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Tatsuaki Okada

  (岡田 達明)

Profile Information

Affiliation
Associate Professor, Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency
Graduate School of Science, Department of Chemistry, The University of Tokyo
Degree
Ph.D.(Mar, 1996, University of Tokyo)
Researcher number
30321566
J-GLOBAL ID
201501026547105146
researchmap Member ID
B000243484
External link

専門は惑星科学、惑星物理学、惑星物質・物性科学、惑星探査科学。特に熱赤外カメラを用いた史上初の小惑星探査により、惑星探査に「熱撮像」の手法を世界で初めて導入に成功し、さらに「太陽系物性科学」の分野を創設。観測機器の開発による惑星探査でのその場観測とサンプルリターンによる帰還試料分析を主な研究手法とする。

主要な開発機器は、蛍光Ｘ線分光計、熱赤外カメラ、多波長熱赤外カメラである。また開発中のものはマルチターン飛行時間型質量分析計等である。地上分析においてはハイパースペクトル顕微鏡（フランスIAFとの共同）やロックインサーモグラフィ法による熱拡散率顕微鏡（石崎拓也氏と共同）による帰還試料の分析の他、将来の資料熱物性分析のための多色熱赤外顕微鏡の開発を推進中である。

◆国内外の惑星探査計画（観測機器担当）

・月探査「Lunar-A」　光学カメラLIC（Co-I）1993-2005 

・火星探査「のぞみ」　HFレーダ高度計PWS/ALT（Co-I）1994-2003、可視カメラMIC（Co-I）1995-2003

・小惑星探査「はやぶさ」　蛍光エックス線分光計XRS担当（PI）1995-2010

・月周回探査「かぐや（SELENE）」　蛍光Ｘ線分光計XRS担当（PI）1998-2009

・小惑星探査「はやぶさ２」　中間赤外カメラTIR担当（PI）2010-present.、

・小惑星探査「はやぶさ２」　小型ランダーMASCOT担当（JAXAリエゾン）2010-2019

・小惑星探査「はやぶさ２」　デジタルエレキDE担当（PI）2010-present

・小惑星探査「はやぶさ２」　ハイパースペクトル顕微鏡MicrOmega担当（Co-PI）2019-present

・二重小惑星探査計画Hera　熱赤外カメラTIRI担当（PI）2020-present

・二重小惑星探査計画Hera　Hera Investigation Team メンバ（招聘）2020-present

・地球近傍遭遇小惑星探査計画RAMSES　熱赤外カメラTIRI担当（PI）2025-present

◆帰還サンプルの分析（地上分析）

・JAXAキュレーションセンター（地球外物質研究グループ所属）2009-present

・ハイパースペクトル顕微鏡MicrOmega-CF（Co-PI）

・熱赤外顕微鏡（PI）

◆海外ミッション参画

・SMART-1　D-CIXS（Co-I）2000-2005

・Chandrayaan-1　C1XS（Co-I）2006-2009

・BepiColombo MIXS（Co-I）2003-present、SIXS （Co-I）2003-present

・Hera (-JP) Proejct Manager & TIRI（PI）2020-present、Investigation Team 2020-present

◆WG参画

・ESA MarcoPolo（=Hayabusa-MkII）においてX線分光、熱積外カメラ、着陸機

・月着陸機SELENE-B、SELENE-II

・月着陸SLIM（科学システム検討担当）

・火星探査MELOS（科学システム検討担当（固体惑星）、着陸探査）

・OKEANOS （科学システム検討担当、質量分析計HRMSの開発）

・月縦孔探査Uzume（科学システム検討担当、熱赤外カメラの開発）

・次世代小天体サンプルリターン理学WG（代表）

 

