (SOHO), Bertaux et al. ( 2000) proposed a new method for earlier detection and monitoring of solar active regions on the far-side hemisphere. However, a quantitative relationship between the sky map of interplanetary Lyman alpha intensity and the enhanced emission from a solar active region was not discussed. Here, we analyze the interplanetary Lyman alpha intensity data obtained by the Ultraviolet Imaging Spectrometer (UVS) on board the Nozomi spacecraft. We develop a method to map the distribution of interplanetary Lyman alpha intensity into the Carrington coordinate system by assuming an interplanetary hydrogen screen at the location of maximum volume emission rate. Analysis period is from January 2000 to March 2000 near solar maximum. The solar activity during this analysis period is much higher as compared with the case study by Bertaux et al. ( 2000). The sky map of the Lyman alpha emission obtained by the UVS is shown to exhibit a high correlation with the solar extreme ultraviolet (EUV) intensity map obtained by the EUV Imaging Telescope (EIT) on board the SOHO satellite. The highest value of two-dimensional correlation coefficient is 0.80. An observed change in the periodicity of interplanetary Lyman alpha intensity is in good agreement with the growth of an active region on the Sun. It has been also confirmed that the far-side observations of UVS detected the growth of an active region in advance. This case study demonstrates that the location and intensity variation of activity on the far side of the Sun can be detected by far-side measurements of interplanetary Lyman alpha emission intensity. It is thus concluded that the developed method contributes to space weather forecasting on a scale of 2 weeks.
  • A Ohkubo, H Fukunishi, Y Takahashi, T Adachi
    GEOPHYSICAL RESEARCH LETTERS 32 4 2005年02月 [査読有り][通常論文]
     
    Sprite luminosities produced by winter lightning in Japan were found to be associated with simultaneous occurrences of clusters of radio atmospherics as observed in the VLF range, suggesting an in- cloud discharge activity. Concurrent ELF data show transient perturbations, indicating continuous charge transfer in causative lightning. These data provide the first evidence that an incloud discharge activity plays an important role in the generation mechanism of sprites. Citation: Ohkubo, A., H. Fukunishi, Y. Takahashi, and T. Adachi ( 2005), VLF/ ELF sferic evidence for in- cloud discharge activity producing sprites.
  • Sato, M, T. Ebisuzaki, Y. Takizawa, Y. Kawasaki, N. Sakaki, M. Bertaina, H.M. Shimizu, Y. Takahashi, T. Adachi
    International Journal of Modern Physics A 20 29 6903 - 6905 2005年 [査読有り][通常論文]
  • Adachi, T, H. Fukunishi, Y. Takahashi, M. Sato
    Geophys. Res. Lett. 31 4 L04107  2004年02月 [査読有り][通常論文]
  • R Miyasato, H Fukunishi, Y Takahashi, MJ Taylor
    JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS 65 5 573 - 581 2003年03月 [査読有り][通常論文]
     
    Sprite halos are brief diffuse glows with an average duration of similar to1 ms occurring at altitudes from 70 to 85 km preceding the development of sprite streamers. Their horizontal scale is similar to50-100 km and they move downward as if focusing into the center. To investigate the energies of electrons producing sprite halos and their spatial and temporal variations, we analyzed photometric and CCD imaging data recorded at Yucca Ridge Field Station, Colorado, USA, during the Sprites'99 campaign. We estimated the electron energies from the intensity ratios of blue (350-500 nm) to red (560-800 nm) emissions captured separately by two array photometers on the assumption that the electron energy distribution is given by the Maxwell-Boltzmann or Druyvesteyn distribution. It is found that the electron energies reach their peaks preceding the luminosity peaks of the red emission (mostly due to the N-2 first positive and the N-2(+) Meinel band systems), exhibiting energy increases in the lower part of the sprite halo. The estimated peak electron energies are in the range 6-23 and 7-16 cV for the assumed Maxwell-Boltzmann and Druyvesteyn distribution, respectively. These results suggest that more energetic processes occur at the initiation of the sprite halo, particularly in its lower part. Nevertheless, the estimated values of electron energies Should be interpreted as a measure of the energetic processes producing sprite halos, represented by the equilibrium temperatures, since the real electron energy distributions would be undoubtedly deviated from the equilibrium states due to additional high-energy tails produced by the thermal runaway electron mechanism. (C) 2003 Elsevier Science Ltd. All rights reserved.
  • Y Takahashi, R Miyasato, T Adachi, K Adachi, M Sera, A Uchida, H Fukunishi
    JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS 65 5 551 - 560 2003年03月 [査読有り][通常論文]
     
    Sprites and elves observation has been carried out in three winter seasons in Japan since December 1998. Thirtyfive sprites' features have been imaged with CCD cameras and 95 optical emission from elves have been captured with hi-speed array photometers. The number of events observed on a night is dependent on the occurrence of intense cloud to ground lightning activity and cloud condition above the observation site. Most of the sprites/elves are directly associated with storms produced by a cold front passing over Japan. It is found that sprites/elves appear not only in the west coast of Japan but also above the Pacific Ocean. The average vertical length of winter sprites in the west cost is shorter than that of summer sprites in the US by about a factor of 2. The altitude of the causative thunderstorm for winter sprites and elves is comparatively lower than that of the summer events in the US and the horizontal width of the cloud is sometimes smaller than 30 km. The sprites' detection in winter in Japan suggests the possibility of winter sprite occurrence in Scandinavia and/or Israel where the climate condition is similar to Japan. (C) 2003 Elsevier Science Ltd. All rights reserved.
  • 池田 幸司, 高橋 芳幸
    The journal of veterinary medical science 63 9 1003 - 1008 社団法人日本獣医学会 2001年08月25日 
    核移植のレシピエントとなる豚卵子の成熟培養時間について検討した.はじめに成熟に要する時間を検討した結果, ほとんどの卵子は32時間で第二減数分裂中期(MII期)に到達した.ついで, 電気刺激(ES)とシクロヘキシミド(CHX)を用いた活性化法を検討した.32, 36, 42及び48時間培養した卵子は, ESとCHXで処理すると, ESのみの処理に比べ前核形成率は高かった.また, ESとCHXで活性化した単為活性化胚の胚盤胞への発育率は42時間培養した卵子が最も高く, 卵子成熟の完了にはMII期到達後さらに10時間程度の培養が必要であることが示唆された.最後に, 成熟培養33時間目(MII期到達直後)および44時間目に除核した卵子と血清飢餓培養した豚胎子繊維芽細胞を融合させて核移植胚を作出した.それぞれ成熟培養39〜40時間目(成熟完了前後)および50〜51時間目にESとCHXで活性化処理して核移植胚の発育を比較した.その結果, 胚盤胞への発育はMII期到達直後に除核して成熟完了時に活性化させて作出した核移植胚の方が高かった(13.6vs.1.8%).以上の結果から, 豚卵子の成熟完了にはMII期到達後も約10時間の培養が必要であり, 核移植のレシピエントとして使用する場合はMII期到達時に除核して成熟完了時に活性化処理すると核移植胚の発生率の高いことが示された.
  • The dynamics of the proton aurora in auroral breakup events
    Takahashi, Y, H. Fukunishi
    J. Geophys. Res. 106 45 - 63 2001年 [査読有り][通常論文]
  • Füllekrug, M, S. Constable, G. Heinson, M. Sato, Y. Takahashi, C. Price, E. Williams
    EOS 81 333  2000年07月 [査読有り][通常論文]
  • Fukunishi, H, Y. Takahashi, M. Sato, A. Shono, M. Fujito, Y. Watanabe
    Geophys. Res. Lett. 23 2973 - 2976 1997年12月 [査読有り][通常論文]
  • H Fukunishi, Y Takahashi, M Kubota, K Sakanoi, US Inan, WA Lyons
    GEOPHYSICAL RESEARCH LETTERS 23 16 2157 - 2160 1996年08月 [査読有り][通常論文]
     
    Observations of optical phenomena at high altitude above thunderstorms using a multichannel high-speed photometer and image intensified CCD cameras were carried out at Yucca. Ridge Field Station (40 degrees 40' N, 104 degrees 56' W), Colorado as part of the SPRITES'95 campaign from 15 June to August 6, 1995. These new measurements indicate that diffuse optical flashes with a duration of < 1 ms and a horizontal scale of similar to 100-300 km occur al 75-105 km altitude in the lower ionosphere just after the onset of cloud-to-ground lightning discharges, but preceding the onset of sprites. Here we designate these events as elves to distinguish them from red sprites''. This finding is consistent with the production of diffuse optical emissions due to the heating of the lower ionosphere by electromagnetic pulses generated by lightning discharges as suggested by several authors.

講演・口頭発表等

  • Optical characteristics of elves observed by FORMOSAT-2/ISUAL and properties of parent lightning discharges  [招待講演]
    Y. Takahashi, T. Adachi, A. Ohkubo, K. Yamamoto, S. Chikada, H. Fukunishi, H. _T. Su, A. B. Chen, R. _R. Hsu, S. B. Mende, H. U. Frey, L. C. Lee
    International Association of Meteorology and Atmospheric Sciences (IAMAS) 2005 meeting Beijing, China
  • Characteristics of TLEs observed by ISUAL/AP onboard FORMOSAT-2  [招待講演]
    Y. Takahashi, T. Adachi, H. Fukunishi, S. Chikada, A. Yoshida, K. Yamamoto, R-R. Hsu, H-T. Su, A. Chen, S. B. Mende, H. U. Frey, L-C. Lee
    American Geophysical Union (AGU) 2006 Fall meeting San Francisco, US
  • SPRITE-SAT mission for sprites and TGFs studies  [招待講演]
    Y. Takahashi, T. Sakanoi, M. Sato, S. Kondo, K. Yoshida, Y. Sakamoto, E. Ujiie, T. Takashima, U. Inan, D. Smith
    European Geoscience Union general assembly Vienna, Austria
  • Lifetime and structures of TLEs captured by high-speed camera on board aircraft  [招待講演]
    Y. Takahashi, Y. Sanmiya, M. Sato, T. Kudo, NHK Cosmic Shore Project, Y. Yair, S. A. Cummer
    American Geophysical Union 2012 Fall Meeting San Francisco, US
  • Role and Scope of Asian Micro-satellite Consortium  [招待講演]
    Yukihiro Takahashi
    34th Asia Conference on Remote Sensing “Applications of remote sensing technology on tropical peatlands” Bali, Indonesia
  • A Scope of Asian Micro-satellite Consortium  [招待講演]
    Yukihiro Takahashi
    IEEE Workshop on Geoscience and Remote Sensing 2013 Melaka, Malaysia
  • High frequency / precision disaster monitoring with micro-satellite constellation  [招待講演]
    Yukihiro Takahashi
    UN World Conference on Disaster Risk Reduction 2015 Sendai, Japan
  • Collaborative Promotion of Micro-satellite Utilization by International Consortium  [招待講演]
    Yukihiro Takahashi
    APRSAF-17 Manila, Philippines
  • Next-generation Earth Monitoring System with Micro-satellites and Ground-based Networks  [招待講演]
    Yukihiro Takahashi
    17th Conference of the Science Council of Asia Manila, Philippines

