研究者業績

臼井 寛裕

ウスイ トモヒロ  (Usui Tomohiro)

基本情報

所属
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 教授
学位
博士(学術)(岡山大学)

J-GLOBAL ID
201901004664301386
researchmap会員ID
B000348549

外部リンク

Personal HP <https://sites.google.com/site/tomohirousui/>

Google Scholar <https://scholar.google.com/citations?user=iCTuRbUAAAAJ&hl=en>

ISAS astromaterial/curation research group HP <https://curation.isas.jaxa.jp/en/>


論文

 87
  • Alexander B Verchovsky, Feargus A J Abernethy, Mahesh Anand, Ian A Franchi, Monica M Grady, Richard C Greenwood, Simeon J Barber, Martin Suttle, Motoo Ito, Naotaka Tomioka, Masayuki Uesugi, Akira Yamaguchi, Makoto Kimura, Naoya Imae, Naoki Shirai, Takuji Ohigashi, Ming-Chang Liu, Kentaro Uesugi, Aiko Nakato, Kasumi Yogata, Hayato Yuzawa, Yuzuru Karouji, Satoru Nakazawa, Tatsuaki Okada, Takanao Saiki, Satoshi Tanaka, Fuyuto Terui, Makoto Yoshikawa, Akiko Miyazaki, Masahiro Nishimura, Toru Yada, Masanao Abe, Tomohiro Usui, Sen-Ichiro Watanabe, Yuichi Tsuda
    Nature communications 15(1) 8075-8075 2024年9月14日  
    Ryugu is the C-type asteroid from which material was brought to Earth by the Hayabusa2 mission. A number of individual grains and fine-grained samples analysed so far for noble gases have indicated that solar wind and planetary (known as P1) noble gases are present in Ryugu samples with concentrations higher than those observed in CIs, suggesting the former to be more primitive compared to the latter. Here we present results of analyses of three fine-grained samples from Ryugu, in one of which Xe concentration is an order of magnitude higher than determined so far in other samples from Ryugu. Isotopically, this Xe resembles P1, but with a much stronger isotopic fractionation relative to solar wind and significantly lower 36Ar/132Xe ratio than in P1. This previously unknown primordial noble gas component (here termed P7) provides clues to constrain how the solar composition was fractionated to form the planetary components.
  • Yuichiro Ueno, Johan A. Schmidt, Matthew S. Johnson, Xiaofeng Zang, Alexis Gilbert, Hiroyuki Kurokawa, Tomohiro Usui, Shohei Aoki
    Nature Geoscience 2024年5月9日  
    Abstract Organic matter found in early Martian sediment may yield clues to the planet’s environmental conditions, prebiotic chemistry and habitability, but its origin remains unclear. Strong 13C depletion in sedimentary organic matter at Gale crater was recently detected by the Curiosity rover. Although this enigmatic depletion remains debated, if correct, a mechanism to cause such strong 13C depletion is required. Here we show from CO2 photolysis experiments and theoretical considerations that solar ultraviolet photolysis of CO2 in a reducing atmosphere can yield strongly 13C-depleted CO. We suggest that atmospheric synthesis of organic compounds from photolysis-produced CO is a plausible mechanism to explain the source of isotopically depleted organic matter in early Martian sediments. Furthermore, this mechanism could explain 13C enrichment of early Martian CO2 without requiring long-term carbon escape into space. A mass balance model calculation using our estimated isotopic fractionation factor indicates the conversion of approximately 20% of volcanic CO2 emissions on early Mars into organics via CO, consistent with the available data for carbon isotopes of carbonate. Although alternative pathways for organic compound production have been proposed, our findings suggest that considerable amounts of organic matter may have been synthesized from CO in a reducing early Martian atmosphere and deposited in sediments.