Research Interests

 32

Research Areas

 1

Research History

 7
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Education

 4

Committee Memberships

 3

Awards

 24
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Papers

 258
  • Tatsuaki Okada, Satoshi Tanaka, Naoya Sakatani, Yuri Shimaki, Takehiko Arai, Hiroki Senshu, Hirohide Demura, Tomohiko Sekiguchi, Toru Kouyama, Masanori Kanamaru, Takuya Ishizaki, Soichiro Furukawa, Ramon Vilardell-Belles, Özgür Karatekin, Joris Blommaert
    Space Science Reviews, Dec, 2025  
  • C. Pilorget, T. Okada, J.-P. Bibring, D. Loizeau, K. Hatakeda, L. Nardelli, L. Riu, R. Sheppard, T. Jiang, M. Mahlke, R. Brunetto, D. Baklouti, R. Fukai, M. Abe, A. Aléon-Toppani, Y. Enokido, V. Hamm, S. Kawasaki, C. Lantz, A. Miyazaki, A. Moussi-Soffys, M. Nishimura, F. Poulet, R. Tahara, T. Usui, T. Yada, K. Yogata
    Nature Communications, Nov 4, 2025  
  • Tatsuaki Okada, Satoshi Tanaka, Naoya Sakatani, Yuri Shimaki, Takehiko Arai, Hiroki Senshu, Hirohide Demura, Tomohiko Sekiguchi, Toru Kouyama, Masanori Kanamaru, Takuya Ishizaki, Ramon Vilardell Belles, Soichiro Furukawa, Ozgur Karatekin, Joris Blommaert, Luca Ruiz Lozano, Gregoire Henry, Jonathan Leon Tavares, Birgit Ritter, Orkun Temel
    Jul 9, 2025  
  • Özgür Karatekin, Tatsuaki Okada, Naoya Sakatani, Joris Blommaert, Grégoire Henry, Luca Ruiz Lozano, Orkun Temel, Birgit Ritter, Dirk Nuyts, Jonathan Leon Tavares, Masanori Kanamaru, Yuri Shimaki, Takehiko Arai, Hiroki Senshu, Hirohide Demura, Tomohiko Sekiguchi, Toru Kouyama, Satoshi Tanaka, Patrick Michel, Michael Küppers
    Mar 15, 2025  
  • Maria Schönbächler, Manuela A. Fehr, Tetsuya Yokoyama, Ikshu Gautam, Nao Nakanishi, Yoshinari Abe, Jérôme Aléon, Conel 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, Makiko K. Haba, Yuki Hibiya, Hiroshi Hidaka, Hisashi Homma, Peter Hoppe, Gary R. Huss, Kiyohiro Ichida, Tsuyoshi Iizuka, Trevor 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, Frédéric Moynier, Izumi Nakai, Kazuhide Nagashima, Ann Nguyen, Larry Nittler, Morihiko Onose, Andreas Pack, Changkun Park, Laurette Piani, Liping Qin, Sara Russell, Naoya Sakamoto, 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
    Meteoritics & Planetary Science, Nov 25, 2024  
    Abstract Nucleosynthetic isotope variations are powerful tracers to determine genetic relationships between meteorites and planetary bodies. They can help to link material collected by space missions to known meteorite groups. The Hayabusa 2 mission returned samples from the Cb‐type asteroid (162173) Ryugu. The mineralogical, chemical, and isotopic characteristics of these samples show strong similarities to carbonaceous chondrites and in particular CI chondrites. The nucleosynthetic isotope compositions of Ryugu overlap with CI chondrites for several elements (e.g., Cr, Ti, Fe, and Zn). In contrast to these isotopes, which are of predominately supernovae origin, s‐process variations in Mo isotope data are similar to those of carbonaceous chondrites, but even more s‐process depleted. To further constrain the origin of this depletion and test whether this signature is also present for other s‐process elements, we report Zr isotope compositions for three bulk Ryugu samples (A0106, A0106‐A0107, C0108) collected from the Hayabusa 2 mission. The data are complemented with that of terrestrial rock reference materials, eucrites, and carbonaceous chondrites. The Ryugu samples are characterized by distinct 96Zr enrichment relative to Earth, indicative of a s‐process depletion. Such depletion is also observed for carbonaceous chondrites and eucrites, in line with previous Zr isotope work, but it is more extreme in Ryugu, as observed for Mo isotopes. Since s‐process Zr and Mo are coupled in mainstream SiC grains, these distinct s‐process variations might be due to SiC grain depletion in the analyzed materials, potentially caused by incomplete sample digestion, because the Ryugu samples were dissolved on a hotplate only to avoid high blank levels for other elements (e.g., Cr). However, local depletion of SiC grains cannot be excluded. An alternative, equally possible scenario is that aqueous alteration redistributed anomalous, s‐process‐depleted, Zr on a local scale, for example, into Ca‐phosphates or phyllosilicates.
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Misc.