その他活動・業績

  • 山野辺晃大, 大矢浩代, 土屋史紀, 山下幸三, 高橋幸弘, 野崎憲朗, 塩川和夫, 中田裕之 大気電気学会誌(Web) 15 (1) 2021年
  • 菅野将史, 高橋幸弘, 大矢浩代, 中田裕之, 佐藤光輝, 久保田尚之, Purwadi 大気電気学会誌(Web) 15 (1) 2021年
  • 丸山慶, 庄子聖人, 大野夏樹, 大矢浩代, 土屋史紀, 津川卓也, 西岡未知, 山下幸三, 高橋幸弘, 中田裕之, 鷹野敏明 大気電気学会誌 13 (1) 2020年
  • K. Bandholnopparat, M. Sato, T. Adachi, T. Ushio, Y. Takahashi Journal of Atmospheric and Solar-Terrestrial Physics 189 87 -97 2019年08月01日 [査読無し][通常論文]
     
    © 2019 Elsevier Ltd We developed a new method to distinguish the lightning discharge type using lightning data obtained by JEM-GLIMS spaced-based mission and ground-based lightning network that are JLDN, NLDN, WWLLN, and GEON. As a first step, we selected 1057 lightning events detected by the JEM-GLIMS cameras (LSI) and spectrophotometers (PH) in 2014. Then, we compared the JEM-GLIMS optical data to the ground-based lightning data in order to check the simultaneous detection of JEM-GLIMS lightning events by the ground-based lightning networks, and finally we identified the discharge type of the JEM-GLIMS lightning events. We succeed in identifying 941 simultaneous lightning events and found that 582, 93, and 266 lightning events were IC, +CG, and -CG discharges, respectively. As a next step, we calculated intensity ratios between blue and red PH channels, i.e., 337nm/762 nm, 316nm/762 nm, 392nm/762 nm, 337nm/(599–900 nm), 316nm/(599–900 nm), and 392nm/(599–900 nm) for the 941 lightning events in order to specify the optical characteristics of IC, +CG, and -CG discharges. It is found that the PH intensity ratio of +CG discharges is the highest and that the PH intensity ratio of IC and -CG discharges is smaller than that of +CG discharge. We also found that the characteristics of the LSI intensity ratio are almost comparable to those of the PH intensity ratio. As the differences of the 337nm/762 nm, 337nm/(599–900 nm), and 392nm/(599–900 nm) ratio of IC, +CG, and -CG discharges are relatively large, these three ratios are a useful proxy for classifying the discharge types for additional 7349 lightning events detected by JEM-GLIMS in order to estimate the global ratio between IC and CG discharges (Z ratio).
  • R. Kitamura, Y. Hobara, M. Sato, Y. Takahashi, T. Adachi, T. Ushio, M. Suzuki 2019 URSI Asia-Pacific Radio Science Conference, AP-RASC 2019 2019年03月01日 [査読無し][通常論文]
     
    © 2019 URSI. All rights reserved. Recent study by [1] demonstrates the remarkable similarity between the time series of lightning optical irradiance observed by high speed photometric observations in GLIMS (Global LIghtning and sprite MeasurementS on JEMEF) mission installed in the International Space Station (ISS) and current moment change estimated by groundbased ELF magnetic field measurement based on 169 lightning strokes around Japan, which also indicates the high correlation between integrated irradiance and charge moment change (Qds).
  • 平松崇, 山浦秀作, 戸梶歩, 白坂成功, 鶴田佳宏, 青柳賢英, 松本健, 中須賀真一, 栗原純一, 高橋幸弘, 桑原聡文, 坂本祐二, 吉田和哉, 増井博一, KIM Sang-kyun, 奥山圭一, CHO Mengu, ANH Tuan Pham 宇宙科学技術連合講演会講演集(CD-ROM) 63rd 2019年
  • 齊藤誠一, 平田貴文, ALABIA Irene, 平譯享, 平譯享, 栗原純一, 高橋幸弘, 坂本祐二, 桑原聡文, 藤田伸哉, 羽生浩介, 村田悠, SAKAL Morokot, 冨尾蓮花, 佐藤悠司, LEE Ming-An, 望月貫一郎, 高橋文宏, 村上浩 日本海洋学会大会講演要旨集 2019 2019年
  • 高橋 幸弘, 今井 正尭, 佐藤 光輝 遊・星・人 = Planetary people : 日本惑星科学会誌 27 (1) 43 -45 2018年03月 [査読無し][通常論文]
  • 坂本祐二, 桑原聡文, 吉田和哉, 石田哲朗, 栗原純一, 高橋幸弘 宇宙科学技術連合講演会講演集(CD-ROM) 62nd 2018年
  • 栗原純一, 石田哲朗, 高橋幸弘, 長田亨 日本リモートセンシング学会学術講演会論文集(CD-ROM) 65th 2018年
  • 佐藤光輝, 高橋幸弘, 春山純一, 今井正尭 日本気象学会大会講演予稿集 (114) 2018年
  • 山下幸三, 岩崎博之, 大矢浩代, 高橋幸弘 大気電気学会誌 12 (1) 2018年
  • 丸山慶, 大矢浩代, 土屋史紀, 山下幸三, 高橋幸弘, 中田裕之, 鷹野敏明 地球電磁気・地球惑星圏学会総会及び講演会(Web) 144th 2018年
  • 清水千春, 佐藤光輝, 高橋幸弘, 本郷保二, 土屋史紀, 阿部修司, 吉川顕正 大気電気学会誌 11 (1) 59‐60 2017年11月15日 [査読無し][通常論文]
  • 鈴木克徳, 柿沼遠方, 芳原容英, 佐藤光輝, 高橋幸弘, 足立透, 牛尾知雄, 河崎善一郎, 森本健志, 山崎敦, 鈴木睦, LINSCOTT I. R, INAN U. S 大気電気学会誌 11 (1) 102‐103 2017年11月15日 [査読無し][通常論文]
  • 石田哲朗, 栗原純一, 高橋幸弘 日本リモートセンシング学会学術講演会論文集(CD-ROM) 63rd 2017年
  • 芳原容英, 鈴木克徳, 柿沼遠方, 佐藤光輝, 高橋幸弘, 足立透, 牛尾知雄, 河崎善一郎, 森本健志, 山崎敦, 鈴木睦, LINSCOTT Ivan, INAN Umran 日本地球惑星科学連合大会予稿集(Web) 2017 ROMBUNNO.MIS05‐06 (WEB ONLY) 2017年 [査読無し][通常論文]
  • BANDHOLNOPPARAT Kittanapat, SATO Mitsuteru, TAKAHASHI Yukihiro, ADACHI Toru, USHIO Tomoo 日本地球惑星科学連合大会予稿集(Web) 2017 ROMBUNNO.MIS05‐P03 (WEB ONLY) 2017年 [査読無し][通常論文]
  • 今村 剛, 中村 正人, 田口 真, 佐藤 毅彦, 岩上 直幹, 高橋 幸弘, 渡部 重十, 山崎 敦 宇宙科学技術連合講演会講演集 60 4p 2016年09月06日
  • 石田 哲朗, 高橋 幸弘, 栗原 純一, 長妻 努 宇宙科学技術連合講演会講演集 60 3p 2016年09月06日 [査読無し][通常論文]
  • 栗原 純一, 高橋 幸弘 宇宙科学技術連合講演会講演集 60 3p 2016年09月06日 [査読無し][通常論文]
  • 中村 正人, 山﨑 敦, 田口 真, 岩上 直幹, 佐藤 毅彦, 高橋 幸弘, 今村 剛 遊・星・人 = Planetary people : 日本惑星科学会誌 25 (1) 4 -7 2016年03月 
    金星探査機「あかつき」は2015年12月に金星周回軌道に入った.日本初の惑星周回機の誕生である.観測機器の初期チェックは順調に進んでいる.中村プロジェクトマネージャーと観測機器担当者が所感を記す.
  • Masato Nakamura, Nobuaki Ishii, Takeshi Imamura, Takehiko Satoh, Takumi Abe, Chikako Hirose, Atsushi Yamazaki, Junichi Nakatsuka, Tsutomu Ichikawa, Tomoaki Toda, Hiroyuki Toyoda, Sumitaka Tachikawa, Yukio Kamata, Makoto Suzuki, Takao M. Sato, Shin Ya Murakami, Yukio Yamamoto, Naomoto Iwagami, Makoto Taguchi, Tesuya Fukuhara, Shigeto Watanabe, Yukihiro Takahashi, Munetaka Ueno, Manabu Yamada, George L. Hashimoto, Naru Hirata, Toru Kouyama, Kazunori Ogohara, Hiroki Ando, Koichiro Sugiyama, Hiroki Kashimura, Shoko Ohtsuki Proceedings of the International Astronautical Congress, IAC 2016年01月01日 [査読無し][通常論文]
     