  • Noriko T. Kita, Kouki Kitajima, Kazuhide Nagashima, Noriyuki Kawasaki, Naoya Sakamoto, Wataru Fujiya, Yoshinari Abe, Jérôme Aléon, Conel M. O'D. Alexander, Sachiko Amari, Yuri Amelin, Ken‐ichi Bajo, Martin Bizzarro, Audrey Bouvier, Richard W. Carlson, Marc Chaussidon, Byeon‐Gak Choi, Nicolas Dauphas, Andrew M. Davis, Tommaso Di Rocco, Ryota Fukai, Ikshu Gautam, Makiko K. Haba, Yuki Hibiya, Hiroshi Hidaka, Hisashi Homma, Peter Hoppe, Gary R. Huss, Kiyohiro Ichida, Tsuyoshi Iizuka, Trevor R. Ireland, Akira Ishikawa, Shoichi Itoh, Thorsten Kleine, Shintaro Komatani, Alexander N. Krot, Ming‐Chang Liu, Yuki Masuda, Kevin D. McKeegan, Mayu Morita, Kazuko Motomura, Frédéric Moynier, Izumi Nakai, Ann Nguyen, Larry Nittler, Morihiko Onose, Andreas Pack, Changkun Park, Laurette Piani, Liping Qin, Sara S. Russell, Maria Schönbächler, Lauren Tafla, Haolan Tang, Kentaro Terada, Yasuko Terada, Tomohiro Usui, Sohei Wada, Meenakshi Wadhwa, Richard J. Walker, Katsuyuki Yamashita, Qing‐Zhu Yin, Tetsuya Yokoyama, Shigekazu Yoneda, Edward D. Young, Hiroharu Yui, Ai‐Cheng Zhang, Tomoki Nakamura, Hiroshi Naraoka, Takaaki Noguchi, Ryuji Okazaki, Kanako Sakamoto, Hikaru Yabuta, Masanao Abe, Akiko Miyazaki, Aiko Nakato, Masahiro Nishimura, Tatsuaki Okada, Toru Yada, Kasumi Yogata, Satoru Nakazawa, Takanao Saiki, Satoshi Tanaka, Fuyuto Terui, Yuichi Tsuda, Sei‐ichiro Watanabe, Makoto Yoshikawa, Shogo Tachibana, Hisayoshi Yurimoto
    METEORITICS & PLANETARY SCIENCE 2024年4月  
    Abstract Oxygen 3‐isotope ratios of magnetite and carbonates in aqueously altered carbonaceous chondrites provide important clues to understanding the evolution of the fluid in the asteroidal parent bodies. We conducted oxygen 3‐isotope analyses of magnetite, dolomite, and breunnerite in two sections of asteroid Ryugu returned samples, A0058 and C0002, using a secondary ion mass spectrometer (SIMS). Magnetite was analyzed by using a lower primary ion energy that reduced instrumental biases due to the crystal orientation effect. We found two groups of magnetite data identified from the SIMS pit morphologies: (1) higher δ18O (from 3‰ to 7‰) and ∆17O (~2‰) with porous SIMS pits mostly from spherulitic magnetite, and (2) lower δ18O (~ −3‰) and variable ∆17O (0‰–2‰) mostly from euhedral magnetite. Dolomite and breunnerite analyses were conducted using multi‐collection Faraday cup detectors with precisions ≤0.3‰. The instrumental bias correction was applied based on carbonate compositions in two ways, using Fe and (Fe + Mn) contents, respectively, because Ryugu dolomite contains higher amounts of Mn than the terrestrial standard. Results of dolomite and breunnerite analyses show a narrow range of ∆17O; 0.0‰–0.3‰ for dolomite in A0058 and 0.2‰–0.8‰ for dolomite and breunnerite in C0002. The majority of breunnerite, including large ≥100 μm grains, show systematically lower δ18O (~21‰) than dolomite (25‰–30‰ and 23‰–27‰ depending on the instrumental bias corrections). The equilibrium temperatures between magnetite and dolomite from the coarse‐grained lithology in A0058 are calculated to be 51 ± 11°C and 78 ± 14°C, depending on the instrumental bias correction scheme for dolomite; a reliable temperature estimate would require a Mn‐bearing dolomite standard to evaluate the instrumental bias corrections, which is not currently available. These results indicate that the oxygen isotope ratios of aqueous fluids in the Ryugu parent asteroid were isotopically heterogeneous, either spatially, or temporary. Initial water ice accreted to the Ryugu parent body might have ∆17O &gt; 2‰ that was melted and interacted with anhydrous solids with the initial ∆17O &lt; 0‰. In the early stage of aqueous alteration, spherulitic magnetite and calcite formed from aqueous fluid with ∆17O ~ 2‰ that was produced by isotope exchange between water (∆17O &gt; 2‰) and anhydrous solids (∆17O &lt; 0‰). Dolomite and breunnerite, along with some magnetite, formed at the later stage of aqueous alteration under higher water‐to‐rock ratios where the oxygen isotope ratios were nearly at equilibrium between fluid and solid phases. Including literature data, δ18O of carbonates decreased in the order calcite, dolomite, and breunnerite, suggesting that the temperature of alteration might have increased with the degree of aqueous alteration.
