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Hiroya Yamaguchi

  (山口 弘悦)

Profile Information

Affiliation
Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency
Degree
博士(理学)(Mar, 2008, 京都大学)
Researcher number
00513467
J-GLOBAL ID
201801007525282778
researchmap Member ID
B000340695
External link

主な研究テーマ・プロジェクト業務

Ia型超新星、原子過程/Ｘ線分光学、将来計画の成果最大化

下記の業績リストは不完全です。「論文」は主要論文のみ、「講演・口頭発表等」は最近の招待講演のみリストしています。

 

座右の銘

努力して運を待て（仁科芳雄） 努力を続けていれば運が向いた時に見逃さないって意味だと思う。運は誰にでも同じ頻度で巡ってくる。それに気づき活かせるかは本人の努力次第。

疑行無名、疑事無功（『戦国策』） 後から迷走しないように達成目標と実施計画を明確にすべしって意味だと思う。目的意識もなく仕事に取り掛かるから、行き当たりばったりになり良い成果が挙がらない。

人、城を頼らば、城、人を捨せん（織田信長） プロジェクトがあれば何とかなると考えていたらプロジェクトが頓挫したときに自力で起き上がれないって意味だと思う。この懸念は2016年に現実のものとなった。 

Research Interests

 5

Research Areas

 2

Research History

 8
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Education

 3

Committee Memberships

 6
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Awards

 9
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Papers

 44
  • Tomoya Kinugawa, Hiroki Takeda, Ataru Tanikawa, Hiroya Yamaguchi
    The Astrophysical Journal, 938(1) 52-52, Oct 1, 2022  
    Abstract It is generally believed that Type Ia supernovae are thermonuclear explosions of carbon–oxygen white dwarfs (WDs). However, there is currently no consensus regarding the events leading to the explosion. A binary WD (WD–WD) merger is a possible progenitor of Type Ia supernovae. Space-based gravitational wave (GW) detectors with considerable sensitivity in the decihertz range such as the DECi-hertz Interferometer Gravitational wave Observatory (DECIGO) can observe WD–WD mergers directly. Therefore, access to the decihertz band of GWs would enable multi-messenger observations of Type Ia supernovae to determine their progenitors and explosion mechanism. In this paper, we consider the event rate of WD–WD mergers and the minimum detection range to observe one WD–WD merger per year, using a nearby galaxy catalog and the relation between Ia supernovae and their host galaxies. Furthermore, we calculate DECIGO’s ability to localize WD–WD mergers and to determine the masses of binary mergers. We estimate that a decihertz GW observatory can detect GWs with amplitudes of h ∼ 10−20 [Hz−1/2] at 0.01–0.1 Hz, which is 1000 times higher than the detection limit of DECIGO. Assuming the progenitors of Ia supernovae are merging WD–WD (1 M⊙ and 0.8 M⊙), DECIGO is expected to detect 6600 WD–WD mergers within z = 0.08, and identify the host galaxies of such WD–WD mergers within z ∼ 0.065 using GW detections alone.
  • H. Sano, H. Yamaguchi, M. Aruga, Y. Fukui, K. Tachihara, M. D. Filipović, G. Rowell
    The Astrophysical Journal, 933(2) 157-157, Jul 1, 2022  
    Abstract We report new H i observations of the Type Ia supernova remnant (SNR) SN 1006 using the Australia Telescope Compact Array with an angular resolution of $4\buildrel{\,\prime}\over{.} 5\times 1\buildrel{\,\prime}\over{.} 4$ (∼2 pc at the assumed SNR distance of 2.2 kpc). We find an expanding gas motion in position–velocity diagrams of H i with an expansion velocity of ∼4 km s−1 and a mass of ∼1000 M⊙. The spatial extent of the expanding shell is roughly the same as that of SN 1006. We here propose a hypothesis that SN 1006 exploded inside the wind-blown bubble formed by accretion winds from the progenitor system consisting of a white dwarf and a companion star, and then the forward shock has already reached the wind wall. This scenario is consistent with the single-degenerate model. We also derived the total energy of cosmic-ray protons Wp to be only ∼1.2–2.0 × 1047 erg by adopting the averaged interstellar proton density of ∼25 cm−3. The small value is compatible with the relation between the age and Wp of other gamma-ray SNRs with ages below ∼6 kyr. The Wp value in SN 1006 will possibly increase up to several 1049 erg in the next ∼5 kyr via the cosmic-ray diffusion into the H i wind shell.