    Copyright © 2016 by the International Astronautical Federation (IAF). All rights reserved. Japan's Venus Climate Orbiter Akatsuki was proposed to ISAS (Institute of Space and Astronautical Science) in 2001 as an interplanetary mission. We made 5 cameras with narrow-band filters to image Venus at different wavelengths to track the cloud and minor components distribution at different heights to study the Venusian atmospheric dynamics in 3 dimension. It was launched on May 21st, 2010 and reached Venus on December 7th, 2010. With the thrust by the orbital maneuver engine, Akatsuki tried to go into the westward equatorial orbit around Venus with the 30 hours' orbital period, however it failed by the malfunction of the propulsion system. Later the spacecraft has been orbiting the sun for 5 years. On December 7th, 2015 Akatsuki met Venus again after the orbit control and Akatsuki was put into the westward equatorial orbit whose apoapsis is about 0.44 million km and orbital period of 14 days. Its main target is to shed light on the mechanism of the fast atmospheric circulation of Venus. The systematic imaging sequence by Akatsuki is advantageous for detecting meteorological phenomena with various temporal and spatial scales. We have five photometric sensors as mission instruments for imaging, which are 1 m-infrared camera (IR1), 2 m-infrared camera (IR2), ultra-violet imager (UVI), long-wave infrared camera (LIR), and lightning and airglow camera (LAC). These photometers except LIR have changeable filters in the optics to image in certain wavelengths. Akatsuki's long elliptical orbit around Venus is suitable for obtaining cloud-tracked wind vectors over a wide area continuously from high altitudes. With the observation, the characterizations of the meridional circulation, mid-latitude jets, and various wave activities are anticipated. The technical issues of Venus orbit insertion in 2015 and the scientific new results will be given in this paper.
  • 佐藤光輝, 平木康隆, 足立透, 牛尾知雄, 森本健志, 菊池博史, 鈴木睦, 山崎敦, 高橋幸弘 地球電磁気・地球惑星圏学会総会及び講演会(Web) 140th ROMBUNNO.R005‐P18 (WEB ONLY) 2016年 [査読無し][通常論文]
  • 佐藤光輝, 足立透, 佐藤剛志, 牛尾知雄, 森本健志, 鈴木睦, 山崎敦, 高橋幸弘 日本地球惑星科学連合大会予稿集(Web) 2016 ROMBUNNO.PEM16‐12 (WEB ONLY) 2016年 [査読無し][通常論文]
  • 佐藤剛志, 佐藤光輝, 牛尾知雄, 森本健志, 足立透, 鈴木睦, 山崎敦, 高橋幸弘 日本地球惑星科学連合大会予稿集(Web) 2016 ROMBUNNO.PEM16‐P04 (WEB ONLY) 2016年 [査読無し][通常論文]
  • SHIMIZU Chiharu, SATO Mitsuteru, TAKAHASHI Yukihiro, TSUCHIYA Fuminori, HONGO Yasuji, ABE Shuji, YOSHIKAWA Akimasa 地球電磁気・地球惑星圏学会総会及び講演会(Web) 140th ROMBUNNO.R005‐P02 (WEB ONLY) 2016年 [査読無し][通常論文]
  • M. Sato, M. Mihara, T. Adachi, T. Ushio, T. Morimoto, M. Kikuchi, H. Kikuchi, M. Suzuki, A. Yamazaki, Y. Takahashi, U. Inan, I. Linscott, R. Ishida, Y. Sakamoto, K. Yoshida, Y. Hobara Journal of Geophysical Research 121 (7) 3171 -3194 2016年01月01日 [査読無し][通常論文]
     
    © 2016. American Geophysical Union. All Rights Reserved. Global Lightning and Sprite Measurements on Japanese Experiment Module (JEM-GLIMS) started the nadir observations of lightning discharges and transient luminous events (TLEs) from the International Space Station (ISS) since November 2012. In the nadir observations, JEM-GLIMS optical instruments have to simultaneously detect incomparably intense lightning emissions and weak TLE emissions. To distinguish TLEs, especially sprite events, from lightning events, combined data analytical methods are adopted: (1) a subtraction of the wideband camera image from the narrowband camera image, (2) a calculation of the intensity ratio between different photometer channels, and (3) an estimation of the polarization and charge moment changes for the TLE-producing lightning discharges. We succeeded in identifying numbers of sprite events using the combined analytical methods, and here we report three sprite events detected by JEM-GLIMS as a case study. In the subtracted images, sprite emissions are located over the area of the sprite-producing lightning emissions. However, these sprites and sprite-producing lightning discharges did not occur at the nadir point of the ISS. For this reason, the geometry conversion of the sprite and sprite-producing lightning emissions as observed from the point just over the sprite-producing lightning discharges is performed. In the geometry-converted images, the locations of the sprite emissions are clearly displaced by 8-20 km from the peak positions of the sprite-producing lightning emissions. Thus, the first quantitative spatial distributions of sprites and sprite-producing lightning discharges from the JEM-GLIMS nadir observations are revealed.
  • 小林 ゆい, 渡邊 恭也, 今井 正尭, 渡辺 健介, 成瀬 延康, 高橋 幸弘, 根本 征樹 雪氷研究大会講演要旨集 2016 (0) 2016年 [査読無し][通常論文]
  • 山下 幸三, 高橋 幸弘 電子情報通信学会ソサイエティ大会講演論文集 2015 (1) 229 -229 2015年08月25日
  • 若生 一広, 栗原 純一, 高橋 幸弘 電気評論 100 (8) 73 -76 2015年08月 [査読無し][通常論文]
  • 鈴木克徳, 柿沼遠方, 芳原容英, LINSCOTT I.R, INAN U.S, 佐藤光輝, 高橋幸弘, 牛尾知雄, 河崎善一郎, 森本健志, 山崎敦, 鈴木睦 大気電気学会誌 9 (1) 92 -93 2015年04月20日 [査読無し][通常論文]
  • 春山純一, 高橋幸弘, 佐藤光輝 日本惑星科学会秋季講演会予稿集(Web) 2015 2015年
  • 牛尾 知雄, 佐藤 光輝, 鈴木 睦, 森本 健志, 菊池 博史, 菊池 雅行, 足立 透, 山崎 敦, 高橋 幸弘, Inan U., Lhscott I., 石田 良平, 坂本 祐二, 吉田 和哉, 芳原 容英, 阿部 琢己, 中村 正人, 織田 裕久 大会講演予講集 108 380 -380 2015年
  • 前田惇徳, 田口真, 荘司泰弘, 中野壽彦, 今井正尭, 合田雄哉, 高橋幸弘, 渡辺誠, 吉田和哉, 坂本祐二 地球電磁気・地球惑星圏学会総会及び講演会予稿集(CD-ROM) 138th 2015年
  • 山下幸三, 高橋幸弘, 大矢浩代, 土屋史紀 電子情報通信学会大会講演論文集(CD-ROM) 2015 2015年
  • 鈴木克徳, 柿沼遠方, 芳原容英, LINSCOTT Ivan, INAN Umran, 佐藤光輝, 高橋幸弘, 牛尾知雄, 河崎善一郎, 森本健志, 山崎敦, 鈴木睦 日本地球惑星科学連合大会予稿集(Web) 2015 ROMBUNNO.PEM11‐12 (WEB ONLY) 2015年 [査読無し][通常論文]
  • 石丸 亮, 坂本 祐二, 小林 正規, 郷内 稔也, 藤田 伸哉, 千秋 博紀, 和田 浩二, 石橋 高, 黒澤 耕介, 山田 学, 阿部 新助, 吉田 和哉, 佐藤 光輝, 高橋 幸弘, 松井 孝典 日本惑星科学会秋期講演会予稿集 2014 "O13 -03" 2014年09月10日 [査読無し][通常論文]
  • 今井 正尭, 高橋 幸弘, 渡部 重十, 渡邊 誠 日本惑星科学会秋期講演会予稿集 2014 "P1 -04" 2014年09月10日 [査読無し][通常論文]
  • 春山 純一, 高橋 幸弘, 佐藤 光輝 日本惑星科学会秋期講演会予稿集 2014 "P2 -31" 2014年09月10日 [査読無し][通常論文]
  • Takahashi Yukihiro, Haruyama Jun-ichi, Sato Mitsuteru Proceedings of the ISAS Lunar and Planetary Symposium 46 3p 2014年08月05日
  • 佐藤 光輝, 山本 真行, 石坂 圭吾, 高橋 幸弘, 小郷原 一智, 鴨川 仁, 宮本 英昭, 阿部 琢美, Sato Mitsuteru, Yamamoto Masayuki, Ishisaka Keigo, Takahashi Yukihiro, Ogohara Kazunori, Kamogawa Masashi, Miyamoto Hideaki, Abe Takumi 第47回月・惑星シンポジウム = Proceedings of the 47th ISAS Lunar and Planetary Symposium 2014年08月 
    第47回月・惑星シンポジウム (2014年8月4日-6日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)), 相模原市, 神奈川県形態: カラー図版あり資料番号: SA6000033004
  • 佐藤光輝, 三原正大, 高橋幸弘, 足立透, 牛尾知尾, 森本健志, 鈴木睦, 山崎敦, 菊池雅行, INAN U, LINSCOTT I 大気電気学会誌 8 (1) 37 2014年04月18日 [査読無し][通常論文]
  • 栗原 純一, 高橋 幸弘, 武山 芸英 O plus E : Optics・Electronics 36 (4) 398 -401 2014年04月 [査読無し][通常論文]
  • 莊司 泰弘, 田口 真, 中野 壽彦, 前田 惇徳, 高橋 幸弘, 今井 正尭, 仲本 純平, 渡辺 誠, 合田 雄哉, 川原 健史, 吉田 和哉, 坂本 祐二 宇宙航空研究開発機構研究開発報告 13 (13-011) 87 -105 2014年03月 [査読無し][通常論文]
     
    地上望遠鏡を使った高分解能光学撮像において,シーイングは最も重要な条件である.成層圏環境は気流が安定しており,密度も地上の 1/100程度と,天体の光学観測に適している.このような成層圏環境の利点を活用することによって,口径が 1 m以下の比較的小規模な望遠鏡でも,口径数 mの地上大型望遠鏡に匹敵する分解能での観測が可能になると期待される.この点に着目して我々は惑星観測を行うための極周回成層圏テレスコープ(風神, FUJIN)を提案し, 2002年より開発を行ってきた. 2009年にはプロトタイプによる最初の飛翔試験を実施したものの,飛翔中に搭載 CPUがハングアップしたため十分な成果を残すことができなかった.再度 2013年に国内で飛翔実験するために,発生した不具合等に対処した FUJIN-1システムを開発した.飛翔実験自体は気象条件が整わず,また気球飛翔制御システムに問題が発生したために実施できなかったものの, FUJIN-1システムはポインティング機能の性能確認を中心とした地上試験を経て,完全なフライトレディ状態で待機していた.地上でのポインティング性能確認試験によって, FUJIN-1搭載望遠鏡の回折限界未満である 0.4"(σ)のポインティング精度を確認した.この結果を受けて FUJIN-1の開発を終了し,極域での実験を行うため FUJIN-2の開発を開始した.本稿では FUJINの概要を説明し,今回開発した FUJIN-1システムと地上ポインティング試験について述べる.
  • 高橋 幸弘 プラズマ・核融合学会誌 90 (2) 128 -131 2014年02月25日 [査読無し][通常論文]
     