  • Kaori Hirata, Tomohiro Usui, Ryuki Hyodo, Hidenori Genda, Ryota Fukai, David J. Lawrence, Nancy L. Chabot, Patrick N. Peplowski, Hiroki Kusano
    Icarus 410 2024年3月1日  
    The formation process of the two Martian moons, Phobos and Deimos, is still debated with two main competing hypotheses: the capture of an asteroid or a giant impact onto Mars. In order to reveal their origin, the Martian Moons eXploration (MMX) mission by Japan Aerospace Exploration Agency (JAXA) plans to measure Phobos’ elemental composition by a gamma-ray and neutron spectrometer called MEGANE. This study provides a model of Phobos’ bulk elemental composition, assuming the two formation hypotheses. Using the mixing model, we established a MEGANE data analysis flow to discriminate between the formation hypotheses by multivariate analysis. The mixing model expresses the composition of Phobos in 6 key lithophile elements that will be measured by MEGANE (Fe, Si, O, Ca, Mg, and Th) as a linear mixing of two mixing components: material from Mars and material from an asteroid as represented by primitive meteorite compositions. The inversion calculation includes consideration of MEGANE's measurement errors (EP) and derives the mixing ratio for a given Phobos composition, based on which the formation hypotheses are judged. For at least 65% of the modeled compositions, MEGANE measurements will determine the origin uniquely (EP = 30%), and this increases from 74 to 87% as EP decreases from 20 to 10%. Although the discrimination performance depends on EP, the current operation plan for MEGANE predicts an instrument performance for EP of 20—30%, resulting in 70% discrimination between the original hypotheses. MEGANE observations can also enable the determination of the asteroid type of the captured body or the impactor. The addition of other measurements, such as MEGANE's measurements of the volatile element K, as well as observations by other MMX remote sensing instruments, will also contribute to the MMX mission's goal to constrain the origin of Phobos.
  • Yan Hu, Frédéric Moynier, Wei Dai, Marine Paquet, Tetsuya Yokoyama, Yoshinari Abe, Jérôme Aléon, Conel M. O'D. Alexander, Sachiko Amari, Yuri Amelin, Ken-ichi Bajo, Martin Bizzarro, Audrey Bouvier, Richard W. Carlson, Marc Chaussidon, Byeon-Gak Choi, Nicolas Dauphas, Andrew M. Davis, Tommaso Di Rocco, Wataru Fujiya, Ryota Fukai, Ikshu Gautam, Makiko K. Haba, Yuki Hibiya, Hiroshi Hidaka, Hisashi Homma, Peter Hoppe, Gary R. Huss, Kiyohiro Ichida, Tsuyoshi Iizuka, Trevor R. Ireland, Akira Ishikawa, Shoichi Itoh, Noriyuki Kawasaki, Noriko T. Kita, Koki Kitajima, Thorsten Kleine, Shintaro Komatani, Alexander N. Krot, Ming-Chang Liu, Yuki Masuda, Mayu Morita, Kazuko Motomura, Izumi Nakai, Kazuhide Nagashima, David Nesvorný, Ann Nguyen, Larry Nittler, Morihiko Onose, Andreas Pack, Changkun Park, Laurette Piani, Liping Qin, Sara S. Russell, Naoya Sakamoto, Maria Schönbächler, Lauren Tafla, Haolan Tang, Kentaro Terada, Yasuko Terada, Tomohiro Usui, Sohei Wada, Meenakshi Wadhwa, Richard J. Walker, Katsuyuki Yamashita, Qing-Zhu Yin, Shigekazu Yoneda, Edward D. Young, Hiroharu Yui, Ai-Cheng Zhang, Tomoki Nakamura, Hiroshi Naraoka, Takaaki Noguchi, Ryuji Okazaki, Kanako Sakamoto, Hikaru Yabuta, Masanao Abe, Akiko Miyazaki, Aiko Nakato, Masahiro Nishimura, Tatsuaki Okada, Toru Yada, Kasumi Yogata, Satoru Nakazawa, Takanao Saiki, Satoshi Tanaka, Fuyuto Terui, Yuichi Tsuda, Sei-ichiro Watanabe, Makoto Yoshikawa, Shogo Tachibana, Hisayoshi Yurimoto
    Icarus 409 115884-115884 2024年2月  