  • Wataru B Iwakiri, Motoko Serino, Tatehiro Mihara, Liyi Gu, Hiroya Yamaguchi, Megumi Shidatsu, Kazuo Makishima
    Publications of the Astronomical Society of Japan, 73(5) 1405-1417, Oct 4, 2021  Peer-reviewed
    Abstract We discover an unidentified strong emission feature in the X-ray spectrum of EXO 1745−248 obtained by RXTE at 40 hr after the peak of a superburst. The structure was centered at 6.6 keV and significantly broadened with a large equivalent width of 4.3 keV, corresponding to a line photon flux of 4.7 × 10−3 ph cm−2 s−1. The 3–20 keV spectrum was reproduced successfully by a power-law continuum with narrow and broad (2.7 keV in full width at half maximum) Gaussian emission components. Alternatively, the feature can be described by four narrow Gaussians, centered at 5.5 keV, 6.5 keV, 7.5 keV, and 8.6 keV. Considering the strength and shape of the feature, it is unlikely to have originated from reflection of the continuum X-rays by some optically thick material, such as an accretion disk. Moreover, the intensity of the emission structure decreased significantly with an exponential time scale of 1 hr. The feature was not detected in an INTEGRAL observation performed 10 hr before the RXTE observation with a line flux upper limit of 1.5 × 10−3 ph cm−2 s−1. The observed emission structure is consistent with gravitationally redshifted charge exchange emission from Ti, Cr, Fe, and Co. We suggest that the emission results from a charge exchange interaction between a highly metal-enriched fall-back ionized burst wind and an accretion disk, at a distance of ∼60 km from the neutron star. If this interpretation is correct, the results provide new information on nuclear burning processes during thermonuclear X-ray bursts.
  • Yuken Ohshiro, Hiroya Yamaguchi, Shing-Chi Leung, Ken’ichi Nomoto, Toshiki Sato, Takaaki Tanaka, Hiromichi Okon, Robert Fisher, Robert Petre, Brian J. Williams
    The Astrophysical Journal Letters, 913(2) L34-L34, Jun 1, 2021  Peer-reviewed
    Abstract The supernova remnant (SNR) 3C 397 is thought to originate from a Type Ia supernova (SN Ia) explosion of a near-Chandrasekhar-mass (MCh) progenitor, based on the enhanced abundances of Mn and Ni revealed by previous X-ray study with Suzaku. Here we report follow-up XMM-Newton observations of this SNR, conducted with the aim of investigating the detailed spatial distribution of the Fe-peak elements. We have discovered an ejecta clump with extremely high abundances of Ti and Cr, in addition to Mn, Fe, and Ni, in the southern part of the SNR. The Fe mass of this ejecta clump is estimated to be ∼0.06 M⊙, under the assumption of a typical Fe yield for SNe Ia (i.e., ∼0.8 M⊙). The observed mass ratios among the Fe-peak elements and Ti require substantial neutronization that is achieved only in the innermost regions of a near-MCh SN Ia with a central density of ρc ∼ 5 × 109 g cm−3, significantly higher than typically assumed for standard near-MCh SNe Ia (ρc ∼ 2 × 109 g cm−3). The overproduction of the neutron-rich isotopes (e.g., 50Ti and 54Cr) is significant in such high-ρc SNe Ia, with respect to the solar composition. Therefore, if 3C 397 is a typical high-ρc near-MCh SN Ia remnant, the solar abundances of these isotopes could be reproduced by the mixture of the high- and low-ρc near-MCh and sub-MCh Type Ia events, with ≲20% being high-ρc near-MCh.
