研究者業績
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 宇宙物理学研究系 教授総合研究大学院大学 先端学術院 宇宙科学コース 教授東京科学大学 理学院物理学系物理学コース 特定教授関西学院大学 大学院理工学研究科 客員教授
- 学位
- 理学博士(東京大学)
- J-GLOBAL ID
- 200901025041369206
- researchmap会員ID
- 1000144439
専門はＸ線天文学。特に、中性子星やブラックホールを含むX線連星の観測的研究および衛星搭載X線CCDカメラの開発研究。
受賞
1-
1996年
論文
252-
The Astrophysical Journal 1003(2) 156-156 2026年5月22日Abstract The supermassive binary system, η Carinae, is experiencing enormous wind-driven mass loss at a rate unparalleled in the rest of the Galaxy. Their wind–wind collision (WWC) continuously produces shock heated, X-ray-emitting plasmas. The XRISM X-ray observatory observed the system in 2023 and 2024 when the X-ray emission began to increase toward periastron passage in 2025. This paper reports unprecedentedly high-resolution X-ray spectra in the Fe K α band between 6.2 and 7.1 keV, obtained with the Resolve X-ray microcalorimeter. The hydrogen-like (Ly α ) and helium-like (He α ) lines reveal three velocity components. Two of them are broadened with maximum velocities of 2000–3000 km s −1 , likely originating from the postshock companion wind. The other is relatively narrow, with a Gaussian broadening of only ∼290 km s −1 in 1 σ , which may originate from the postshock companion wind at the WWC stagnation point or penetrating the primary wind. The Fe fluorescent lines exhibit a moderate blueshift and broadening with velocities at 100–200 km s −1 , consistent with the primary wind’s velocity field. The spectra also confirm a Compton shoulder of the He α line complex for the first time. Both fluorescing and scattering spectral profiles indicate that the binary system is seen from the companion side during these observations. The flux ratio of the Compton-scattering emission to the fluorescent line suggests substantial hydrogen depletion of the primary wind, expected from CNO-cycled hydrogen nuclear fusion gas.
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Publications of the Astronomical Society of Japan 2026年4月9日Abstract We report the presence of a highly ionized absorber in the transient, eclipsing low-mass X-ray binary AX J1745.6-2901, observed from 2024 February 26–29 with XRISM’s Resolve and Xtend instruments. During a soft/high state without dips, Resolve’s high spectral resolution ($E/\Delta E \sim 1000$, full width at half-maximum) revealed narrow velocity widths ($\sigma \sim 110~{\rm km~s^{-1 } }$) for Fe xxvi and Ni xxviii lines, even with low photon statistics. These widths are consistent with binary orbital motion. The observed modest blueshift velocity (${\sim }160~{\rm km~s^{-1 } }$) indicates that the absorber is located sufficiently far from the neutron star (${>}10^9$ cm), so that gravitational redshift effects are not dominant. On the other hand, broad-band spectral analysis using a photoionized plasma model applied to the Xtend data constrains the absorber to lie within a radius of ${\lesssim }10^{9.5}$ cm, as inferred from the upper limits of the best-fitting ionization parameter ($\log \xi \sim 4.4$) and the large column density (${\sim }1.6\times 10^{24}~{\rm cm^{-2 } }$). At this distance, the observed outward velocity of the absorber is about an order of magnitude smaller than the escape velocity from the neutron star.
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Astronomy & Astrophysics 708 A130-A130 2026年4月1日Context. The origin of accretion-disc winds remains disputed. High-inclination, dipping, neutron-star (NS) low-mass X-ray binaries (LMXBs) provide an excellent testbed for studying the launching mechanism of such winds due to them persistently accreting and showing a nearly ubiquitous presence of highly ionised plasmas. Aims. We aim to establish or rule out the presence of a wind in the high-inclination LMXB 4U 1624−49, for which a highly ionised plasma has been repeatedly observed in X-ray spectra by Chandra and XMM-Newton, and a thermal–radiative pressure wind is expected. Methods. We leveraged the exquisite spectral resolution of the X-ray Imaging and Spectroscopy Mission (XRISM) to perform phase-resolved spectroscopy of the full binary orbit to characterise the highly ionised plasma at all phases except during absorption dips. Results. An outflow is clearly detected via phase-resolved spectroscopy of the source with XRISM Resolve. Based on analysis of the radial-velocity curve, we determine an average velocity of ∼200−320 km s −1 and a column density above 10 23 cm −2 . The line profiles are generally narrow, spanning ∼50−100 km s −1 , depending on the orbital phase; this points to a low-velocity sheer or turbulence of the highly ionised outflow and a potential increase of turbulence as the absorption dip is approached, likely due to turbulent mixing. Conclusions. The line profiles, together with the derived launching radius and wind velocity, are consistent with a wind being launched from the outskirts of the disc and without stratification, pointing to a thermal-radiative pressure origin.