MISC

 28
  • Ryuki Hyodo, Tomohiro Usui
    SCIENCE 373(6556) 742-742 2021年8月  
  • 臼井寛裕, 菅倉春菜, 倉本圭, 倉本圭, 川勝康弘
    宇宙科学技術連合講演会講演集(CD-ROM) 65th 2021年  
  • 吉村義隆, 山岸明彦, 宮川厚夫, 今井栄一, 佐々木聰, 塩谷圭吾, 三田肇, 小林憲正, 癸生川陽子, 佐藤直人, 佐藤毅彦, 薮田ひかる, 長沼毅, 藤田和央, 臼井寛裕
    日本惑星科学会秋季講演会予稿集(Web) 2020 2020年  
  • 臼井寛裕, 関華奈子, 藤田和央
    日本惑星科学会秋季講演会予稿集(Web) 2020 2020年  
  • 鈴木 慧花, 菅 大暉, 山口 亮, 臼井 寛裕, 新田 清文, 関澤 央輝, 高橋 嘉夫
    日本地球化学会年会要旨集 66 177-177 2019年  
    <p>火星隕石ナクライトにはIddingsiteという変質脈が存在し、この中の変質鉱物には火星での水の痕跡が残されている。しかし、変質鉱物には炭酸塩と硫酸塩(jarositeなど)という異なるEh-pH条件で形成したと考えられる物質が共存しており、火星でのIddingsite形成環境・過程は不明瞭である。また、これらの関係性を正確に議論した研究は今までにほとんどない。本研究ではナクライト隕石Y000593のIddingsiteを対象とし、微量元素とその化学種に着目した分析を行った。従来の隕石分析に用いるSEM・EPMA分析に、放射光をベースとしたX線顕微分析(μ-XRF-XAFS@BL37XU SPring-8とsemi-μ-XRF-XAFS@BL-15A KEK-PF)から得られる知見を組み合わせることで、変質過程の詳細な解明を試みた。</p>
  • Akihiko Yamagishi, Takeshi Kakegawa, Tomohiro Usui
    Astrobiology: From the Origins of Life to the Search for Extraterrestrial Intelligence v-vi 2019年1月1日  
  • 佐々木聰, 吉村義隆, 山岸明彦, 塩谷圭吾, 大野宗祐, 宮川厚夫, 藤田和央, 臼井寛裕
    日本化学会春季年会講演予稿集(CD-ROM) 99th 2019年  
  • 関華奈子, 渡部重十, 中本泰史, 寺田直樹, 山崎敦, 松岡彩子, 臼井寛裕, 関根康人, 藤田和央, 横田勝一郎, 笠原慧, 斎藤義文, 中川広務, 熊本篤志, 前澤裕之
    日本地球惑星科学連合大会予稿集(Web) 2019 2019年  
  • 吉村義隆, 山岸明彦, 佐藤毅彦, 宮川厚夫, 今井栄一, 佐々木聰, 小林憲正, 癸生川陽子, 岡田朋華, 塩谷圭吾, 薮田ひかる, 長沼毅, 三田肇, 藤田和央, 臼井寛裕
    日本惑星科学会秋季講演会予稿集(Web) 2019 2019年  
  • 吉村義隆, 山岸明彦, 佐藤毅彦, 宮川厚夫, 今井栄一, 佐々木聰, 小林憲正, 癸生川陽子, 薮田ひかる, 長沼毅, 三田肇, 藤田和央, 臼井寛裕, 臼井寛裕
    日本惑星科学会誌 遊・星・人 27(3) 2018年  
  • 吉村義隆, 山岸明彦, 佐藤毅彦, 宮川厚夫, 今井栄一, 佐々木聰, 小林憲正, 癸生川陽子, 薮田ひかる, 長沼毅, 三田肇, 藤田和央, 臼井寛裕, 臼井寛裕
    日本惑星科学会秋季講演会予稿集(Web) 2018 2018年  
  • 藤田 和央, 畠中 龍太, 西 顕太郎, 池永 敏憲, 鈴木 俊之, 春木 美鈴, 小澤 宇志, 野村 哲史, 臼井 寛裕, 宮本 英昭, 亀田 真吾, Fujita Kazuhisa, Hatakenaka Ryuta, Nishi Kentaro, Ikenaga Toshinori, Suzuki Toshiyuki, Haruki Misuzu, Ozawa Takashi, Nomura Satoshi, Usui Tomohiro, Miyamoto Hirdy, Kameda Singo
