2024/03/06 更新

写真b

クワバラ マサキ
桑原 正輝
KUWABARA Masaki
*大学が定期的に情報更新している項目(その他は、researchmapの登録情報を転載)
所属*
理学部 物理学科
理学研究科 物理学専攻 博士課程後期課程
職名*
助教
学内職務経歴*
  • 2022年4月 - 現在 
    理学部   物理学科   助教
  • 2022年4月 - 2023年1月 
    理学研究科   物理学専攻 博士課程前期課程   助教
  • 2022年4月 - 2023年1月 
    理学研究科   物理学専攻 博士課程後期課程   助教
  • 2021年4月 - 2022年3月 
    理学研究科   物理学専攻 博士課程前期課程   特任准教授
  • 2021年4月 - 2022年3月 
    理学研究科   物理学専攻 博士課程後期課程   特任准教授
 

研究分野

  • 自然科学一般 / 宇宙惑星科学

経歴

  • 2018年4月 - 2021年3月 
    国立研究開発法人宇宙航空研究開発機構   宇宙科学研究所   宇宙航空プロジェクト研究員

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論文

  • Major results from the Hisaki mission and future perspectives

    Fuminori Tsuchiya, Yasumasa Kasaba, Ichiro Yoshikawa, Go Murakami, Atsushi Yamazaki, Kazuo Yoshioka, Tomoki Kimura, Chihiro Tao, Ryoichi Koga, Hajime Kita, Kei Masunaga, Masato Kagitani, Shotaro Sakai, Masaki Kuwabara

        2023年2月22日

  • 振子式衝撃試験装置の性能評価およびMCPの衝撃耐性評価 査読有り

    福場 惇哉, 吉岡 和夫, 桑原 正輝, 吉川 一朗

    宇宙航空研究開発機構研究開発報告JAXA-RR-19-005   1 - 28   2020年2月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)  

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  • Solar System Exploration Sciences by EQUULEUS on SLS EM-1 and Science Instruments Development Status

    Satoshi Ikari, Masahiro Fujiwara, Hirotaka Kondo, Shuhei Matsushita, Ichiro Yoshikawa, Kazuo Yoshioka, Reina Hikida, Yosuke Kawabata, Shintaro Nakajima, Ryu Funase, Masaki Kuwabara, Hajime Yano, Kota Miyoshi, Tatsuaki Hashimoto, Shinsuke Abe, Ryota Fuse, Yosuke Masuda, Shosaku Harima, Masahisa Yanagisawa, Kenji Yamamoto, Ryuji Shimada, Takayuki Hirai, Haruki Nakano, Kosuke Kando, Kazuyoshi Arai, Masayuki Fujii

    33rd Annual AIAA/USU Conference on Small SatellitesSSC19 ( WKV-04 ) 1 - 9   2019年8月3日

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    記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:AIAA  

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  • 超小型探査機搭載の極端紫外光観測装置PHOENIXの開発 査読有り

    桑原 正輝, 吉岡 和夫, 疋田 伶奈, 村上 豪, 荒尾 昇吾, 吉川 一朗

    宇宙航空研究開発機構研究開発報告JAXA-RR-18-010   1 - 16   2019年3月

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    担当区分:筆頭著者, 責任著者   記述言語:日本語   掲載種別:研究論文(学術雑誌)  

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  • 超小型探査機搭載に向けた汚染防止用蓋開閉システムの開発 査読有り

    吉岡 和夫, 桑原 正輝, 疋田 伶奈, 荒尾 昇吾, 吉川 一朗

    宇宙航空研究開発機構研究開発報告JAXA-RR-18-007   1 - 9   2019年2月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)  

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  • Mission to Earth-Moon Lagrange Point by a 6U CubeSat: EQUULEUS 査読有り

    Ryu Funase, Satoshi Ikari, Kota Miyoshi, Yosuke Kawabata, Shintaro Nakajima, Shunihiro Nomura, Nobuhiro Funabiki, Akihiro Ishikawa, Kota Kakihara, Shuhei Matsushita, Ryohei Takahashi, Kanta Yanagida, Daiko Mori, Yusuke Murata, Toshihiro Shibukawa, Ryo Suzumoto, Masahiro Fujiwara, Kento Tomita, Hiroki Aohama, Keidai Iiyama, Sho Ishiwata, Hirotaka Kondo, Wataru Mukuriya, Hiroto Seki, Hiroyuki Koizumi, Jun Asakawa, Keita Nishii, Akihiro Hattori, Yuji Saito, Kosei Kikuchi, Yuta Kobayashi, Atsushi Tomiki, Wataru Torii, Taichi Ito, Stefano Campagnola, Naoya Ozaki, Nicola Baresi, Ichiro Yoshikawa, Kazuo Yoshioka, Masaki Kuwabara, Reina Hikida, Shogo Arao, Shinsuke Abe, Masahisa Yanagisawa, Ryota Fuse, Yosuke Masuda, Hajime Yano, Takayuki Hirai, Kazuyoshi Arai, Ritsuko Jitsukawa, Eigo Ishioka, Haruki Nakano, Toshinori Ikenaga, Tatsuaki Hashimoto