 536
  • 岡田達明
    日本惑星科学会誌 遊・星・人, 14(3), 2005  
  • Ogawa Kazunori, Okada Tatsuaki, Shirai Kei, Kato Manabu
    Abstracts for fall meeting of the Japanese Society for Planetary Science, 2005 33-33, 2005  
    We have developed a X-ray analyzer for future SELENE-2 lunar lander. The X-ray fluorescence spectrometer / diffractometer (XRF/XRD) is mounted on SELENE-2 lander, and will analyze lunar rock samples which SELENE-2 rover picks up from scientifically important area on the lunar surface. The X-ray tube as a primary X-ray generator for the XRF/XRD has some advantages to carry out quicker and higher quality measurements, compared with radioactive isotopes which were conventionally used in past landing missions. The problem to mount X-ray tube on the spacecraft is its large size and mass. We adopt a new type of X-ray tube based on electron field emission (FE) from carbon nanotubes (CNT) to achieve significant miniaturization. This presentation shows results of our experiments of the electron field emission, and actual application methods of the miniaturized X-ray tube on the X-ray instrument.
  • Okada Tatsuaki, Kato Manabu, Shirai Kei, Arai Takehiko, Ogawa Kazunori, Hosono Kozue, Inoue Tatsutoshi, Inoue Tomoka, Maruyama Yoko, Yamamoto Yukio
    Abstracts for fall meeting of the Japanese Society for Planetary Science, 2005 40-40, 2005  
    The Hayabusa will rendezvous 25143 Itokawa, an S (IV)-class near-earth asteroid, in September to October, 2005. The XRS is among the remote sensing instruments aboard. We present here the main objectives of the XRS observation. The XRS will determine major elemental composition of surface of the asteroid. Elemental variation will be surveyed by asteroid rotation in longitudinal direction, maybe with spatial resolution of 60 degrees. The XRS always detect such major elements as Mg, Al, Si, and S, but it also can do for higher atomic number elements such as Ca and Fe, especially during the occurrence of solar flare. Furthermore, microscopic roughness of the surface is informed by observation at various solar phase angles due to particle size effect in X-ray fluorescence. Since thermal design of the XRS has been well calibrated, thermal radiation intensity off the asteroid surface will be estimated by monitoring the temperature profile during descent of the spacecraft for asteroid touchdown.
  • Arai Takehiko, Yamamoto Yukio, Okada Tatsuaki, Shirai Kei, Ogawa Kazunori, Hosono Kozue, Kato Manabu
    Abstracts for fall meeting of the Japanese Society for Planetary Science, 2005 58-58, 2005  
    SELENE XRS will determine major elemental composition of lunar surface. In this study, we will introduce the intelligent observation system of XRS with onboard computer-control.
  • Hosono Kozue, Shirai Kei, Arai Takehiko, Ogawa Kazunori, Okada Tatsuaki, Kato Manabu
    Abstracts for fall meeting of the Japanese Society for Planetary Science, 2005 59-59, 2005  
    XRS ( X-Ray fluorescence Spectrometer ) which will be installed on SELENE , will observe x-ray fluorescence emitted from the lunar surface and quantify the major elemental composition of the lunar surface. Determination accuracy for major elemental composition of the lunar surface can be enhanced by comparing spectrum from the lunar surface with one from the standard sample. In this study , we attemped to evaluate the accuracy of elemental composition ratio acquired by this method.
  • 岡田 達明, 加藤 學, 佐々木 晶
    宇宙科学シンポジウム, 4 235-238, Jan 8, 2004  
  • 加藤 學, 佐々木 晶, 岡田 達明
    宇宙科学シンポジウム, 4 243-246, Jan 8, 2004  