  • Hiroya Yamaguchi, Fabio Acero, Chuan-Jui Li, You-Hua Chu
    The Astrophysical Journal Letters, 910(2) L24-L24, Apr 1, 2021  Peer-reviewedLead author
    Abstract The geometric structure of supernova remnants (SNR) provides a clue to unveiling the pre-explosion evolution of their progenitors. Here we present an X-ray study of N103B (0509–68.7), a Type Ia SNR in the Large Magellanic Cloud, that is known to be interacting with dense circumstellar matter (CSM). Applying our novel method for feature extraction to deep Chandra observations, we have successfully resolved the CSM, Fe-rich ejecta, and intermediate-mass element (IME) ejecta components, and revealed each of their spatial distributions. Remarkably, the IME ejecta component exhibits a double-ring structure, implying that the SNR expands into an hourglass-shape cavity and thus forms bipolar bubbles of the ejecta. This interpretation is supported by more quantitative spectroscopy that reveals a clear bimodality in the distribution of the ionization state of the IME ejecta. These observational results can be naturally explained if the progenitor binary system had formed a dense CSM torus on the orbital plane prior to the explosion, providing further evidence that the SNR N103B originates from a single-degenerate progenitor.
  • Tanaka, Takaaki, Okuno, Tomoyuki, Uchida, Hiroyuki, Yamaguchi, Hiroya, Lee, Shiu-Hang, Maeda, Keiichi, Williams, Brian J
    The Astrophysical Journal Letters, 906 L3, Jan, 2021  Peer-reviewed
  • Suzuki Hitomi, Yamaguchi Hiroya, Ishida Manabu, Uchida Hiroyuki, Plucinsky Paul P, Foster Adam R, Miller Eric D
    The Astrophysical Journal (in press), Jul, 2020  Peer-reviewed
  • Fukushima, Kotaro, Yamaguchi, Hiroya, Slane, Patrick O., Park, Sangwook, Katsuda, Satoru, Sano, Hidetoshi, Lopez, Laura A., Plucinsky, Paul P., Kobayashi, Shogo B., Matsushita, Kyoko
    The Astrophysical Journal, 897(1) 62, Jul, 2020  Peer-reviewed
  • Okon, Hiromichi, Tanaka, Takaaki, Uchida, Hiroyuki, Yamaguchi, Hiroya, Tsuru, Takeshi Go, Seta, Masumichi, Smith, Randall K., Yoshiike, Satoshi, Orlando, Salvatore, Bocchino, Fabrizio, Miceli, Marco
    The Astrophysical Journal, 890(1) 62, Feb, 2020  Peer-reviewed
  • Hiroya Yamaguchi
    Astronomische Nachrichten, 341(2) 150-155, Feb, 2020  Peer-reviewedInvitedLead author
  • Simionescu, A, Nakashima, S, Yamaguchi, H, Matsushita, K, Mernier, F, Werner, N, Tamura, T, Nomoto, K, de Plaa, J, Bamba, A, Bulbul, E, Ezoe, Y, Fabian, A. C, Fukazawa, Y, Gu, L, Ichinohe, Y, Ishigaki, M. N, Kaastra, J. S, Kilbourne, C, Kitayama, T, Leung, S.-C, Leutenegger, M, Loewenstein, M, Maeda, Y, Miller, E. D, Mushotzky, R. F, Noda, H, Pinto, C, Porter, F. S, Safi-Harb, S, Sato, K, Takahashi, T, Ueda, S, Zha, S
    Monthly Notices of the Royal Astronomical Society, 483(2) 1701-1721, Feb, 2019  Peer-reviewed
  • Mernier, F, Biffi, V, Yamaguchi, H, Medvedev, P, Simionescu, A, Ettori, S, Werner, N, Kaastra, J. S, de Plaa, J, Gu, L