    最近,太陽自転周期である27日程度の大気変動がみつかっている.ここでは特に西太平洋における雲変動に焦点を当てて紹介する.従来,11年周期についての調査は多くなされてきたが,それらは振幅が小さく,測定誤差の問題が指摘されているが,1ヶ月程度の周期変動は振幅が数10%を超えることもある.本節では,全球の積乱雲活動の指標であるシューマン共鳴現象と,衛星から観測される雲の変動が,共に太陽極大期のみ27日の周期性を示すことを紹介する.また,太陽振幅ではなく,周期が11年周期の太陽活動に関連していることを指摘し,それがエルニーニョなどより長い時間変動に影響している可能性を議論する.
  • 高橋 幸弘 プラズマ・核融合学会誌 90 (2) 137 -140 2014年02月25日 [査読無し][通常論文]
     
    積乱雲による発電を駆動源とし,地面と電離圏が成す巨大な球殻コンデンサーを基本構造とし,磁気圏・電離圏電流とも結合している可能性のある地球規模の電流回路-全地球回路(グローバルサーキット)-は,その仮説提唱から80年以上経つ今も十分定量的な理解に至っていない.しかし,その回路で運ばれるイオンや電場は,雲の生成・発達・消滅や雲頂高度に作用し,気候変動にも関与している可能性が指摘されている.
  • 足立 透, 佐藤 光輝, 牛尾 知雄, 山崎 敦, 鈴木 睦, 菊池 雅行, 高橋 幸弘, Inan Umran, Linscott Ivan, 芳原 容英, Cohen M. B., Lu G., Cummer S. A., Hsu R. R., Chen A. B., Frey H. U. 大会講演予講集 105 296 -296 2014年
  • 前田惇徳, 田口真, 吉田和哉, 坂本祐二, 中野壽彦, 荘司泰弘, 高橋幸弘, 仲本純平, 今井正尭, 渡辺誠, 合田雄哉 地球電磁気・地球惑星圏学会総会及び講演会予稿集(CD-ROM) 136th 2014年
  • 坂本祐二, 杉村伸雄, 冨岡義弘, 桑原聡文, 吉田和哉, 栗原純一, 福原哲哉, 高橋幸弘 宇宙科学技術連合講演会講演集(CD-ROM) 58th ROMBUNNO.1K07 2014年 [査読無し][通常論文]
  • 今井 正尭, 高橋 幸弘, 渡部 重十, 渡邊 誠 日本惑星科学会秋期講演会予稿集 2013 "P3 -30" 2013年11月20日 [査読無し][通常論文]
  • 栗原 純一, 高橋 幸弘, 桑原 総文 宇宙科学技術連合講演会講演集 57 4p 2013年10月09日 [査読無し][通常論文]
  • 山下 幸三, 高橋 幸弘, 松本 淳, 濱田 純一 電子情報通信学会ソサイエティ大会講演論文集 2013 (1) 50 -50 2013年09月03日 [査読無し][通常論文]
  • 桑原聡文, 坂本祐二, 吉田和哉, 栗原純一, 高橋幸弘, 高田淳史, 山川宏 宇宙科学技術連合講演会講演集(CD-ROM) 57th 2013年
  • 工藤 剛史, 高橋 幸弘, 佐藤 光輝, 岩崎 博之, 長 康平 大会講演予講集 104 78 -78 2013年
  • 足立 透, 佐藤 光輝, 牛尾 知雄, 山崎 敦, 鈴木 睦, 菊池 雅行, 高橋 幸弘, Inan Umran, Linscott Ivan, 芳原 容英 大会講演予講集 104 79 -79 2013年
  • 佐藤光輝, 牛尾知雄, 森本健志, 足立透, 鈴木睦, 山崎敦, 菊池雅行, 高橋幸弘, INAN Umran, LINSCOTT Ivan, 芳原容英 大気圏シンポジウム・講演集(Web) 27th III-4 (WEB ONLY) 2013年 [査読無し][通常論文]
  • 佐藤光輝, 足立透, 牛尾知雄, 森本健志, 鈴木睦, 山崎敦, 菊池雅行, 高橋幸弘, INAN Umran, LINSCOTT Ivan, 芳原容英 地球電磁気・地球惑星圏学会総会及び講演会予稿集(CD-ROM) 134th ROMBUNNO.S001-07 2013年 [査読無し][通常論文]
  • 牛尾 知雄, 森本 健志, 佐藤 光輝, 鈴木 睦, 山崎 敦, 芳原 容英, 菊地 雅行, 高橋 幸弘, INAN Umran, 石田 良平, 坂本 祐二, 吉田 和哉, 阿部 琢美, 河崎 善一郎 大気電気学会誌 = / Society of Atmospheric Electricity of Japan 6 (2) 2012年11月15日 [査読無し][通常論文]
  • 濱本 昂, 高橋 幸弘, 渡辺 誠 大会講演予講集 102 148 -148 2012年09月30日 [査読無し][通常論文]
  • 小林 直樹, 高橋 芳幸, 鈴木 絢子, 和田 浩二 遊・星・人 : 日本惑星科学会誌 21 (3) 324 -329 2012年09月25日 
    2012年7月24日,神戸大学惑星科学研究センター内の講義室にて「惑星科学の今後を考える会」なる催しが開かれた.本稿はその会議の参加記録であり,紹介である. 1992年に惑星科学会が発足して以来20年の歳月が流れた.その間,惑星探査,大型望遠鏡観測,大規模シミュレーション科学等の大型プロジェクトに関わる研究者も増え,拠点と呼ばれる組織も生まれてきた.本会では惑星科学コミュニティにおけるそうした拠点組織の持つ役割と課題を整理し,現状認識を深め,大型プロジェクト研究を推進できる力を持つコミュニティの今後のあり方について議論した.
  • 高橋 幸弘 遊・星・人 : 日本惑星科学会誌 21 (3) 195 -195 2012年09月25日
  • 高橋 幸弘 遊・星・人 : 日本惑星科学会誌 21 (3) 2012年09月25日 [査読無し][通常論文]
  • 高橋 幸弘, 佐藤 光輝, 福原 哲哉, 栗原 純一, 中島 健介, 竹内 覚, ヨアブ ヤイル, フィッシャー ゲオルグ, アプリン カレン 遊・星・人 : 日本惑星科学会誌 21 (3) 224 -228 2012年09月25日 [査読無し][通常論文]
     
    近年,木星大気の大規模構造を決める力学や,大気組成を決める化学過程を理解する上で,積乱雲や雷放電観測の重要性が指摘されている.しかし,対流強度は雲頂高度など雲本体の観測のみからでは難しい.雷放電発光の強度,頻度,高度の情報はそれを補う優れた指標のひとつであるが,通常のカメラでは時間分解能が不十分で,積乱雲活動の定量的な評価は困難である.ここで提案する雷放電発光検出器"OLD"は,高速撮像・画像処理によって雷放電発光の頻度から対流活動強度を求め,また色情報から高度推定することを可能にする.
  • 山下 幸三, 大矢 浩代, 土屋 史紀, 高橋 幸弘, 松本 淳 電子情報通信学会ソサイエティ大会講演論文集 2012 (1) 2012年08月28日 [査読無し][通常論文]
  • 吉田 和哉, 坂本 祐二, クワ]原 聡文, 高橋 幸弘 計測と制御 = Journal of the Society of Instrument and Control Engineers 51 (5) 438 -443 2012年05月10日 [査読無し][通常論文]
  • 高橋 幸弘 計測と制御 = Journal of the Society of Instrument and Control Engineers 51 (5) 445 -448 2012年05月10日 [査読無し][通常論文]
  • 木村 真一, 中須賀 真一, 郷田 直輝, 山本 雅也, 岩崎 晃, 倉原 直美, 吉田 和哉, 高橋 幸弘 日本航空宇宙学会誌 60 (4) 137 -148 2012年04月05日 [査読無し][通常論文]
     
    近年,従来の数トン級衛星ではなく,100〜500kgの「小型衛星」が世界各国の地図作成,安全保障,防災,都市計画,自然環境・気象観測,農産物の生産管理,科学調査等の様々な分野に利用され,また,大学・研究機関・企業等の宇宙利用のニーズが高まってきた.こうした状況に合わせ,日本航空宇宙学会誌では計測自動制御学会誌と共同特集企画として,主に超小型衛星の利用に焦点を当てた特集「小型衛星を用いたセンシングアプリケーション」を掲載することとした.日本航空宇宙学会誌では,計測自動制御学会の特集号に先立ち,その特集号にて掲載される内容をダイジェスト版として紹介する.
  • 三宮 佑介, 高橋 幸弘, 佐藤 光輝, 山下 幸三 大会講演予講集 102 565 -565 2012年
  • 高橋幸弘, 吉川顕正, 山本衛 地球電磁気・地球惑星圏学会総会及び講演会予稿集(CD-ROM) 132nd 2012年
  • 高橋幸弘, 福原哲哉, 濱本昂, 尾崎彰士, 渡辺誠, 田中培生, 大月祥子, 神山徹 大気圏シンポジウム・講演集(Web) 26th 2012年
  • 濱本昂, 高橋幸弘, 尾崎彰士, 渡辺誠 大気圏シンポジウム・講演集(Web) 26th 2012年
  • 田口真, 山元夢摘, 吉田和哉, 坂本祐二, 中野壽彦, 荘司泰弘, 高橋幸弘, 渡辺誠, 濱本昂, 今井正尭, 仲本純平 日本天文学会年会講演予稿集 2012 2012年
  • 桑原聡文, 坂本祐二, 吉田和哉, 栗原純一, 高橋幸弘, 高田淳史, 山川宏 宇宙科学技術連合講演会講演集(CD-ROM) 56th ROMBUNNO.2M12 2012年 [査読無し][通常論文]
  • 今井 正尭, 高橋 幸弘, 渡辺 誠, 濱本 昂 大会講演予講集 102 147 -147 2012年 [査読無し][通常論文]
  • Mitsuteru Sato, Yukihiro Takahashi, Masayuki Kikuchi, Makoto Suzuki, Atsushi Yamazaki, Tomoo Ushio IEEJ Transactions on Fundamentals and Materials 131 (12) 994 -999 2011年12月01日 [査読無し][通常論文]
     