  • 岡田達明, 佐伯和人, 杉原孝充, 佐々木晶, 加藤学
    太陽系科学シンポジウム, 25th, 2004  
  • 向井利典, 早川基, 山川宏, 小川博之, 笠羽康正, 岡田達明
    日本惑星科学会秋季講演会予稿集, 2004, 2004  
  • 細野梢, 細野梢, 荒井武彦, 荒井武彦, 岡田達明, 加藤学
    日本惑星科学会秋季講演会予稿集, 2004, 2004  
  • 小川和律, 加藤学, 岡田達明, 白井慶, 山本幸生, 荒井武彦, 菊池宣陽
    太陽系科学シンポジウム, 25th, 2004  
  • Kato Manabu, Okada Tatsuaki, Shirai Kei, Yamamoto Yukio, Arai Takehiko, Ogawa Kazunori, Hosono Kozue, Takigawa Akihiro, SELENE XRS Team
    Abstracts for fall meeting of the Japanese Society for Planetary Science, 2004 34-34, 2004  
    The SELENE (SELenological and Engineering Explorer) is a Japanese lunar polar orbiter with 14 scientific instruments. The XRS is to map major elemental composition in 20km spatial resolution, to provide the clue to understanding the lunar evolution. Energy resolution and efficient detection area of the XRS has been much improved by using arrays of Si CCD with 100cm2 detection area and ultra-thin beryllium window for better transparency at low energy. We present the specification, performance and current status of the XRS and method of remote X-ray spectrometry.
  • Ogawa Kazunori, Okada Tatsuaki, Kato Manabu
    Abstracts for fall meeting of the Japanese Society for Planetary Science, 2004 42-42, 2004  
  • Okada Tatsuaki, Hasebe Nobuyuki, Kato Manabu, Grande Manuel, Dunkin Sarah K., Muinonen Karri, d'Uston Claude, MIXS & MANGA Team
    Abstracts for fall meeting of the Japanese Society for Planetary Science, 2004 78-78, 2004  
    The first global remote X-ray and gamma-ray spectrometry have been proposed for the Bepi Colombo mission, to map abundances of major and radioactive elements on the surface of Mercury. The Mercury Planetary Orbiter (MPO) that orbits around the relatively low altitude (400 x 1500 km) appropriate for surface global mapping. We present the outlines of X-ray and Gamma-ray spectrometers that have been designed with new technologies such as the X-ray detector using GaAs array on ASIC as well as the low-power stirling cryostat for pure germanium Gamma-ray detector.
  • 佐々木 晶, 久保田 孝, 岡田 達明
    宇宙科学シンポジウム, 3 75-78, Jan 9, 2003  
  • 菊池宣陽, 山本幸生, 荒井武彦, 白井慶, 岡田達明, 加藤学
    太陽系科学シンポジウム, 24th, 2003  
  • 岡田達明, 加藤學, 白井慶, 山本幸生, 荒井武彦, 荒井武彦
    搭載機器基礎開発実験経費・宇宙科学推進戦略的開発研究経費実績報告書, 2003, 2003  
  • OKADA TATSUAKI, SHIRAI KEI, Rover/Science Team the SELENE-B, SUGIHARA TAKAMITSU, SAIKI KAZUTO, AKIYAMA HIROAKI, OHTAKE MAKIKO, SASAKI SHO, HASEBE NOBUYUKI, KUNII YASUHARU, KUBOTA TAKASHI
    Abstracts for fall meeting of the Japanese Society for Planetary Science, 2003 48-48, 2003  
    We have been studying the instrumentation onboard the lander and rover for a lunar geological exploration with the SELENE-B that demonstrates the next generation technologies of a pin-point and soft landing on planetary surfaces of scientific interest and an autonomous controlled scientific rover. In this mission, imaging spectroscopy and multi-band imagery will characterize the target site around a crater central peak and gamma-ray spectrometry will measure radioactivity along the rover's track. Lunar rocks and soils at the target crops or around the lander are selected to brush up and grind for detailed analyses by microscopy and x-ray fluorescence/diffraction method. The systematic configuration of instruments is also introduced.
  • KATO Manabu, OKADA Tatsuaki, SHIRAI KEI, YAMAMOTO Yukio, ARAI Takehiko, KIKUCHI Nobuaki, OGAWA Kazunori, Team XRS
    Abstracts for fall meeting of the Japanese Society for Planetary Science, 2003 70-70, 2003  