    Space Science Reviews, 214(8) 129, Dec, 2018  Peer-reviewedInvited
  • Yamaguchi, Hiroya, Tanaka, Takaaki, Wik, Daniel R, Rho, Jeonghee, Bamba, Aya, Castro, Daniel, Smith, Randall K, Foster, Adam R, Uchida, Hiroyuki, Petre, Robert, Williams, Brian J
    The Astrophysical Journal Letters, 868 L35, Dec, 2018  Peer-reviewedLead author
  • Sano, H, Yamane, Y, Tokuda, K, Fujii, K, Tsuge, K, Nagaya, T, Yoshiike, S, Filipović, M. D, Alsaberi, R. Z. E, Barnes, L, Onishi, T, Kawamura, A, Minamidani, T, Mizuno, N, Yamamoto, H, Tachihara, K, Maxted, N, Voisin, F, Rowell, G, Yamaguchi, H, Fukui, Y
    The Astrophysical Journal, 867(1) 7, Nov, 2018  Peer-reviewed
  • Martínez-Rodríguez, Héctor, Badenes, Carles, Lee, Shiu-Hang, Patnaude, Daniel J, Foster, Adam R, Yamaguchi, Hiroya, Auchettl, Katie, Bravo, Eduardo, Slane, Patrick O, Piro, Anthony L, Park, Sangwook, Nagataki, Shigehiro
    The Astrophysical Journal, 865(2) 151, Oct, 2018  Peer-reviewed
  • Tanaka, Takaaki, Yamaguchi, Hiroya, Wik, Daniel R, Aharonian, Felix A, Bamba, Aya, Castro, Daniel, Foster, Adam R, Petre, Robert, Rho, Jeonghee, Smith, Randall K, Uchida, Hiroyuki, Uchiyama, Yasunobu, Williams, Brian J
    The Astrophysical Journal Letters, 866(2) L26, Oct, 2018  Peer-reviewed
  • Kasuga, Tomoaki, Sato, Toshiki, Mori, Koji, Yamaguchi, Hiroya, Bamba, Aya
    Publications of the Astronomical Society of Japan, 70(5) 88, Oct, 2018  Peer-reviewed
  • Gu, Liyi, Zhuravleva, Irina, Churazov, Eugene, Paerels, Frits, Kaastra, Jelle, Yamaguchi, Hiroya
    Space Science Reviews, 214(7) 108, Oct, 2018  Peer-reviewedInvited
  • Hitomi Collaboration, Corresponding authors: Miller, Eric D, Yamaguchi, Hiroya
    Publications of the Astronomical Society of Japan, 70(2) 16, Mar, 2018  Peer-reviewedCorresponding author
  • Felix Aharonian, Hiroki Akamatsu, Fumie Akimoto, Steven W. Allen, Lorella Angelini, Marc Audard, Hisamitsu Awaki, Magnus Axelsson, Aya Bamba, Marshall W. Bautz, Roger Blandford, Laura W. Brenneman, Gregory V. Brown, Esra Bulbul, Edward M. Cackett, Maria Chernyakova, Meng P. Chiao, Paolo S. Coppi, Elisa Costantini, Jelle De Plaa, Jan-Willem den Herder, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Teruaki Enoto, Yuichiro Ezoe, Andrew C. Fabian, Carlo Ferrigno, Adam R. Foster, Ryuichi Fujimoto, Yasushi Fukazawa, Akihiro Furuzawa, Massimiliano Galeazzi, Luigi C. Gallo, Poshak Gandhi, Margherita Giustini, Andrea Goldwurm, Liyi Gu, Matteo Guainazzi, Yoshito Haba, Kouichi Hagino, Kenji Hamaguchi, Ilana M. Harrus, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Kiyoshi Hayashida, Junko S. Hiraga, Ann Hornschemeier, Akio Hoshino, John P. Hughes, Yuto Ichinohe, Ryo Iizuka, Hajime Inoue, Yoshiyuki Inoue, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Masachika Iwai, Jelle Kaastra, Tim Kallman, Tsuneyoshi Kamae, Jun Kataoka, Satoru Katsuda, Nobuyuki Kawai, Richard L. Kelley, Caroline A. Kilbourne, Takao Kitaguchi, Shunji Kitamoto, Tetsu Kitayama, Takayoshi Kohmura, Motohide Kokubun, Katsuji Koyama, Shu Koyama, Peter Kretschmar, Hans A. Krimm, Aya Kubota, Hideyo Kunieda, Philippe Laurent, Shiu-Hang Lee, Maurice A. Leutenegger, Olivier Limousine, Michael Loewenstein, Knox S. Long, David Lumb, Greg Madejski, Yoshitomo Maeda, Daniel Maier, Kazuo Makishima, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian R. McNamara, Missagh Mehdipour, Eric D. Miller, Jon M. Miller, Shin Mineshige, Kazuhisa Mitsuda, Ikuyuki Mitsuishi, Takuya Miyazawa, Tsunefumi Mizuno, Hideyuki Mori, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard F. Mushotzky, Takao Nakagawa, Hiroshi Nakajima, Takeshi Nakamori, Shinya Nakashima, Kazuhiro Nakazawa, Kumiko K. Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Takaya Ohashi, Masanori Ohno, Takashi Okajima, Naomi Ota, Masanobu Ozaki, Frits Paerels, StPhane Paltani, Robert Petre, Ciro Pinto, Frederick S. Porter, Katja Pottschmidt, Christopher S. Reynolds, Samar Safi-Harb, Shinya Saito, Kazuhiro Sakai, Toru Sasaki, Goro Sato, Kosuke Sato, Rie Sato, Makoto Sawada, Norbert Schartel, Peter J. Serlemitsos, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall K. Smith, Yang Soong, Lukasz Stawarz, Yasuharu Sugawara, Satoshi Sugita, Andrew Szymkowiak, Hiroyasu Tajima, Hiromitsu Takahashi, Tadayuki Takahashi, Shin'ichiro Takeda, Yoh Takei, Toru Tamagawa, Takayuki Tamura, Takaaki Tanaka, Yasuo Tanaka, Yasuyuki T. Tanaka, Makoto S. Tashiro, Yuzuru Tawara, Yukikatsu Terada, Yuichi Terashima, Francesco Tombesi, Hiroshi Tomida, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Go Tsuru, Hiroyuki Uchida, Hideki Uchiyama, Yasunobu Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shin'ichiro Uno, C. Megan Urry, Eugenio Ursino, Cor P. de Vries, Shin Watanabe, Norbert Werner, Daniel R. Wik, Dan R. Wilkins, Brian J. Williams, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Y. Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Yoichi Yatsu, Daisuke Yonetoku, Irina Zhuravleva, Abderahmen Zoghbi
    NATURE, 551(7681) 478-+, Nov, 2017  Peer-reviewedCorresponding author
    The metal abundance of the hot plasma that permeates galaxy clusters represents the accumulation of heavy elements produced by billions of supernovae(1). Therefore, X-ray spectroscopy of the intracluster medium provides an opportunity to investigate the nature of supernova explosions integrated over cosmic time. In particular, the abundance of the iron-peak elements (chromium, manganese, iron and nickel) is key to understanding how the progenitors of typical type Ia supernovae evolve and explode(2-6). Recent X-ray studies of the intracluster medium found that the abundance ratios of these elements differ substantially from those seen in the Sun(7-11), suggesting differences between the nature of type Ia supernovae in the clusters and in the Milky Way. However, because the K-shell transition lines of chromium and manganese are weak and those of iron and nickel are very close in photon energy, highresolution spectroscopy is required for an accurate determination of the abundances of these elements. Here we report observations of the Perseus cluster, with statistically significant detections of the resonance emission from chromium, manganese and nickel. Our measurements, combined with the latest atomic models, reveal that these elements have near-solar abundance ratios with respect to iron, in contrast to previous claims. Comparison between our results and modern nucleosynthesis calculations(12-14) disfavours the hypothesis that type Ia supernova progenitors are exclusively white dwarfs with masses well below the Chandrasekhar limit (about 1.4 times the mass of the Sun). The observed abundance pattern of the iron-peak elements can be explained by taking into account a combination of near-and sub-Chandrasekhar-mass type Ia supernova systems, adding to the mounting evidence that both progenitor types make a substantial contribution to cosmic chemical enrichment(5,15,16).