    Lightning and Sprite Imager (LSI) is a science instrument of JEM-GLIMS to capture images of lightning discharges and upper atmospheric transient luminous events (TLEs), such as sprites, elves and blue jets. LSI consists of two CMOS cameras; one is a wide-band camera named LSI-1 that is equipped with an optical filter whose pass-band ranges from 765nm to 830nm, the other is a narrow-band camera named LSI-2 that is equipped with an optical filter whose transmittance centers at the wavelength of 762 nm and has band width of 14 nm. From the comparison of LSI-1 images with LSI-2 images the time evolution and spatial distribution of lightning discharges and TLEs can be identified. Since the telemetry speed provided for JEM-GLIMS is limited, LSI images will be acquired not continuously but intermittently according to the onboard event trigger logic. This trigger logic selects only the transient optical flashes caused by lightning discharges or TLEs effectively. © 2011 The Institute of Electrical Engineers of Japan.
  • Mitsuteru Sato, Yukihiro Takahashi, Makoto Suzuki, Atsushi Yamazaki, Tomoo Ushio IEEJ Transactions on Fundamentals and Materials 131 (12) 1000 -1005 2011年12月01日 [査読無し][通常論文]
     
    Six-channel spectrophotometers (PH) are the science instruments of JEM-GLIMS to measure absolute intensity of the emission originated from lightning discharges and upper atmospheric transient luminous events (TLEs). PH unit-1 (PH-U1) consists of four spectrophotometer channels named from PH1 to PH4, while PH unit-2 (PH-U2) two spectrophotometer channels named PH5 and PH6. Optical filters of these spectrophotometers are selected to detect TLE emission lines of N21PG, N22PG, N+21NG, and N2LBH. Since the bandwidth of the optical filter of PH2,3,5, and 6 is 10 nm and since PH1 measures NUV emission, photomultiplier tubes with high-voltage converters are used as a photon detector. To the contrary, PH4 uses a photodiode as a photon detector because the pass-band of the optical filter is enough wide to detect transient optical emission. Though PH does not equip spatial resolution, it can acquire light curve data with a high time resolution of 50 μs with a 12-bit resolution. Thus, the combinational analysis of PH data and Lightning and Sprite Imager (LSI) data, it is possible to clarify the relationship between TLEs and their parent lightning discharges, the occurrence condition of TLEs, and the energy of the electrons which excite TLE emission. © 2011 The Institute of Electrical Engineers of Japan.
  • 高橋 幸弘, 福原 哲哉, 栗原 純一 電子情報通信学会技術研究報告. SANE, 宇宙・航行エレクトロニクス 111 (239) 33 -35 2011年10月10日 [査読無し][通常論文]
     
    現在日本では複数の50kgクラスの超小型衛星のプロジェクトが進んでいるが、今後このクラスの衛星が市民権を得て成功していくためには、ミッション、中でもリモートセンシングの性能を向上させることが鍵となる。北海道大学では、RISING及びRISING-2のふたつの衛星の開発を通して、これまでにない、超小型衛星に適した高性能・高機能、かつ安価な光学センサーの開発を進めている。本発表では、それらの開発の現状と展望について紹介する。
  • 坂本 祐二, 桑原 聡文, 吉田 和哉, 高橋 幸弘 年次大会 : Mechanical Engineering Congress, Japan 2011 "S192025 -1"-"S192025-3" 2011年09月11日 [査読無し][通常論文]
     
    The development of 50-kg class microsatellite RISING-2 was started in July, 2009 by Tohoku Univ. and Hokkaido Univ. At the time of May, 2011, the fabrication and evaluation tests of engineering model (EM) and the fabrication of flight model (FM) were finished. The launch opportunity has been not decided yet. The satellite has a telescope with 10-cm diameter and 1-m focal length, and the resolution of image is 5 meters. It observes multi-spectrum images of cumulonimbus clouds using liquid crystal tunable filter as well as RGB color photos. Also, transient luminous events in upper atmosphere such as sprite are observed using CMOS sensors. This paper shows the final specifications of FM, and the verification tests of bus system.
  • 坂本 祐二, 桑原 聡文, 吉田 和哉, 高橋 幸弘 スペース・エンジニアリング・コンファレンス講演論文集 : Space Engineering Conference 2010 (19) "F3 -1"-"F3-6" 2011年01月27日 [査読無し][通常論文]
     
    Tohoku University and Hokkaido University started the development of a new 50-kg microsatellite RISING-2 at July 2009. This satellite inherits the development technique of RISING (SPRITE-SAT) launched on January 2009. The progress is shown in this paper. Using a Cassegrain telescope with 10-cm diameter and 1-m focal length, earth surface is observed with 5-m resolution from 700-km-alt sun synchronous orbit. By 3-axis attitude stabilization using reaction wheels and star sensors, the designated area on earth surface can be observed. In addition to color images, multi-spectrum images of cumulonimbus are observed by using a liquid crystal tunable filter. As a secondary mission, transient luminous events such as sprite are observed, which is same mission as SPRITE-SAT.
  • M. Nakamura, T. Imamura, N. Ishii, T. Abe, T. Satoh, M. Suzuki, M. Ueno, A. Yamazaki, N. Iwagami, S. Watanabe, M. Taguchi, T. Fukuhara, Y. Takahashi, M. Yamada, N. Hoshino, S. Ohtsuki, K. Uemizu, G. L. Hashimoto, M. Takagi, Y. Matsuda, K. Ogohara, N. Sato, Y. Kasaba, T. Kouyama, N. Hirata, R. Nakamura, Y. Yamamoto, N. Okada, T. Horinouchi, M. Yamamoto, Y. Hayashi Earth, Planets and Space 63 (5) 443 -457 2011年 [査読無し][通常論文]
     
    The Akatsuki spacecraft of Japan was launched on May 21, 2010. The spacecraft planned to enter a Venusencircling near-equatorial orbit in December 7, 2010 however, the Venus orbit insertion maneuver has failed, and at present the spacecraft is orbiting the Sun. There is a possibility of conducting an orbit insertion maneuver again several years later. The main goal of the mission is to understand the Venusian atmospheric dynamics and cloud physics, with the explorations of the ground surface and the interplanetary dust also being the themes. The angular motion of the spacecraft is roughly synchronized with the zonal flow near the cloud base for roughly 20 hours centered at the apoapsis. Seen from this portion of the orbit, cloud features below the spacecraft continue to be observed over 20 hours, and thus the precise determination of atmospheric motions is possible. The onboard science instruments sense multiple height levels of the atmosphere to model the three-dimensional structure and dynamics. The lower clouds, the lower atmosphere and the surface are imaged by utilizing nearinfrared windows. The cloud top structure is mapped by using scattered ultraviolet radiation and thermal infrared radiation. Lightning discharge is searched for by high speed sampling of lightning flashes. Night airglow is observed at visible wavelengths. Radio occultation complements the imaging observations principally by determining the vertical temperature structure. Copyright © The Society of Geomagnetism and Earth Planetary and Space Sciences (SGEPSS).
  • 濱本昂, 高橋幸弘, 渡辺誠, 渡部重十, 福原哲哉, 佐藤光輝 地球電磁気・地球惑星圏学会総会及び講演会予稿集(CD-ROM) 130th 2011年
  • 渡辺誠, 高橋幸弘, 渡部重十, 佐藤光輝, 福原哲也, 濱本昂, 徂徠和夫, 中尾光, 田中培生, 館内謙, 関口朋彦 日本天文学会年会講演予稿集 2011 2011年
  • 舘内謙, 田中培生, 山室智康, 川端拡信, 高橋英則, 渡部重十, 高橋幸弘, 佐藤光輝, 渡辺誠, 福原哲哉, 濱本昂 日本天文学会年会講演予稿集 2011 2011年
  • 渡辺誠, 高橋幸弘, 渡部重十, 佐藤光輝, 福原哲也, 濱本昂 日本天文学会年会講演予稿集 2011 2011年
  • 高橋幸弘, 栗原純一 宇宙科学技術連合講演会講演集(CD−ROM) 55th ROMBUNNO.3S13 2011年 [査読無し][通常論文]
  • 牛尾 知雄, 佐藤 光輝, 森本 健志, 鈴木 睦, 菊地 博史, 山崎 敦, 高橋 幸弘, 芳原 容英, 坂本 祐二, 石田 良平, 菊池 雅行, 吉田 和哉, 河崎 善一郎 電気学会論文誌. A, 基礎・材料・共通部門誌 = The transactions of the Institute of Electrical Engineers of Japan. A, A publication of Fundamentals and Materials Society 131 (1) 16 -20 2011年 [査読無し][通常論文]
     
    Lightning and sprite measurement sensors on the International Space Station (ISS) are introduced in this paper. Lightning is an electrical discharge which neutralizes the charge inside thunderstorm. In the early 1990s, optical transient luminous events (TLEs) occurring just above the thunderstorm were firstly reported by the US scientists and are associated with positive cloud-to-ground discharges with a large amount of charge. Though the luminous events so-called sprite, elves and jets have been investigated by numerous researchers all over the world based mainly on the ground observations, some important problems have not been fully understood yet such as generation mechanisms of columniform fine structure and horizontal offset of some sprites from the parent lightning discharges. In the JEM-GLIMS mission, observations from our synchronized sensors are going to shed light on above-mentioned unsolved problems regarding TLEs as well as causative lighting discharges. Our goals are (1) to detect and locate lightning and sprite within storm scale resolution over a large region of the Earth's surface along the orbital track of the ISS without any bias, (2) to clarify the generation mechanism of sprite, and (3) to identify the occurrence conditions of TLEs.
  • 大谷 栄治, 木村 淳, 高橋 幸弘, 中島 健介, 中本 泰史, 三好 由純, 小林 憲正, 山岸 明彦, 並木 則行, 小林 直樹, 出村 裕英, 倉本 圭, 大槻 圭史, 今村 剛, 寺田 直樹, 渡部 重十, 荒川 政彦, 伊藤 孝士, 圦本 尚義, 渡部 潤一 日本惑星科学会誌遊星人 20 (4) 349 -365 2011年 [査読無し][通常論文]
     