    The SELENE (SELenological and Engineering Explorer) is a Japanese lunar polar orbiter and performs lunar global mapping with more than 10 scientific instruments. The XRS will map major elemental composition in 20km spatial resolution and provide the clue to understanding the lunar evolution. For that purpose, the XRS has been designed to improve energy resolution and efficient detection area. Then the X-ray detector has arrays of CCD with 100cm2 detection area, and is kept below -50C by radiation cooling. Ultra-thin beryllium window are developed for better transparency at low energy. We present the specification and the current status of the XRS as prepared for the interface test, as well as the plan of pre-flight tests and observation plan.
  • OKADA TATSUAKI, SHIRAI KEI, YAMAMOTO YUKIO, ARAI TAKEHIKO, KIKUCHI NOBUAKI, OGAWA KAZUNORI, KATO MANABU, XRS TEAM
    Abstracts for fall meeting of the Japanese Society for Planetary Science, 2003 85-85, 2003  
    We present the results of initial operation, the current status, and the future observation plan of the X-ray fluorescence spectrometer (XRS) onboard Hayabusa, which was launched with the fifth M-V launch vehicle on May 9th, 2003. The XRS observes X-rays characteristic of elements excited by solar irradiation, to determine major elemental composition of asteroid Itokawa (1998SF36). Then we classify the S-class asteroid and prospect the degree of evolution processes. During the two-year long cruising phase, the XRS are checked out its function and the detectors against radiation damage, and observes X-ray bodies such as super nova remnants or active galactic cores as well as cosmic backgrounds of X-rays for in-flight calibration. The XRS also monitors solar X-rays using the standard sample. Flight demonstration of the newly developed onboard computer proves usability for more than 20 days.
  • Arai Takehiko, Yamamoto Yukio, Shirai Kei, Okada Tatsuaki, Kato Manabu
    Abstracts for fall meeting of the Japanese Society for Planetary Science, 2003 62-62, 2003  
    X-ray fluorescence spectrometer (XRS) onboard HAYABUSA (MUSES-C) spacecraft that was launched by the fifth M-V launch vehicle on 9 May 2003. The XRS has plans to observe supernova remnants (SNR), active galactic nuclei (AGN) and cosmic X-ray backgrounds for in-flight calibration and scientific observation during the transfer and return phase. When HAYABUSA spacecraft performed tests of the ion electric propulsion system (IES) and its heater control system, the XRS observed spectra were noisy. This study shows method of reducing heat noise.
  • Yamamoto Yukio, Arai Takehiko, Shirai Kei, Okada Tatsuaki, Kato Manabu
    Abstracts for fall meeting of the Japanese Society for Planetary Science, 2003 66-66, 2003  
    X-ray spectrometer onboard HAYABUSA spacecraft has a standard sample to perform comparative analysis. Comparing with the X-rays from the standard sample and asteroid surface, the dependency of induced X-ray, solar X-rays, is reduced [1].<BR>It takes more than 2 years to reach the Asteroid, and the temporal variance of the XRS performance is investigated periodically by the observation of the X-rays from Cosmic X-ray Backgrounds, astronomical X-ray bodies, and the standard sample.<BR>From 28 May 2003 to 30 May 2003, just after the launch of HAYABUSA, XRS observed an X-ray source: SCO-X1 [2]. The observation continued two days due to the initial checkout. Fortunately, an X.1 class solar flare happened during this term. The spectra from the standard sample were composed of Ca and Si line spectra together with Mg, Al, and Si line spectra. These data is available for the XRS in-flight calibration: energy gain and intensities. In addition, model parameter is determined by this data.