  • Slavin, Jonathan D, Smith, Randall K, Foster, Adam, Winter, Henry D, Raymond, John C, Slane, Patrick O, Yamaguchi, Hiroya
    The Astrophysical Journal, 846(1) 77, Sep, 2017  Peer-reviewed
  • Martínez-Rodríguez, Héctor, Badenes, Carles, Yamaguchi, Hiroya, Bravo, Eduardo, Timmes, F. X, Miles, Broxton J, Townsley, Dean M, Piro, Anthony L, Mori, Hideyuki, Andrews, Brett, Park, Sangwook
    The Astrophysical Journal, 843(1) 35, Jul, 2017  Peer-reviewed
  • Williams, Brian J, Coyle, Nina M, Yamaguchi, Hiroya, Depasquale, Joseph, Seitenzahl, Ivo R, Hewitt, John W, Blondin, John M, Borkowski, Kazimierz J, Ghavamian, Parviz, Petre, Robert, Reynolds, Stephen P
    The Astrophysical Journal, 842(1) 28, Jun, 2017  Peer-reviewed
  • Yamaguchi, Hiroya, Hughes, John P, Badenes, Carles, Bravo, Eduardo, Seitenzahl, Ivo R, Martínez-Rodríguez, Héctor, Park, Sangwook, Petre, Robert
    The Astrophysical Journal, 834(2) 124, Jan, 2017  Peer-reviewed
  • Hitomi Collaboration, Corresponding author, Fabian, Andrew
    Nature, 535(7610) 117, Jul, 2016  Peer-reviewed
  • Yamaguchi, Hiroya, Katsuda, Satoru, Castro, Daniel, Williams, Brian J, Lopez, Laura A, Slane, Patrick O, Smith, Randall K, Petre, Robert
    The Astrophysical Journal Letters, 820(1) L3, Mar, 2016  Peer-reviewed
  • Uchida, Hiroyuki, Koyama, Katsuji, Yamaguchi, Hiroya
    The Astrophysical Journal, 808(1) 77, Jul, 2015  Peer-reviewed
  • Takei, D, Drake, J. J, Yamaguchi, H, Slane, P, Uchiyama, Y, Katsuda, S
    The Astrophysical Journal, 801(2) 92, Mar, 2015  Peer-reviewed
  • Yamaguchi, Hiroya, Badenes, Carles, Foster, Adam R, Bravo, Eduardo, Williams, Brian J, Maeda, Keiichi, Nobukawa, Masayoshi, Eriksen, Kristoffer A, Brickhouse, Nancy S, Petre, Robert, Koyama, Katsuji
    The Astrophysical Journal Letters, 801(2) L31, Mar, 2015  Peer-reviewed
  • Hiroya Yamaguchi, Carles Badenes, Robert Petre, Toshio Nakano, Daniel Castro, Teruaki Enoto, Junko S. Hiraga, John P. Hughes, Yoshitomo Maeda, Masayoshi Nobukawa, Samar Safi-Harb, Patrick O. Slane, Randall K. Smith, Hiroyuki Uchida
    ASTROPHYSICAL JOURNAL LETTERS, 785(2) L27, Apr, 2014  Peer-reviewed
    Supernova remnants (SNRs) retain crucial information about both their parent explosion and circumstellar material left behind by their progenitor. However, the complexity of the interaction between supernova ejecta and ambient medium often blurs this information, and it is not uncommon for the basic progenitor type (Ia or core-collapse) of well-studied remnants to remain uncertain. Here we present a powerful new observational diagnostic to discriminate between progenitor types and constrain the ambient medium density of SNRs using solely Fe K-shell X-ray emission. We analyze all extant Suzaku observations of SNRs and detect Fe K alpha emission from 23 young or middle-aged remnants, including five first detections (IC 443, G292.0+ 1.8, G337.2-0.7, N49, and N63A). The Fe Ka centroids clearly separate progenitor types, with the Fe-rich ejecta in Type Ia remnants being significantly less ionized than in core-collapse SNRs. Within each progenitor group, the Fe Ka luminosity and centroid are well correlated, with more luminous objects having more highly ionized Fe. Our results indicate that there is a strong connection between explosion type and ambient medium density, and suggest that Type Ia supernova progenitors do not substantially modify their surroundings at radii of up to several parsecs. We also detect a K-shell radiative recombination continuum of Fe in W49B and IC 443, implying a strong circumstellar interaction in the early evolutionary phases of these core-collapse remnants.