    「月惑星探査の来たる10年」検討では第一段階で5つのパネルの各分野に於ける第一級の科学について議論した.そのとりまとめを報告する.地球型惑星固体探査パネルでは,月惑星内部構造の解明,年代学・物質科学の展開による月惑星進化の解明,固体部分と結合した表層環境の変動性の解明,が挙げられた.地球型惑星大気・磁気圏探査パネルは複数学会に跨がる学際性を考慮して,提案内容に学会間で齟齬が生じないように現在も摺り合わせを進めている.本稿では主たる対象天体を火星にしぼって第一級の科学を論じる.小天体パネルでは始原的・より未分化な天体への段階的な探査と,発見段階から理解段階へ進むための同一小天体の再探査が提案された.木星型惑星・氷衛星・系外惑星パネルは広範な科学テーマの中から,木星の大気と磁気圏探査,氷衛星でのハビタブル環境の探査,系外惑星でも生命存在可能環境と生命兆候の発見について具体的な議論を行った.アストロバイオロジーパネルでは現実的な近未来の目標として火星生命探査を,長期的な目標として氷衛星・小天体生命探査を目指した観測装置開発が検討された.これらのまとめを元に「月惑星探査の来たる10年」検討は2011年7月より第二段階に移行し,ミッション提案・観測機器提案の応募を受け付けた.
  • 牛尾 知雄, 佐藤 光輝, 森本 健志, 鈴木 睦, 菊地 博史, 山崎 敦, 高橋 幸弘, 芳原 容英, INAN Umran, 石田 良平, 河崎 善一郎 電気学会研究会資料. EMC, 電磁環境研究会 2010 (29) 1 -4 2010年11月01日 [査読無し][通常論文]
  • 吉田 和哉, 荘司 泰弘, 坂本 祐二, 田口 真, 高橋 幸弘 電子情報通信学会総合大会講演論文集 2010 (1) "SS -78"-"SS-79" 2010年03月02日 [査読無し][通常論文]
  • 田口 真, 荘司 泰弘, 坂本 祐二, 吉田 和哉, 高橋 幸弘, 寺口 朋子, 大西 智也, Steve Battazzo, 佐藤 隆雄, 星野 直哉, 宇野 健, 吉村 淳 宇宙航空研究開発機構研究開発報告 9 53 -72 2010年03月 [査読無し][通常論文]
     
    惑星大気・プラズマ中で起こる時間変動現象を研究するためには長期連続観測が重要である.極域成層圏の特殊性を利用して惑星を連続観測することを目的とした気球搭載望遠鏡を開発している.口径300mm のシュミットカセグレン望遠鏡が気球ゴンドラに搭載される.ゴンドラはコントロールモーメントジャイロ,デカップリング機構,各種姿勢センサーを使って姿勢制御され,極域成層圏に 1 週間以上滞留可能な性能を持つ.ゴンドラ姿勢制御,望遠鏡経緯台による天体捕捉,2 軸ティップティルトミラーによる追尾誤差補正によって,目標天体を0.1"rms の精度で捉える.金星をターゲットとして,最初の気球実験が 2009 年6 月3 日に北海道大樹町において実施された.4:10 に放球され,その後2 時間,システムは正常に動作した.高度約 14km でのレベルフライト時に太陽捕捉の実験を行った.ゴンドラ姿勢制御を開始するとゴンドラの方位角は振動しつつ収束し,数分間,方位角誤差は1°rms の範囲内に収まった.残念ながら搭載コンピュータの不具合により,金星捕捉は叶わなかった.しかし,サンセンサーのビデオ信号から,姿勢制御していない状態でのゴンドラの方位角角速度は20°/min 以下であることがわかった.地上試験も含めた今回の気球実験結果から,気球望遠鏡システムの姿勢制御,天体捕捉・追尾の原理は有効であることが確証された.今後の実験へ向けて,より信頼性が高い搭載コンピュータに改善していく.
  • 坂本 祐二, 吉田 和哉, 高橋 幸弘 スペース・エンジニアリング・コンファレンス講演論文集 : Space Engineering Conference 2009 (18) 35 -39 2010年01月28日 
    The microsatellite RISING(SPRITE-SAT) developed by Tohoku University was launched in January 2009. The former part of this paper shows the outline of mission and system design. The operation result of initial phase and the reason of serious trouble are introduced. On July 2009, our team initiated the development of second microsatellite named RISING-2. This satellite has a high precision telescope and reaction wheels. The outline of this new project is shown in the latter part.
  • 牛尾 知雄, 森本 健志, 佐藤 光輝, 鈴木 睦, 山崎 敦, 芳原 容英, 菊地 雅行, 高橋 幸弘, Inan Umran, 石田 良平, 坂本 祐二, 吉田 和哉, 阿部 琢美, 河崎 善一郎 大会講演予講集 97 52 -52 2010年
  • 福原哲哉, 高橋幸弘, 佐藤光輝, 渡部重十, 渡辺誠, 佐藤創我 大気圏シンポジウム・講演集(Web) 24th 2010年
  • 高橋 幸弘, 星野 直哉 遊・星・人 : 日本惑星科学会誌 18 (4) 238 -241 2009年12月25日 [査読無し][通常論文]
     
    金星における世界初の雷放電観測専用機能と微弱大気光の検出能力を兼ね備えた雷・大気光カメラLACは,ハードウェアの製作・各種試験が完了し,実地観測に備えたパラメータ設定と詳細シーケンスの検討に入った.LACの科学的背景と目標,設計方針,これまで行った試験などについて紹介する.
  • 佐藤 光輝, 牛尾 知雄, 森本 健志, 高橋 幸弘, INAN Umran, 芳原 容英, 菊池 雅行, 鈴木 睦, 山崎 敦, 阿部 琢美, 吉田 和哉, 坂本 祐二, 奥山 圭一, 石田 良平, 河崎 善一郎 大気電気学会誌 = / Society of Atmospheric Electricity of Japan 3 (2) 60 -61 2009年10月30日 [査読無し][通常論文]
  • 佐々木 晶, 藤本 正樹, 木村 淳, 高島 健, 矢野 創, 笠羽 康正, 高橋 幸弘, 川口 淳一郎, 川勝 康弘, 津田 雄一, 船瀬 龍, 森 治, 森本 睦子, 木星探査WG 日本惑星科学会秋期講演会予稿集 2009 59 -59 2009年09月28日
  • 福原 哲哉, 高橋 幸弘, 佐藤 光輝, 渡部 重十, 佐藤 創我, 渡邉 誠 日本惑星科学会秋期講演会予稿集 2009 2009年09月28日 [査読無し][通常論文]
  • 杉田 精司, 宮本 英昭, 橘 省吾, 岡田 達明, 出村 裕英, 大森 聡一, 並木 則行, 高橋 幸弘, 三浦 弥生, 長尾 敬介, 三河内 岳, 佐藤 毅彦 遊・星・人 : 日本惑星科学会誌 18 (2) 79 -83 2009年06月25日 
    我々はこれまでの火星複合探査ワーキンググループの中で,MELOSの着陸機によってどのような火星表層探査を行うべきか,またどのような測定によって実現されるのか議論を行ってきた.本稿では,その議論で見えてきた火星着陸探査による表面探査の科学目標と搭載機器候補について解説する.
  • 今村 剛, 笠井 康子, 佐川 英夫, 黒田 剛史, 佐藤 毅彦, 上野 宗孝, 鈴木 睦, 高橋 幸弘, 高橋 芳幸, はしもと じょーじ, 倉本 圭 遊・星・人 : 日本惑星科学会誌 18 (2) 76 -78 2009年06月25日 [査読無し][通常論文]
     
    火星表層の水循環や気象学の理解を目的とする火星周回衛星の検討を進めている.可視〜赤外域での高解像度の分光撮像による水蒸気マッピングと大気力学場モニター,そしてサブミリ波サウンダーによる水蒸気やその他微量ガスの3次元分布の観測が,二つの柱である.着陸機による局地気象の直接観測や大気電気観測との連携についても検討中である.
  • 高橋 幸弘 日本物理學會誌 64 (5) 365 -372 2009年05月05日 
    ふつう雷といえば,雷雲と地上,あるいは雷雲内での放電を思い浮かべるであろう.しかし,1989年に偶然発見された放電現象は,雷雲上空から電離圏の間で発生していた.スプライトと命名されたこの現象に代表される放電発光は,当初米国を中心として研究が進められてきたが,発見から15年以上が過ぎて,その研究は世界的な広がりを見せ国際協力が盛んである.人工衛星を含む様々な手法を総動員した観測によってメカニズムの解明が進む一方,従来の標準的モデルの修正や関連する新現象の発見も相次いでおり,話題に事欠かない.1995年から研究に携わってきた筆者が,最新の研究の展開と現場の熱気を,エピソードとともに紹介する.
  • Nakagawa Hiromu, Fukunishi Hiroshi, Watanabe Shigeto, TAKAHASHI Yukihiro, TAGUCHI Makoto, LALLEMENT Rosine Earth, planets and space 61 (3) 373 -382 2009年03月01日
  • 鶴島 大樹, 境田 清隆, 高橋 幸弘, 本間 規泰 大会講演予講集 96 341 -341 2009年
  • Adachi, T, S. A. Cummer, J. Li, Y. Takahashi, R.-R. Hsu, H.-T. Su, A. B. Chen, S. B. Mende, H. U. Frey Geophys. Res. Lett. 36, L18808 (18) L18808 2009年 [査読無し][通常論文]
  • Adachi Toru, Takahashi Yukihiro, Ohya Hiroyo, Tsuchiya Fuminori, Yamashita Kozo, Yamamoto Mamoru, Hashiguchi Hiroyuki Kyoto Working Papers on Area Studies: G-COE Series 11 1 -20 2008年12月 
    In this report, a newly-developed lightning observation network system is outlined. The network consists of an optical observation site (Padang in Indonesia) and three electromagnetic observation sites (Pontianak in Indonesia, Tainan in Taiwan, and Saraburi in Thailand). At Padang site, a small low-light CCD camera was installed to observe the optical emission of lightning flash. On the other hand, a monopole, a dipole, and a set of orthogonal loop antennas were installed at each site to detect electromagnetic waves in the frequency range of 0.1-40 kHz. The obtained data are analyzed to monitor lightning activity in Southeast Asia in various spatiotemporal scales and clarify severe weather phenomena which cause significant damages on the human activity.
  • M. Sato, Y. Takahashi, A. Yoshida, T. Adachi Journal of Physics D: Applied Physics 41 2008年12月01日 [査読無し][通常論文]
     
    In order to study the temporal and regional variation of lightning occurrences and their relation to sprite activity and climate variability, we have analysed the 1-100 Hz ELF magnetic field waveform data obtained at the Syowa station in Antarctica, Onagawa in Japan and Esrange in Sweden for a one year period from September 2003 to August 2004. We have selected totally 1.7 × 105 events of transient Schumann resonances from the ELF magnetic field data whose amplitude exceeds 40 pT at all stations. Then, the lightning locations are estimated by a triangulation method with an estimation error of 0.5 Mm. It is found that in the summer season (from June to August) the lightning occurrence rates are higher in the northern hemisphere than in the southern hemisphere with large enhancements in North America, South-East Asia and the northern part of Africa. On the other hand, in the winter season (from December to February) these rates are higher in the southern hemisphere with large enhancements in South America, Australia and the southern part of Africa. These features are consistent with the results of global lightning measurements from space conducted by the Optical Transient Detector and the Tropical Rainfall Measuring Mission satellite. Then, we have also calculated the charge moment value (Q · dl) of lightning discharges using ELF magnetic field waveform data and have estimated the distribution function of charge moments for positive cloud-to-ground (+CG) discharges and for negative cloud-to-ground (-CG) discharges. It is found that the shape of the distribution function for both +CG and -CG discharges is almost the same for all seasons and that the distribution function of -CG discharges has a steeper slope at high Q · dl than that of +CG discharges. © 2008 IOP Publishing Ltd.
  • 佐々木 晶, 藤本 正樹, 木村 淳, 高島 健, 笠羽 康正, 山路 敦, 長沼 毅, 桜庭 中, 高橋 幸弘, 栗田 敬, 生駒 大洋 日本惑星科学会秋期講演会予稿集 2008 148 -148 2008年11月01日
  • 氏家 恵理子, 吉田 和哉, 高橋 幸弘, 坂本 祐二, 坂野井 健, 升本 喜就, 笠羽 康正, 近藤 哲志 電子情報通信学会技術研究報告. SANE, 宇宙・航行エレクトロニクス 108 (267) 1 -6 2008年10月24日 
    東北大学は50kgクラスの小型人工衛星であるスプライト観測衛星(SPRITE-SAT)を開発中であり,2009年初頭,H-IIAのピギーバック衛星として打ち上げ予定である。本衛星は雷放電と,それに付随して発生するスプライト発光現象,およびTerrestrial Gamma-ray Flashes (TGFs)を同時観測することで,現象の発生メカニズムを解明することがミッションである。新たに開発した伸展マストを搭載し,ほとんどのミッション機器を搭載するボトムパネルが常時地球方向を指向する重力傾斜安定方式を採用している。本文書ではミッションおよび衛星システムの概要を述べる。
  • 上田 剛, 榎戸 輝揚, 中澤 知洋, 三谷 烈史, 高島 健, 坂野井 健, 氏家 恵理子, 笠羽 康正, 吉田 和哉, 高橋 幸弘, 森 國城, 牧島 一夫 日本物理学会講演概要集 63 (2) 94 -94 2008年08月25日
  • 今村 剛, 佐藤 毅彦, 上野 宗孝, 寺田 直樹, 高橋 幸弘 遊・星・人 : 日本惑星科学会誌 17 (1) 54 -57 2008年03月25日 
    惑星大気探査の将来構想を紹介する.今後10年は地球型惑星である金星と火星を対象として研究を深めつつ経験を蓄積し,将来は木星をも対象とする.
  • 高橋 幸弘, Miyahara Hiroko, Sato Mitsuteru 大会講演予講集 94 479 -479 2008年
  • 足立透, 大矢浩代, 土屋史紀, 高橋幸弘 大気圏シンポジウム 22nd(CD-ROM) 2008年
  • 大矢浩代, 足立透, 土屋史紀, 高橋幸弘 大気圏シンポジウム 22nd(CD-ROM) 2008年
  • 地上光学・電磁波観測器とMUレーダーを用いた雷活動と電離圏擾乱現象の同時観測
    足立透, 山本衛, 大塚雄一, 高橋幸弘, 佐藤光輝 京都大学生存圏研究所MU共同利用成果報告書 2008年 [査読無し][通常論文]
  • 吉田 暁洋, 高橋 幸弘, 佐藤 光輝, 足立 透, 近藤 哲志, Hsu Rue-Ron, Su Han-Tzong, Chen Alfred Bing-Chih, Frey H. U., Mende S. B., Lee Lou-Chuang 大会講演予講集 92 221 -221 2007年
  • 坂野井健, 高橋幸弘, 上野宗孝, 笠羽康正, 吉田和哉, 山崎敦, 今村剛, 阿部琢美, 田口真, 澤井秀次郎, 高橋幸弘 地球電磁気・地球惑星圏学会総会及び講演会予稿集(CD-ROM) 122nd 2007年
  • 吉田 純, 高橋 幸弘, 上田 真也, 堤 雅基, 牛尾 知雄 大会講演予講集 90 70 -70 2006年
  • 吉田 純, 高橋 幸弘, 田村 大輔 大会講演予講集 90 71 -71 2006年
  • 足立 透, 福西 浩, 高橋 幸弘, 山本 桂, Hsu R. R., Su H. T., Chen A. B., Mende S. B., Frey H. U., Lee L. C. 大会講演予講集 90 296 -296 2006年
  • FORMOSAT-2/ISUALで観測されたスプライトの形態と雷放電の電気的特徴
    足立透, 福西浩, 高橋幸弘, 平木康隆, 山本桂, R.-R. Hsu, H.-T. Su, A. B. Chen, S. B. Mende, H, U. Frey, C. Lee 第20回大気圏シンポジウム原稿集 2006年 [査読無し][通常論文]
  • 観測システム紹介3: 衛星による超高層発光現象の観測
    足立透, 福西浩, 高橋幸弘, R.-R. Hsu, H.-T. Su, A. B. Chen, S. B. Mende, H, U. Frey, C. Lee MTI ハンドブック(2006年度) 2006年 [査読無し][通常論文]
  • Adachi, T, H. Fukunishi, Y. Takahashi, Y. Hiraki, R.-R Hsu, H.-T. Su, A. B. Chen, S. B. Mende, H. U. Frey, L. C. Lee Geophys. Res. Lett. 33 (17) L17803-L17803-5 2006年 [査読無し][通常論文]
  • 吉田 純, 高橋 幸弘, 福西 浩, 堤 雅基, 牛尾 知雄 宇宙航空研究開発機構研究開発報告 4 1 -54 2005年03月 
    現在,金星大気超回転の解明を主目的とした金星気象衛星(VCO:Venus Climate Orbiter)を打ち上げるPlanet-Cミッションが宇宙航空研究開発機構/宇宙科学研究本部を中心として進行中である.我々はVCOに搭載する雷・大気光カメラ(LAC:Lightning and Airglow Camera)の開発を行っている.LACは金星夜面における雷放電発光・大気光を2次元で高速イメージングする観測器である.雷放電観測では,まずこの現象の存在の決定的な証拠を得て,長年の論争を収束させることを目標とする.さらに,その電荷生成・分離メカニズムの解明や硫酸雲物理学の理解,惑星メソスケール気象学の発展,金星大気中における熱的・化学的寄与の見積もりなど,様々な分野に貢献することが期待される.大気光観測では,発光強度の緯度・経度分布から金星超高層大気の運動を継続的にモニターし,さらに波状構造をイメージングすることで,金星下部熱圏と下層大気の力学的結合過程の解明,金星熱圏大気大循環メカニズムの理解の進展が期待される.さらに近年,地上望遠鏡で発見された558nm[OI]の連続観測も実施し,その発光強度分布や時間変動を捉え,オーロラとも解釈できるこの発光現象の解明を目指す.LACのセンサーとしては,高感度を有し,かつ高速サンプリングが可能なものが要求される.また本観測器は,雷放電発光観測用に波長777nm[OI]の干渉フィルタを採用し,50kHzプレトリガーサンプリングでデータを取得する.一方,大気光観測時には波長551nm[O_2Herzberg II],558nm[OI]で連続サンプリングを行い,積分時間10secで1枚の画像を作成する.VCOは金星低緯度を周回する長楕円軌道をとるが,LACはこのうち近金点(高度300km)付近から金星より3Rv離れた地点までの高度範囲で運用する.その際,雷放電発光観測に関しては距離3Rvの地点から地球の平均的発光強度のものを,1000kmの高度からはその1/100レベルのものまでを検出することを目標とする.一方,大気光に関しては発光強度100Rのものを,SN比=10を確保して検出することを目標とする.上記の性能を達成するため,我々は第一に,LACのセンサーとして光電子増倍管(PMT:Photo Multiplier Tube)とアバランシェ・フォトダイオード(APD:Avalanche Photo Diode)の2つを検討した.いずれも8×8の2次元配列素子である.絶対感度校正実験から得られた出力電流値と,暗電流測定試験から得られた暗電流値から,本観測器で100Raylieghの光源を観測した場合の暗電流統計揺らぎによるSN比が10以上であることを確認した.しかしながらAPDについてはバックグラウンドレベルの温度安定性が低く,光量の小さい大気光観測は適さないことがわかった.またPMTに関しては波長777nmにおける量子効率がAPDに比べて小さく,雷放電発光観測は困難であることが判明した.第二に,金星夜面観測の際に視野内に混入することが予想される迷光(太陽直達光,金星昼面光)の量を見積もり,迷光減衰要求量11桁を達成する高い遮光技術を有する光学系の設計・開発を行った.衛星側面に設置し片側を宇宙空間に暴露させ,対物側に4枚の遮光板(vane)と1段バッフルを取り付けた光学系を設計した.本光学系を採用する際,衛星表面を覆う金色のサーマルブランケットや設置面上にある突起物を介して,迷光が観測視野内に混入することが懸念されるため,我々は暗室内で精密な模型実験を行った.その結果,衛星突起物がベーン陰影内にある場合,その迷光量はカメラ部の1段バッフルから検出器間の遮光対策で十分減衰可能な量であることを定量的に示した.第三に,高速サンプリング時におけるデータ取得方法の考案・検討を実施した.忘却係数という概念を用いてトリガーサンプリング方法を考案し,地上フォトメータで捉えられた地球雷放電発光の波形で試験した結果,ノイズと分離して信号を検出することに成功した.本研究成果により,LAC開発に必要不可欠な基礎技術の活用に見通しを立てることができた.
  • 坂野井 健, 高橋 幸弘, 吉田 和哉 宇宙科学シンポジウム 5 392 -395 2005年01月06日
  • 高橋 幸弘, 坂野井 健, 吉田 和哉 宇宙科学シンポジウム 5 368 -375 2005年01月06日
  • 小笠原 麻喜, 新野 宏, 高橋 幸弘 大会講演予講集 87 193 -193 2005年
  • ROCSAT-2/ISUAL Array Photometer によるスプライト観測:電場の推定
    足立透, 福西浩, 高橋幸弘, 平木康隆, R.-R. Hsu, H.-T. Su, A. B. Chen, S. B. Mende, H, U. Frey, C. Lee 第19回大気圏シンポジウム原稿集 2005年 [査読無し][通常論文]
  • Adachi, T, H. Fukunishi, Y. Takahashi, M. Sato, A. Ohkubo, K. Yamamoto J. Geophys.Res 110 (D11) D11203, doi: 10.1029/2004JD005012 2005年 [査読無し][通常論文]
  • 永野 元彦, 宮崎 芳郎, 高橋 幸弘, 村上 敏夫, 米徳 大輔, 木舟 正, 石川 正, 金子 敏明, 栗原 良将, 清水 韶光, 藤本 順平, 竹田 成宏, 林田 直明, 間瀬 圭一, 井上 直也, 和田 吉満, 上野 嘉之, 上原 嘉宏, 戎崎 俊一, 大谷 知行, 大森 整, 川井 和彦, 川崎 賀也, 榊 直人, 佐藤 光輝, 清水 裕彦, 鈴木 亨, 滝澤 慶之, Bertaina M E, 森田 晋也, 林 偉民, 北本 俊二, 近 匡, 本田 建, 梶野 敏貴, 水本 好彦, 内堀 幸夫, 吉田 滋, 門多 顕司, 柴田 徹, 吉田 篤正, 高橋 義幸, 梶野 文義, 佐藤 文隆, 坂田 通徳, 山本 嘉昭, 田島 俊樹, 千川 道幸, 政池 明, 川上 三郎, 吉井 尚, 手嶋 政廣 日本物理学会講演概要集 59 (2) 81 -81 2004年08月25日
  • 高橋 幸弘, 坂野井 健, 吉田 和哉 宇宙科学シンポジウム 4 445 -448 2004年01月08日
  • 高橋 幸弘, 足立 透, 近田 昌吾, 高橋 久夫, 今村 剛 大会講演予講集 86 42 -42 2004年
  • 福西 浩, 高橋 幸弘, 足立 透, Hsu R. -R., Su H. -T., Chen A. -B., Mende S. B., Frey H. U., Lee L. -C. 大会講演予講集 86 423 -423 2004年
  • 足立 透, 福西 浩, 高橋 幸弘, Hsu R. R., Su H. T., Chen A. B., Mende S. B., Frey H. U., Lee L. C. 大会講演予講集 86 422 -422 2004年
  • 足立 透, 福西 浩, 高橋 幸弘, 佐藤 光輝, 大久保 敦史 大会講演予講集 85 266 -266 2004年
  • 日本に発生する冬季スプライトと雷雲に関する研究
    足立透, 福西浩, 高橋幸弘, 佐藤光輝 第18回大気圏シンポジウム原稿集 2004年 [査読無し][通常論文]
  • 高橋 幸弘, 今村 剛 遊・星・人 : 日本惑星科学会誌 12 (4) 230 -230 2003年12月25日
  • 吉田 純, 高橋 幸弘 遊・星・人 : 日本惑星科学会誌 12 (4) 261 -267 2003年12月25日
  • 高橋 幸弘, 佐藤 光輝, 平木 康隆, 東北大学スプライト研究チーム 日本物理学会講演概要集 58 (2) 134 -134 2003年08月15日
  • 高橋 幸弘, 坂野井 健, 吉田 和哉 宇宙科学シンポジウム 3 453 -456 2003年01月09日
  • 福西 浩, 荒川 真木子, 高橋 幸弘 宇宙科学シンポジウム 3 551 -554 2003年01月09日
  • 足立 透, 高橋 幸弘, 大久保 敦史 宇宙科学シンポジウム 3 415 -418 2003年01月09日
  • 鈴木 睦, 奥村 真一郎, 吉田 重臣, 小川 利紘, 北 和之, 今村 剛, 中村 正人, 高橋 幸弘, 牛尾 知雄 大会講演予講集 84 387 -387 2003年
  • 足立 透, 福西 浩, 高橋 幸弘, 佐藤 光輝, 大久保 敦史 大会講演予講集 84 402 -402 2003年
  • 鈴木 睦, 奥村 真一郎, 吉田 重臣, 小川 利紘, 北 和之, 今村 剛, 中村 正人, 高橋 幸弘, 牛尾 知雄 大会講演予講集 84 83 -83 2003年
  • 高橋 幸弘, 牛尾 知雄, 堤 雅樹, 鈴木 睦, 奥村 真一郎, 吉田 重臣 大会講演予講集 84 86 -86 2003年
  • 高橋 幸弘, 足立 透, 福西 浩 大会講演予講集 83 418 -418 2003年
  • 足立 透, 福西 浩, 高橋 幸弘 大会講演予講集 83 417 -417 2003年
  • 佐藤 光輝, 福西 浩, 高橋 幸弘 大会講演予講集 83 419 -419 2003年
  • 山本真行, 矢野創, 阿部新助, 吉田和哉, 高橋幸弘, 海老塚昇, 清水裕彦 宇宙科学シンポジウム 平成14年度 第3回 2003年
  • Chern, J. L, R. R. Hsu, H. T. Su, S. B. Mende, H. Fukunishi, Y. Takahashi, L. C. Lee J. Atmos. Solar. Terr. Phys 65 (5) 647 -659 2003年 [査読無し][通常論文]
  • 中川 広務, 福西 浩, 高橋 幸弘 宇宙科学シンポジウム 2 491 -494 2001年11月19日
  • 福西 浩, 高橋 幸弘, Mende S. B. 宇宙科学シンポジウム 2 323 -330 2001年11月19日
  • 高橋 幸弘 大会講演予講集 79 171 -171 2001年05月08日
  • 福西 浩, 船橋 豪, 高橋 幸弘 宇宙科学シンポジウム 1 253 -256 2001年01月11日
  • 福西 浩, 高橋 幸弘, Mende S.B. 宇宙科学シンポジウム 1 165 -172 2001年01月11日
  • 今村 剛, 高橋 幸弘, はしもと じょーじ 日本惑星科学会秋期講演会予稿集 2000 83 -83 2000年10月31日
  • 高橋 幸弘, 倉本 圭, 今村 剛 日本惑星科学会秋期講演会予稿集 2000 85 -85 2000年10月31日 [査読無し][通常論文]
  • 高橋 幸弘, 倉本 圭 遊・星・人 : 日本惑星科学会誌 9 (1) 33 -46 2000年03月25日 [査読無し][通常論文]
  • 竹内 覚, 今村 剛, 小山 孝一郎, 笠羽 康正, 高橋 幸弘, 松田 佳久, 金星探査計画ワーキンググループ 大会講演予講集 76 401 -401 1999年11月24日
  • 土岐 剛史, 高橋 幸弘, 山田 嘉典, 福西 浩, 中村 卓司, TAYLOR Michal J. 宇宙科学研究所報告. 特集 38 83 -91 1998年03月 
    1996年8月に実施されたSEEKキャンペーンにおいて, 地上からの高感度イメージャーによる大気波動の観測が鹿児島県内の内之浦, 山川, 大隅と信楽の計4ヵ所で実施された。キャンペーン期間中の鹿児島地方は天候に優れない日が多かったが, 8月9日から22日の間に, 内之浦, 山川, 大隅でそれぞれ, 4夜, 7夜, 1夜, 大気光イメージデータが取得された。信楽での観測は8夜であった。今回の地上からの大気光観測の主な目的は, レーダーで観測される電離圏における準周期的イレギュラリティーと大気光に見られる中性大気中の重力波の特性を, ロケットによる観測とあわせてそのメカニズムを検討解明することにある。各観測データと比較する上で, 大気光の発光高度を正確に決定することは極めて重要な課題である。我々は鹿児島の3ヵ所の観測から, 三画法を用いてOH大気光の発光高度の推定を計画した。残念ながらロケット打ち上げ時は天候に恵まれず同時観測データは得られなかったが, キャンペーン期間中内之浦と山川に設置された2台の大気光全天イメージャによる同時観測に成功した。8月19日の晩, 2台のイメージャで同時に顕著なOH大気光の波状構造を観測した。これら2地点で同時に取得された画像に, 大気波動構造の発光高度決定としては初めて, FFT及び精密な三角法を用いて解析を行った。その結果, 波状構造の発光高度は89±3kmと求められた。これはロケット観測などによる従来の結果とほぼ一致する。MFレーダーによって, この高度の数km上空で回時に強い南向きの風速シアーが観測されており, 重力波の発生原因の有力な候補と考えられる。
  • 津田 敏隆, 中村 卓司, 三好 勉信, 川原 琢也, 堤 雅基, 村山 泰啓, 高橋 幸弘, 坂野井 健 天気 45 (11) 848 -849 1998年