    IEEE Aerospace & Electronics Systems Magazine   2019年

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    記述言語:英語   掲載種別:研究論文(学術雑誌)  

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  • Extreme ultraviolet spectra of Venusian airglow observed by EXCEED 査読有り

    Yusuke Nara, Ichiro Yoshikawa, Kazuo Yoshioka, Go Murakami, Tomoki Kimura, Atsushi Yamazaki, Fuminori Tsuchiya, Masaki Kuwabara, Naomoto Iwagami

    Icarus307   207 - 215   2018年6月1日

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    記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:Academic Press Inc.  

    Extreme ultraviolet (EUV) spectra of Venus in the wavelength range 520−1480 Å with 3−4 Å resolutions were obtained in March 2014 by an EUV imaging spectrometer EXCEED (Extreme Ultraviolet Spectroscope for Exospheric Dynamics) on the HISAKI spacecraft. Due to its high sensitivity and long exposure time, many new emission lines and bands were identified. Already known emissions such as the O II 834 Å O I 989 Å HILy−β1026 Å and the C I 1277 Å lines (Broadfoot et al., 1974
    Bertaux et al., 1980
    Feldman et al., 2000) are also detected in the EXCEED spectrum. In addition, N2 band systems such as the Lyman-Birge-Hopfield (a1Πg−X1Σg +) (2, 0), (2, 1), (3, 1), (3, 2) and (5, 3) bands, the Birge-Hopfield (b1Πu−X1Σg +) (1, 3) band, and the Carroll-Yoshino (c4 ′ 1Σu +−X1Σg +) (0, 0) and (0, 1) bands together are identified for the first time in the Venusian airglow. We also identified the CO Hopfield-Birge (B1Σ+−X1Σ+) (1, 0) band in addition to the already known (0, 0) band, and the CO Hopfield-Birge (C1Σ+−X1Σ+) (0, 1), (0, 2) bands in addition to the already known (0, 0) band (Feldman et al., 2000
    Gérard et al., 2011).

    DOI: 10.1016/j.icarus.2017.10.028

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  • Evaluation of hydrogen absorption cells for observations of the planetary coronas 査読有り

    M. Kuwabara, M. Taguchi, K. Yoshioka, T. Ishida, N. De Oliveira, K. Ito, S. Kameda, F. Suzuki, I. Yoshikawa

    Review of Scientific Instruments89 ( 2 ) 023111   2018年2月1日

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    担当区分:筆頭著者, 責任著者   記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:American Institute of Physics Inc.  

    Newly designed Lyman-alpha absorption cells for imaging hydrogen planetary corona were characterized using an ultra high resolution Fourier transform spectrometer installed on the DESIRS (Dichroïsme Et Spectroscopie par Interaction avec le Rayonnement Synchrotron) beamline of Synchrotron SOLEIL in France. The early absorption cell installed in the Japanese Mars orbiter NOZOMI launched in 1998 had not been sufficiently optimized due to its short development time. The new absorption cells are equipped with the ability to change various parameters, such as filament shape, applied power, H2 gas pressure, and geometrical configuration. We found that the optical thickness of the new absorption cell was ∼4 times higher than the earlier one at the center wavelength of Lyman-alpha absorption, by optimizing the condition to promote thermal dissociation of H2 molecules into two H atoms on a hot tungsten filament. The Doppler temperature of planetary coronas could be determined with an accuracy better than 100 K with the performance of the newly developed absorption cell.

    DOI: 10.1063/1.5007812

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  • Ecliptic North-South Symmetry of Hydrogen Geocorona 査読有り

    S. Kameda, S. Ikezawa, M. Sato, M. Kuwabara, N. Osada, G. Murakami, K. Yoshioka, I. Yoshikawa, M. Taguchi, R. Funase, S. Sugita, Y. Miyoshi, M. Fujimoto

    Geopysical Research Letters44   11706 - 11712   2017年11月

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    記述言語:英語   掲載種別:研究論文(学術雑誌)  

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  • ひさき衛星搭載の極端紫外分光撮像装置(EXCEED)の回折格子の性能評価 査読有り