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Nature Astronomy 2026年3月31日
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Nature 651(8107) 909-913 2026年3月25日
MISC
207-
Publications of the Astronomical Society of Japan 70(2) 2018年3月1日
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J. Astron. Telesc. Instrum. Syst. 4(1), 011211 (2018) 4(1) 2018年1月22日
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Proceedings of SPIE - The International Society for Optical Engineering 10699 2018年1月1日
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70(2) 2017年7月1日The Crab nebula originated from a core-collapse supernova (SN) explosion<br /> observed in 1054 A.D. When viewed as a supernova remnant (SNR), it has an<br /> anomalously low observed ejecta mass and kinetic energy for an Fe-core collapse<br /> SN. Intensive searches were made for a massive shell that solves this<br /> discrepancy, but none has been detected. An alternative idea is that the SN1054<br /> is an electron-capture (EC) explosion with a lower explosion energy by an order<br /> of magnitude than Fe-core collapse SNe. In the X-rays, imaging searches were<br /> performed for the plasma emission from the shell in the Crab outskirts to set a<br /> stringent upper limit to the X-ray emitting mass. However, the extreme<br /> brightness of the source hampers access to its vicinity. We thus employed<br /> spectroscopic technique using the X-ray micro-calorimeter onboard the Hitomi<br /> satellite. By exploiting its superb energy resolution, we set an upper limit<br /> for emission or absorption features from yet undetected thermal plasma in the<br /> 2-12 keV range. We also re-evaluated the existing Chandra and XMM-Newton data.<br /> By assembling these results, a new upper limit was obtained for the X-ray<br /> plasma mass of <~ 1Mo for a wide range of assumed shell radius, size, and<br /> plasma temperature both in and out of the collisional equilibrium. To compare<br /> with the observation, we further performed hydrodynamic simulations of the Crab<br /> SNR for two SN models (Fe-core versus EC) under two SN environments (uniform<br /> ISM versus progenitor wind). We found that the observed mass limit can be<br /> compatible with both SN models if the SN environment has a low density of <~<br /> 0.03 cm-3 (Fe core) or <~ 0.1 cm-3 (EC) for the uniform density, or a<br /> progenitor wind density somewhat less than that provided by a mass loss rate of<br /> 10-5 Mo yr-1 at 20 km s-1 for the wind environment.
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ASTROPHYSICAL JOURNAL LETTERS 837(1) 2017年3月
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SPACE TELESCOPES AND INSTRUMENTATION 2016: OPTICAL, INFRARED, AND MILLIMETER WAVE 9904 2016年 査読有り
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日本物理学会講演概要集 69(2) 37-37 2014年8月22日
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日本物理学会講演概要集 69(1) 129-129 2014年3月5日
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日本物理学会講演概要集 68(1) 134-134 2013年3月26日
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PASJ : publications of the Astronomical Society of Japan 64(5) "112-1"-"112-11" 2012年10月25日
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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 112(229) 17-22 2012年10月3日Japan Aerospace Exploration Agency (JAXA) has been developing an X-ray astronomy satellite named "ASTRO-H", which will be launched in 2014. This paper provides a summary of the design overview and development status of an electrical power subsystem for ASTRO-H. The subsystem consists of rigid solar array paddles that generate approximately 3500W at the end of life of the system, a power control unit that delivers an unregulated 50V bus power supply, shunt dissipators, battery charge control units, two 100-Ah Li-ion batteries, and a non-explosive actuator controller. Currently, manufacturing and verification tests for the satellite system have been implemented for the launch.
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日本物理学会講演概要集 67(2) 119-119 2012年8月24日
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日本物理学会講演概要集 67(2) 119-119 2012年8月24日
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Astrophysical Journal 753(2) 2012年7月10日
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PASJ : publications of the Astronomical Society of Japan 64(3) "53-1"-"53-12" 2012年6月25日
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日本物理学会講演概要集 67(1) 139-139 2012年3月5日
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SUZAKU 2011: Exploring the X-ray Universe: Suzaku and Beyond. AIP Conference Proceedings 1427 247-248 2012年3月
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SUZAKU 2011: EXPLORING THE X-RAY UNIVERSE: SUZAKU AND BEYOND 1427 253-254 2012年 査読有り
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日本物理学会講演概要集 66(2) 112-112 2011年8月24日
所属学協会
4-
2000年1月 - 現在
共同研究・競争的資金等の研究課題
15-
日本学術振興会 科学研究費助成事業 基盤研究(C) 2019年4月 - 2023年3月
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日本学術振興会 科学研究費助成事業 新学術領域研究(研究領域提案型) 2012年6月 - 2017年3月
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日本学術振興会 科学研究費助成事業 2012年4月 - 2015年3月
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日本学術振興会 科学研究費助成事業 基盤研究(B) 2010年4月 - 2013年3月
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日本学術振興会 科学研究費助成事業 特別研究員奨励費 2005年 - 2007年
● 指導学生等の数
1-
年度2021年度(FY2021)修士課程学生数2連携大学院制度による学生数2学術特別研究員数1
● 専任大学名
1-
専任大学名総合研究大学院大学（SOKENDAI)