  • Yamaguchi, Hiroya, Eriksen, Kristoffer A, Badenes, Carles, Hughes, John P, Brickhouse, Nancy S, Foster, Adam R, Patnaude, Daniel J, Petre, Robert, Slane, Patrick O, Smith, Randall K
    The Astrophysical Journal, 780(2) 136, Jan, 2014  Peer-reviewed
  • Castro, Daniel, Lopez, Laura A, Slane, Patrick O, Yamaguchi, Hiroya, Ramirez-Ruiz, Enrico, Figueroa-Feliciano, Enectali
    The Astrophysical Journal, 779(1) 49, Dec, 2013  Peer-reviewed
  • Lopez, Laura A, Pearson, Sarah, Ramirez-Ruiz, Enrico, Castro, Daniel, Yamaguchi, Hiroya, Slane, Patrick O, Smith, Randall K
    The Astrophysical Journal, 777(2) 145, Nov, 2013  Peer-reviewed
  • Uchida, Hiroyuki, Yamaguchi, Hiroya, Koyama, Katsuji
    The Astrophysical Journal, 771(1) 56, Jul, 2013  Peer-reviewed
  • Yamaguchi, H, Tanaka, M, Maeda, K, Slane, P. O, Foster, A, Smith, R. K, Katsuda, S, Yoshii, R
    The Astrophysical Journal, 749(2) 137, Apr, 2012  Peer-reviewed
  • Yamaguchi, Hiroya, Ozawa, Midori, Ohnishi, Takao
    Advances in Space Research, 49(3) 451-457, Feb, 2012  Peer-reviewed
  • Yamaguchi, Hiroya, Koyama, Katsuji, Uchida, Hiroyuki
    Publications of the Astronomical Society of Japan, 63(SP3) S837-S848, Nov, 2011  Peer-reviewed
  • Yamaguchi, H, Sawada, M, Bamba, A
    The Astrophysical Journal, 715(1) 412-420, May, 2010  Peer-reviewed
  • Yamaguchi, H, Ozawa, M, Koyama, K, Masai, K, Hiraga, J. S, Ozaki, M, Yonetoku, D
    The Astrophysical Journal Letters, 705(1) L6-L9, Nov, 2009  Peer-reviewed
  • Yamaguchi, H, Katsuda, S
    The Astrophysical Journal, 696(2) 1548-1553, May, 2009  Peer-reviewed
  • Yamaguchi, Hiroya, Bamba, Aya, Koyama, Katsuji
    Publications of the Astronomical Society of Japan, 61(SP1) S175-S181, Jan, 2009  Peer-reviewed
  • Yamaguchi, Hiroya, Koyama, Katsuji, Nakajima, Hiroshi, Bamba, Aya, Yamazaki, Ryo, Vink, Jacco, Kawachi, Akiko
    Publications of the Astronomical Society of Japan, 60(SP1) S123-S130, Jan, 2008  Peer-reviewed
  • Yamaguchi, Hiroya, Koyama, Katsuji, Katsuda, Satoru, Nakajima, Hiroshi, Hughes, John P, Bamba, Aya, Hiraga, Junko S, Mori, Koji, Ozaki, Masanobu, Tsuru, Takeshi Go
    Publications of the Astronomical Society of Japan, 60(SP1) S141-S152, Jan, 2008  Peer-reviewed
  • Yamaguchi, Hiroya, Ueno, Masaru, Koyama, Katsuji, Bamba, Aya, Yamauchi, Shigeo
    Publications of the Astronomical Society of Japan, 56(6) 1059-1065, Dec, 2004  Peer-reviewed

Misc.

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Books and Other Publications

 1

Presentations

 28
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Teaching Experience

 5

Professional Memberships

 3

Research Projects

 4

● 指導学生の顕著な論文

 1
  • Student name
    Yuken Ohshiro
    Student affiliation
    東京大学
    Author(s), journal, volume number, pagination (year of publication)
    Ohshiro et al., ApJL 913, L34, 7 (2021)
    Title
    Discovery of a Highly Neutronized Ejecta Clump in the Type Ia Supernova Remnant 3C 397
    DOI
    https://doi.org/10.3847/2041-8213/abff5b

● 専任大学名

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