<BR>Yamamoto et al reported that the energy calibration, comparison of the energy flux between GOED 10 and XRS, and the comparison of the observation and calculation using thess data [3]. The energy calibration of the line spectra: Mg, Al, Si, Ca, and Fe, was determined within 1% accuracy comparing with 55Fe calibration data before launch. Temporal variation of energy flux obtained by XRS showed the consistency with that obtained by GOES 10 satellite. Moreover, the model calculation was performed and compared with the observation. The comparison showed the background noise in the energy range 0.5-3keV clearly existed. This noise was serious problem to determine the intensities of Mg, Al, and Si X-ray fluorescence spectra.Therefore, we report here the method to remove this background noise, and the effect of the method.<BR>[1] Okada, T., Fujiwara, A., Tsunemi, H., and Kitamoto, S. 2000. X-ray fluorescence spectrometer onboard MUSES-C, Adv. Space Res. 25, 345-348.<BR>[2] Arai et al, 2003. Proc. ISAS Lunar Planet. Symp.<BR>[3] Yamamoto et al, 2003. Proc. ISAS Lunar Planet. Symp.<BR>
  • sugihara takamitsu, sasaki sho, saiki kazuto, okada tatsuaki
    Abstracts for fall meeting of the Japanese Society for Planetary Science, 2003 46-46, 2003  
  • 岡田達明, 杉原孝充, 国井康晴
    宇宙科学シンポジウム 平成14年度 第3回, 3 79-82, 2003  
  • 白井慶, 青木美希, 山本幸生, 荒井武彦, 赤川健一, 岡田達明, 加藤学
    宇宙科学シンポジウム 平成14年度 第3回, 87-88, 2003  
  • 国井康晴, 佐伯和人, 久保田孝, 金森洋史, 若林幸子, 杉原孝充, 岡田達明, 大竹真紀子, 佐々木晶
    宇宙科学技術連合講演会講演集, 46th(Pt.3), 2002  
  • ARAI Takehiko, YAMAMOTO Yukio, OKADA Tatsuaki, KATO Manabu
    Abstracts for fall meeting of the Japanese Society for Planetary Science, 2002 55-55, 2002  
  • Akagawa Kenichi, Okada Tatsuaki, Yamamoto Yukio, Kato Manabu
    Abstracts for fall meeting of the Japanese Society for Planetary Science, 2002 61-61, 2002  
  • Sasaki Sho, Demura Hirohide, Kanamori Hiroshi, Haruyama Jun-ichi, Matsumoto Kotaro, Wakabayashi Sachiko, Akiyama Hiroaki, Takeda Hiroshi, Shibamura Eido, Hasebe Nobuyuki, Kubota Takashi, Okada Tatsuaki, Kato Manabu, Saiki Kazuto, Kunii Yasuharu, Otake Makiko, Sugihara Takamitsu, Hirata Naru
    SICE Division Conference Program and Abstracts, 2002 441-441, 2002  
    Unmanned lunar geologic exploration of a crater&rsquo;s central peak to investigate subsurface layering is discussed. Rover-lander corporative mission is executed. From a lander which is within 500m from the frank of the central peak, a rover should make a round-trip to the frank and bring samples back to the lander. Multi-band camera, gamma-ray spectrometer, rock-coring mechanism, sampling and transportation mechanism should be on board the rover. Detailed analyses of the returned samples including microscopic spectroscopy and X-ray spectrometry and diffraction should be done in the lander.
  • 岡田 達明, 水星探査WG
    宇宙科学シンポジウム, 2 17-20, Nov 19, 2001  
  • 佐々木 晶, 久保田 孝, 岡田 達明
    宇宙科学シンポジウム, 2 57-59, Nov 19, 2001  
  • Aoki M., Shirai K., Okada T., Kato M.
    Abstracts Fall Meeting of the Japanese Society for Planetary Sciences, 2001 27-27, Oct 6, 2001  
    We are developing X-Ray fluorescence spectrometer onboard MUSES-C which will be launched in 2002. Charge-coupled device (CCD) is used to detect X-Ray fluorescence from the surface of asteroid. We have made an apparatus to evaluate the CCD with various conditions. We will report about this apparatus and the performance of CCD itself when temperature and driving pulse voltage are varied.
