研究者業績

田代 信

タシロ マコト  (Makoto Tashiro)

基本情報

所属
埼玉大学大学院 理工学研究科 教授
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 特任教授
学位
修士(理学)(東京大学)
博士(理学)(東京大学)

J-GLOBAL ID
200901083726265608
researchmap会員ID
1000161587

外部リンク

委員歴

 2

論文

 185
  • Satoru Katsuda, Hiroyuki Shinagawa, Hitoshi Fujiwara, Hidekatsu Jin, Yasunobu Miyoshi, Yoshizumi Miyoshi, Yuko Motizuki, Motoki Nakajima, Kazuhiro Nakazawa, Kumiko K Nobukawa, Yuichi Otsuka, Atsuki Shinbori, Takuya Sori, Chihiro Tao, Makoto S Tashiro, Yuuki Wada, Takaya Yamawaki
    Geophysical Research Letters 2024年8月29日  
  • Yoshiaki Kanemaru, Ryo Iizuka, Yoshitomo Maeda, Takashi Okajima, Takayuki Hayashi, Kazuhiro Kiyokane, Yuto Nihei, Takashi Kominato, Manabu Ishida, Chikara Natsukari, Shin Watanabe, Kosuke Sato, Yukikatsu Terada, Katsuhiro Hayashi, Chris Baluta, Tessei Yoshida, Akio Hoshino, Shoji Ogawa, Kotaro Fukushima, Hiromitsu Takahashi, Masayoshi Nobukawa, Tsunefumi Mizuno, Kazuhiro Nakazawa, Shin'ichiro Uno, Ken Ebisawa, Satoshi Eguchi, Satoru Katsuda, Aya Kubota, Naomi Ota, Megumi Shidatsu, Atsushi Tanimoto, Yuichi Terashima, Yohko Tsuboi, Yuusuke Uchida, Hideki Uchiyama, Shigeo Yamauchi, Yoneyama Tomokage, Satoshi Yamada, Nagomi Uchida, Rie Sato, Matt Holland, Michael Loewenstein, Eric D. Miller, Tahir Yaqoob, Robert S. Hill, Trisha F. Doyle, Efrain Perez-Solis, Morgan D. Waddy, Mark Mekosh, Joseph B. Fox, Makoto S. Tashiro, Kenichi Toda, Hironori Maejima
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray 224-224 2024年8月21日  
  • Megumi Shidatsu, Yukikatsu Terada, Takashi Kominato, So Kato, Ryohei Sato, Minami Sakama, Takumi Shioiri, Yugo Motogami, Yuki Niida, Toshihiro Takagi, Chikara Natsukari, Makoto S. Tashiro, Kenichi Toda, Hironori Maejima, Shin Watanabe, Ryo Iizuka, Rie Sato, Chris Baluta, Katsuhiro Hayashi, Tessei Yoshida, Shoji Ogawa, Yoshiaki Kanemaru, Kotaro Fukushima, Akio Hoshino, Hiromitsu Takahashi, Masayoshi Nobukawa, Tsunefumi Mizuno, