Curriculum Vitaes
Profile Information
- Affiliation
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency
- Degree
- 理学博士(中央大学)理学修士(中央大学)
- J-GLOBAL ID
- 201201017168289883
- researchmap Member ID
- 7000000018
Research Interests
2Research Areas
2Education
4-
- 2011
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- 2008
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- 2002
Committee Memberships
1-
2012
Papers
27-
Monthly Notices of the Royal Astronomical Society, 484(2) 2229-2233, Apr, 2019 Peer-reviewed
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 70(6), Oct 1, 2018
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Astrophysical Journal, Supplement Series, 238(2), Oct, 2018
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PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 70(3), Jun, 2018 Peer-reviewed
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Journal of Astronomical Telescopes, Instruments, and Systems, 4(2), Apr, 2018 Peer-reviewed
Misc.
16-
Proceedings of Science, Jan 1, 2017
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Nov 4, 2015Colliding Wolf-Rayet (WR) winds produce thermal X-ray emission widely<br /> observed by X-ray telescopes. In wide WR+O binaries, such as WR 140, the X-ray<br /> flux is tied to the orbital phase, and is a direct probe of the winds'<br /> properties. In the Galactic center, $\sim$30 WRs orbit the super massive black<br /> hole (SMBH) within $\sim$10", leading to a smorgasbord of wind-wind collisions.<br /> To model the X-ray emission of WR 140 and the Galactic center, we perform 3D<br /> hydrodynamic simulations to trace the complex gaseous flows, and then carry out<br /> 3D radiative transfer calculations to compute the variable X-ray spectra. The<br /> model WR 140 RXTE light curve matches the data well for all phases except the<br /> X-ray minimum associated with periastron, while the model spectra agree with<br /> the RXTE hardness ratio and the shape of the Suzaku observations throughout the<br /> orbit. The Galactic center model of the Chandra flux and spectral shape match<br /> well in the region r$<$3", but the model flux falls off too rapidly beyond this<br /> radius.
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Suzaku-MAXI 2014: Expanding the Frontiers of the X-ray Universe, pp.pp220-221, Sep, 2014
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Suzaku-MAXI 2014: Expanding the Frontiers of the X-ray Universe, pp.pp208-209, Sep, 2014
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Suzaku-MAXI 2014: Expanding the Frontiers of the X-ray Universe, pp.pp164-165, Sep, 2014
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May 20, 2014Colliding wind binaries (CWBs) are unique laboratories for X-ray<br /> astrophysics. The massive stars in these systems possess powerful stellar winds<br /> with speeds up to $\sim$3000 km s$^{-1}$, and their collision leads to hot<br /> plasma (up to $\sim10^8$K) that emit thermal X-rays (up to $\sim$10 keV). Many<br /> X-ray telescopes have observed CWBs, including Suzaku, and our work aims to<br /> model these X-ray observations. We use 3D smoothed particle hydrodynamics (SPH)<br /> to model the wind-wind interaction, and then perform 3D radiative transfer to<br /> compute the emergent X-ray flux, which is folded through X-ray telescopes'<br /> response functions to compare directly with observations. In these proceedings,<br /> we present our models of Suzaku observations of the multi-year-period, highly<br /> eccentric systems $\eta$ Carinae and WR 140. The models reproduce the<br /> observations well away from periastron passage, but only $\eta$ Carinae's X-ray<br /> spectrum is reproduced at periastron; the WR 140 model produces too much flux<br /> during this more complicated phase.
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Proceedings of SPIE - The International Society for Optical Engineering, 9144, 2014
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Space Telescopes and Instrumentation 2012: Ultraviolet to Gamma Ray. Proceedings of the SPIE, 8443, Sep, 2012
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SUZAKU 2011: EXPLORING THE X-RAY UNIVERSE: SUZAKU AND BEYOND, 1427 296-297, 2012
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DEATH OF MASSIVE STARS: SUPERNOVAE AND GAMMA-RAY BURSTS, 279(279) 351-352, 2012
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Proceedings of the International Astronomical Union, 10(16) 51-79, 2012
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Proceedings of SPIE - The International Society for Optical Engineering, 8443, 2012
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JAXA Special Publication: The Energetic Cosmos: from Suzaku to ASTRO-H, 198-199, Jan, 2010
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Active OB-Stars: Laboratories for Stellar and Circumstellar Physics, 361 500-502, Mar, 2007
Presentations
68Professional Memberships
3Works
1Research Projects
3-
科学研究費補助金 若手研究(B), Apr, 2016 - Mar, 2019
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科学研究費補助金 特別研究促進費, Apr, 2009 - Mar, 2011
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2005