  • Abstracts Fall Meeting of the Japanese Society for Planetary Sciences, 2001 28-28, Oct 6, 2001  
    We are developing an X-Ray fluorescence Spectrometer (XRS) onboard the asteroid probe MUSES-C. Variation of solar X-rays must be considered to analyze major elements quantitatively. XRS observes solar X-rays indirectly using a standard sample. Therefore X-rays from a planetary surface can be calibrated with those from a standard sample in addition to investigation of the spectra and intensities of solar X-rays. We make a model of solar X-ray flux and simulate X-rays observed from a standard sample under various solar conditions. We estimate inversely solar X-rays with calculated emissions and investigate suitable integration times.
  • ARAI T., YAMAMOTO Y., OKADA T., KATO M.
    Abstracts Fall Meeting of the Japanese Society for Planetary Sciences, 2001 84-84, Oct 6, 2001  
    We are developing an X-Ray fluorescence Spectrometer (XRS) onboard the asteroid probe MUSES-C. XRS contains 5 CCD chips. XRS will not carry in-flight calibration sources. Therefore we will observe cosmic X-ray objects for the calibration with XRS during the cruise. We performed numerical simulation of observing some known X-ray objects. Those simulations were run with exposure time about 3 hours, based on the best-fit models to the ASCA SIS spectra.
  • Ito Satomi, Shirai Kei, Okada Tatsuaki, Kato Manabu
    Abstracts Fall Meeting of the Japanese Society for Planetary Sciences, 2001 85-85, Oct 6, 2001  
    We are developing an XRF/XRD instrument for future planetary landing probes. Using this CCD-based device, major elemental and mineral composition is determined through x-ray fluorescence and diffraction method. We have designed and fabricated a miniaturized laboratory model with a two-dimensional CCD. We considered a geometric configuration of the CCD and samples to improve precision of measurement. We investigated a method of onboard data analysis to decrease an amount of telemetry data. We report results of measurements and analyses for XRF and XRD of major minerals.
  • 佐々木 晶, 久保田 孝, 岡田 達明
    宇宙科学シンポジウム, 1 91-98, Jan 11, 2001  
  • 伊藤知美, 白井慶, 岡田達明, 加藤学
    日本惑星科学会秋季講演会予稿集, 2001, 2001  
  • 松田智規, 岡田達明, 加藤学
    太陽系科学シンポジウム, 22nd, 2001  
  • 山本幸生, 岡田達明, 加藤学
    太陽系科学シンポジウム, 22nd, 2001  
  • 岡田達明
    太陽系科学シンポジウム, 22nd, 2001  
  • 増田英二, 岡田達明, 山本幸生, 加藤学
    太陽系科学シンポジウム, 22nd, 2001  
  • 小山 泰弘, 布施 哲治, OSTRO Steven J., CHOATE Dennis, CORMIER Reginald A., WINKLER Ron, JURGENS Raymond F., GIORGINI Jon D., ROSEMA Keith D., MITCHELL David L., YEOMANS Donald K., 中島 潤一, SLADE Martin A., ZAITSEV Alexander L., 関戸 衛, 吉川 真, 中村 昭子, 平林 久, 岡田 達明, 阿部 正直, 西堀 俊幸
    情報通信研究機構研究報告, 47(1) 145-153, 2001  
  • FUJIWARA Akira, MUKAI Tadashi, OKADA Tatsuaki
    Journal of The Society of Instrument and Control Engineers, 39(9) 584-588, Sep 10, 2000  Corresponding author
  • Yamamoto Yukio, Shirai Kei, Okada Tatsuaki, Matsuda Tomoki, Kato Manabu
    Abstracts Fall Meeting of the Japanese Society for Planetary Sciences, 1999 61-61, Nov 13, 1999  
  • Okada T., Shirai K., Yamamoto Y., Matsuda T., Kato M., Tsukahara F., Murao H., Taguchi K.
    Abstracts Fall Meeting of the Japanese Society for Planetary Sciences, 1999 62-62, Nov 13, 1999  
  • 岡田達明
    太陽系科学シンポジウム, 20th, 1999  
  • 山本直孝, 渡部潤一, 岡田達明, 寺田健太郎, 佐々木晶
    日本天文学会年会講演予稿集, 1998, 1998  
  • 岡田達明, 加藤学, 白井慶, 山本幸生, 常深博, 北本俊二
    地球惑星科学関連学会合同大会予稿集, 1998, 1998  
  • 山本幸生, 桑田良隆, 白井慶, 岡田達明, 加藤学
    地球惑星科学関連学会合同大会予稿集, 1998, 1998  
  • 横田康弘, 飯島祐一, 本田理恵, 岡田達明, 水谷仁
    地球惑星科学関連学会合同大会予稿集, 1998, 1998  