    疋田 伶奈, 吉岡 和夫, 村上 豪, 桑原 正輝, 吉川 一朗

    宇宙航空研究開発機構研究開発報告JAXA-RR-16-012   1 - 10   2017年2月

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    記述言語:日本語   掲載種別:研究論文(学術雑誌)  

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  • Radial variation of sulfur and oxygen ions in the Io plasma torus as deduced from remote observations by Hisaki 査読有り

    K. Yoshioka, F. Tsuchiya, T. Kimura, M. Kagitani, G. Murakami, A. Yamazaki, M. Kuwabara, F. Suzuki, R. Hikida, I. Yoshikawa, F. Bagenal, M. Fujimoto

      122   2999 - 3012   2017年2月

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    記述言語:英語   掲載種別:研究論文(学術雑誌)  

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  • ヨウ化セシウムを蒸着したマイクロチャンネルプレートの感度の安定性に関する研究 査読有り

    桑原 正輝, 吉岡 和夫, 村上 豪, 鈴木 文晴, 疋田 伶奈, 吉川 一朗

    宇宙航空研究開発機構研究開発報告JAXA-RR-16-011   1 - 10   2017年2月

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    担当区分:筆頭著者, 責任著者   記述言語:日本語   掲載種別:研究論文(学術雑誌)  

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  • IMAGING OBSERVATIONS OF THE HYDROGEN COMA OF COMET 67P/CHURYUMOV-GERASIMENKO IN 2015 SEPTEMBER BY THE PROCYON/LAICA 査読有り

    Yoshiharu Shinnaka, Nicolas Fougere, Hideyo Kawakita, Shingo Kameda, Michael R. Combi, Shota Ikezawa, Ayana Seki, Masaki Kuwabara, Masaki Sato, Makoto Taguchi, Ichiro Yoshikawa

    ASTRONOMICAL JOURNAL153 ( 2 )   2017年2月

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    記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:IOP PUBLISHING LTD  

    The water production rate of a comet is one of the. fundamental parameters necessary. to understand cometary activity when a comet approaches the Sun within 2.5 au, because water is the most abundant icy material in the cometary nucleus. Wide-field imaging observations of the hydrogen Ly alpha emission in comet 67P/Churyumov-Gerasimenko were performed by the Lyman Alpha Imaging Camera (LAICA) on. board the 50 kg class micro spacecraft, the Proximate Object Close Flyby with Optical Navigation (PROCYON), on UT 2015 September 7.40, 12.37, and 13.17 (corresponding to 25.31, 30.28, and 31.08 days after the perihelion passage of the comet, respectively). We derive the water production rates, QH(2)O, of the comet from Lya images of the comet by using a 2D axi-symmetric Direct Simulation Monte-Carlo model of the atomic hydrogen coma; (1.46. +/- 0.47) x 10(28), (1.24. +/- 0.40) x10(28), and (1.30. +/- 0.42) x 10(28) molecules s(-1) on 7.40, 12.37, and 13.17 September, respectively. These values are comparable to the values from in situ measurements by the Rosetta instruments in the 2015 apparition and the ground-based and space observations during the past apparitions. The comet did not show significant secular change in average water production rates just after the perihelion passage for the apparitions from 1982 to 2015. We emphasize that the measurements of absolute QH(2)O based on the wide field of view (e. g., by the LAICA/PROCYON) are so important to judge the soundness of the coma models used to infer QH(2)O based on in situ measurements by spacecraft, like the Rosetta.

    DOI: 10.3847/1538-3881/153/2/76

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  • The geocoronal responses to the geomagnetic disturbances 査読有り

    M. Kuwabara, K. Yoshioka, G. Murakami, F. Tsuchiya, T. Kimura, A. Yamazaki, I. Yoshikawa

    JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS122 ( 1 ) 1269 - 1276   2017年

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    記述言語:英語   掲載種別:研究論文(学術雑誌)   出版者・発行元:AMER GEOPHYSICAL UNION  

    Atomic hydrogen atoms in the terrestrial exosphere resonantly scatter solar Lyman alpha (121.6 nm) radiation, observed as the hydrogen geocorona. Measurements of scattered solar photons allow us to probe time-varying distributions of exospheric hydrogen atoms. The Hisaki satellite with the extreme ultraviolet spectrometer (EXtreme ultraviolet spectrosCope for ExosphEric Dynamics: EXCEED) was launched in September 2013. EXCEED acquires spectral images (52-148 nm) of the atmospheres/magnetospheres of planets from Earth orbit. Due to its low orbital altitude (similar to 1000 km), the images taken by the instrument also contain the geocoronal emissions. In this context, EXCEED has provided quasi-continuous remote sensing observations of the geocorona with high temporal resolution (similar to 1 min) since 2013. These observations provide a unique database to determine the long-term behavior of the exospheric density structure. In this paper, we report exospheric structural responses observed by EXCEED to geomagnetic disturbances. Several geomagnetic storms with decreases of Dst index occurred in February 2014 and the Lyman alpha column brightness on the night side of the Earth increased abruptly and temporarily by approximately 10%. Hisaki reveal that the time lag between the peaks of the magnetic activity and the changes in the Lyman alpha column brightness is found to be about 2 to 6h during storms. In order to interpret the observational results, we evaluate quantitatively the factors causing the increase. On the basis of these results, a coupling effect via charge exchange between the exosphere and plasmasphere causes variations of the exospheric density structure.

    DOI: 10.1002/2016JA023247

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  • Ultraviolet detector with CMOS-coupled microchannel plates for future space missions 査読有り

    Go Murakami, Masaki Kuwabara, Kazuo Yoshiok, Reina Hikida, Fumiharu Suzuki, Ichiro Yoshikawa

    SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY9905   2016年

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    記述言語:英語   掲載種別:研究論文(国際会議プロシーディングス)   出版者・発行元:SPIE-INT SOC OPTICAL ENGINEERING  

    The extreme ultraviolet (EUV) telescopes and spectrometers have been used as powerful tools in a variety of space applications, especially in planetary science. Many EUV instruments adopted microchannel plate (MCP) detection systems with resistive anode encoders (RAEs). An RAE is one of the position sensitive anodes suitable for space-based applications because of its low power, mass, and volume coupled with very high reliability. However, this detection system with RAE has limitations of resolution (up to 512 x 512 pixels) and incident count rate (up to similar to 10(4) count/sec). Concerning the future space and planetary missions, a new detector with different position sensitive system is required in order to a higher resolution and dynamic range of incident photons. One of the solutions of this issue is using a CMOS imaging sensor. The CMOS imaging sensor with high resolution and high radiation tolerance has been widely used. Here we developed a new CMOS-coupled MCP detector for future UV space and planetary missions. It consists of MCPs followed by a phosphor screen, fiber optic plate, and a windowless CMOS. We manufactured a test model of this detector and performed vibration, thermal cycle, and performance tests. The test sample of FOP-coupled CMOS image sensor achieved the resolving limit of 32 lp/mm and the PSF of 28 um, corresponds to the spatial resolution of 1024 x 1024 pixels. Our results indicate that this new type of UV detector can be widely used for future space applications.

    DOI: 10.1117/12.2232183

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  • Extreme Ultraviolet Radiation Measurement for Planetary Atmospheres/Magnetospheres from the Earth-Orbiting Spacecraft (Extreme Ultraviolet Spectroscope for Exospheric Dynamics: EXCEED) 査読有り

    Ichiro Yoshikawa, Kazuo Yoshioka, Go Murakami, Atsushi Yamazaki, Fuminori Tsuchiya, Masato Kagitani, Takeshi Sakanoi, Naoki Terada, Tomoki Kimura, Masaki Kuwabara, Kuto Fujiwara, Tomoya Hamaguchi, Hiroyasu Tadokoro

    SPACE SCIENCE REVIEWS184 ( 1-4 ) 237 - 258   2014年11月

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    記述言語:英語   出版者・発行元:SPRINGER  

    The Sprint-A satellite with the EUV spectrometer (Extreme Ultraviolet Spectroscope for Exospheric Dynamics: EXCEED) was launched in September 2013 by the Epsilon rocket. Now it is orbiting around the Earth (954.05 km x 1156.87 km orbit; the period is 104 minutes) and one has started a broad and varied observation program. With an effective area of more than 1 cm(2) and well-calibrated sensitivity in space, the EUV spectrometer will produce spectral images (520-1480 angstrom) of the atmospheres/magnetospheres of several planets (Mercury, Venus, Mars, Jupiter, and Saturn) from the Earth's orbit. At the first day of the observation, EUV emissions from the Io plasma torus (mainly sulfur ions) and aurora (H-2 Lyman and Werner bands) of Jupiter have been identified. Continuous 3-month measurement for Io's plasma torus and aurora is planned to witness the sporadic and sudden brightening events occurring on one or both regions. For Venus, the Fourth Positive (A(1)Pi-X-1 Sigma(+)) system of CO and some yet known emissions of the atmosphere were identified even though the exposure was short (8-min). Long-term exposure from April to June (for approximately 2 months) will visualize the Venusian ionosphere and tail in the EUV spectral range. Saturn and Mars are the next targets.

    DOI: 10.1007/s11214-014-0077-z

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