教育活動情報

主要な担当授業

  • 大学院共通授業科目(一般科目):自然科学・応用科学
    開講年度 : 2021年
    課程区分 : 修士課程
    開講学部 : 大学院共通科目
    キーワード : Remote-sensing, Asia, Micro-satellite, Drone, Optical payload
  • 宇宙理学特別講義1
    開講年度 : 2021年
    課程区分 : 修士課程
    開講学部 : 理学院
    キーワード : Remote-sensing, Asia, Micro-satellite, Drone, Optical payload
  • 惑星システム学特論2
    開講年度 : 2021年
    課程区分 : 修士課程
    開講学部 : 理学院
    キーワード : 地球惑星大気,宇宙空間,惑星探査, 光学計測
  • 理学共通演習Ⅱ
    開講年度 : 2021年
    課程区分 : 学士課程
    開講学部 : 理学部
    キーワード : アクティブラーニング、ファシリテーション、チームワーク、化学結合、遷移状態、触媒、タンパク質酵素、市場に出たゲノム編集食品、受精卵に対するゲノム編集、治療特殊相対性理論、光速度不変の原理、地球環境変動、衛星リモートセンシング
  • 地球惑星科学Ⅱ
    開講年度 : 2021年
    課程区分 : 学士課程
    開講学部 : 全学教育
    キーワード : 宇宙,惑星,大気と海洋の運動と構造,気候変動,地球環境
  • 環境と人間
    開講年度 : 2021年
    課程区分 : 学士課程
    開講学部 : 全学教育
    キーワード : 太陽系,惑星,惑星大気,オーロラ,星間物質, 天文学、宇宙の進化, 人工衛星/探査機, 探査ミッション,地上望遠鏡, 室内実験
  • 現代地球惑星科学概論1
    開講年度 : 2021年
    課程区分 : 学士課程
    開講学部 : 理学部
    キーワード : 地球規模課題、グループワーク
  • 地球惑星電磁気学
    開講年度 : 2021年
    課程区分 : 学士課程
    開講学部 : 理学部
    キーワード : 地磁気,岩石磁気,電気伝導度,電離圏,磁気圏,プラズマ,オーロラ

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