Presentations

 522
  • 岡田達明, Hera チーム
    2022 年度プラネタリーディフェンス・シンポジウム, Feb, 2023  Invited
  • 岡田達明, 田中智, 嶌生有理, 坂谷尚哉, 荒井武彦, 千秋博紀, 出村裕英, 関口朋彦, 金丸仁明, 石崎拓也, 神山徹, 和田武彦, 竹内央, 山本幸生, 荒川政彦, 中村昭子, 杉田精司, 宮本英昭, 吉川真, 阿部新助, 安部正真, 池永敏憲, 浦川聖太郎, 菊地翔太, 北里宏平, 小松吾郎, 佐々木晶, 巽瑛理, 津田雄一, 野口高明, 三桝裕也, 薮田ひかる, 渡邊誠一郎, 斎藤啓仁, 金野龍史, 李正林, 古川聡一朗, Hera-JP, TIRIチーム
    第23回宇宙科学シンポジウム, Jan, 2023
  • 坂谷尚哉, 岡田達明, 千秋博紀, 荒井武彦, 出村裕英, 嶌生有理, 関口朋彦, 石崎拓也, 金丸仁明, 神山徹, 田中智
    第23回宇宙科学シンポジウム, Jan, 2023
  • 嶌生有理, 黒川宏之, 坂谷尚哉, 深井稜汰, 癸生川陽子, 青木順, 巽瑛理, 田中智, 渡邊誠一郎, 岡田達明, 浦川聖太郎, 脇田茂, 薮田ひかる, 兵頭龍樹, 藤谷渉, 牛久保孝行, 奥住聡
    第23回宇宙科学シンポジウム, Jan, 2023
  • 吉川真, 柳沢俊史, 安部正真, 池永敏憲, 岩城陽大, 岡田達明, 菊地耕一, 黒崎裕久, 黒田信介, 佐伯孝尚, 嶌生有理, 津田雄一, 西山和孝, 三桝裕也, 浦川聖太郎, 奥村真一郎
    第23回宇宙科学シンポジウム, Jan, 2023
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Teaching Experience

 2

Professional Memberships

 5

Research Projects

 6
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● 専任大学名

 1
  • Affiliation (university)
    東京大学（University of Tokyo)

● 所属する所内委員会

 1
  • ISAS Committee
    放射線安全委員会
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