    平成29年度宇宙航行の力学シンポジウム = Symposium on Flight Mechanics and Astrodynamics: 2017 2017年12月  
    平成29年度宇宙航行の力学シンポジウム(2017年12月7日-8日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)), 相模原市, 神奈川県著者人数: 11名資料番号: SA6000124018
  • Tomohiro Usui
    NATURE 552(7685) 339-340 2017年12月  
  • 山岸 明彦, 佐藤 毅彦, 宮川 厚夫, 吉村 義隆, 長沼 毅, 佐々木 聰, 今井 栄一, 出村 裕英, 薮田 ひかる, 三田 肇, 癸生川 陽子, 小林 憲正, 塩谷 圭吾, 宮本 英昭, 石上 玄也, 藤田 和央, 臼井 寛裕, Yamagishi Akihiko, Satoh Takehiko, Miyakawa Atsuo, Yoshimura Yoshitaka, Naganuma Takeshi, Sasaki Satoshi, Imai Eiichi, Demura Hirohide, Yabuta Hikaru, Mita Hajime, Kebukawa Yoko, Kobayashi Kensei, Enya Keigo, Miyamoto Hideaki, Ishigami Genya, Fujita Kazuhisa, Usui Tomohiro
    第50回月・惑星シンポジウム = Proceedings of the 50th ISAS Lunar and Planetary Symposium 2017年8月  
    第50回月・惑星シンポジウム (2017年8月3-4日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)), 相模原市, 神奈川県著者人数: 17名資料番号: SA6000200012
  • 関根康人, 渋谷岳造, 玄田英典, 福士圭介, 臼井寛裕, 高橋嘉夫, 倉本圭, 鍵裕之, 渡邊誠一郎
    日本惑星科学会秋季講演会予稿集(Web) 2017 2017年  
  • 山岸明彦, 佐藤毅彦, 宮川厚夫, 塩谷圭吾, 吉村義隆, 佐々木聰, 小林憲正, 癸生川陽子, 藪田ひかる, 三田肇, 今井栄一, 長沼毅, 出村裕英, 藤田和央, 臼井寛裕
    日本惑星科学会秋季講演会予稿集(Web) 2017 2017年  
  • 臼井寛裕, 佐藤毅彦, 亀田真吾, 宮本英昭, 山岸明彦, 藤田和央, 石上玄也
    日本惑星科学会秋季講演会予稿集(Web) 2017 2017年  
  • 倉本 圭, 藤本 正樹, 玄田 英典, 今村 剛, 亀田 真吾, 川勝 康弘, 松本 晃治, 三桝 裕也, 宮本 英昭, 諸田 智克, 中村 智樹, 小川 和律, 尾崎 正伸, 澤田 弘崇, 橘 省吾, 寺田 直樹, 臼井 寛裕, 和田 浩二, 渡邊 誠一郎, MMXサイエンスチーム
    宇宙科学技術連合講演会講演集 60 5p 2016年9月6日  
  • 山岸 明彦, 佐藤 毅彦, 宮川 厚夫, 吉村 義隆, 長沼 毅, 佐々木 聰, 今井 栄一, 出村 英裕, 薮田 ひかる, 三田 肇, 癸生川 陽子, 小林 憲正, 塩谷 圭吾, 宮本 英昭, 石上 玄也, 藤田 和央, 臼井 寛裕, Yamagishi Akihiko, Satoh Takehiko, Miyakawa Atsuo, Yoshimura Yoshitaka, Naganuma Takeshi, Sasaki Satoshi, Imai Eiichi, Demura Hidrohide, Yabuta Hikaru, Mita Hjime, Kebukawa Yoko, Kobayashi Kensei, Enya Keigo, Miyamoto Hideaki, Ishigami Genya, Fujita Kazuhisa, Usui Tomohiro
    第49回月・惑星シンポジウム = Proceedings of the 49th ISAS Lunar and Planetary Symposium 2016年7月  
    第49回月・惑星シンポジウム (2016年7月20-21日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)), 相模原市, 神奈川県著者人数: 17名資料番号: SA6000059023
  • 深海 雄介, 飛田 南斗, 横山 哲也, 森脇 涼太, 臼井 寛裕
    日本地球化学会年会要旨集 63 181-181 2016年  
    <p>数ナノグラム以下の極微量Pb同位体分析時に分析精度に大きく影響するのは、存在度の最も低い同位体である204Pb (1.4%)の信号強度の低さであり、極微量PbについてPbイオン信号強度を最大化する事が分析精度の向上に重要である。本研究では、極微量Pb(< 2 ng)に対して同位体分析手法の最適化を行い、表面電離型質量分析計(TIMS)を用いてトータルエバポレーション法と204Pb-207Pbダブルスパイク法を併用した高精度Pb同位体分析手法の開発を行った。Pb信号強度の最大化と測定精度向上のために、イオン化促進剤の量、試料塗布幅、フィラメント電流値変化、測定値の計算方法の検討を行った。本研究の手法における208Pb/204Pb比の繰り返し再現性(2S.D.)として、0.160/00 (2 ng)、0.450/00 (0.5 ng)、1.30/00 (0.1 ng)が得られた。</p>
  • 山岸明彦, 佐藤毅彦, 宮川厚夫, 吉村義隆, 長沼毅, 佐々木聰, 今井栄一, 出村裕英, 藪田ひかる, 三田肇, 癸生川陽子, 小林憲正, 塩谷圭吾, 宮本英昭, 石上玄也, 藤田和央, 臼井寛裕
    日本惑星科学会秋季講演会予稿集(Web) 2016 2016年  
  • Tomohiro Usui, Audrey Bouvier, Justin I. Simon, Noriko Kita
    GEOCHEMICAL JOURNAL 50(1) 1-2 2016年  
  • 山岸明彦, 佐藤毅彦, 宮川厚夫, 吉村義隆, 本多元, 佐々木聡, 今井栄一, 臼井寛裕, 宮本英昭, 藤田和央
    日本地球惑星科学連合大会予稿集(Web) 2015 2015年  
  • 臼井 寛裕, Alexander C. M.O'D., Wang J., Simon J. I., Jones J. H.
    日本惑星科学会秋期講演会予稿集 2013 "O2-01" 2013年11月20日  
  • 森脇 涼太, 臼井 寛裕, 横山 哲也
    日本惑星科学会秋期講演会予稿集 2013 "P1-25" 2013年11月20日  
  • 佐藤毅彦, 久保田孝, 藤田和央, 岡田達明, 岩田隆浩, 今村剛, 大山聖, 尾川順子, 山田和彦, 宮本英昭, 山岸明彦, 小松吾郎, 臼井寛裕, はしもと じょーじ, 出村裕英, 千秋博紀, 佐々木晶, 石上玄也
    宇宙科学技術連合講演会講演集(CD-ROM) 57th 2013年  
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共同研究・競争的資金等の研究課題

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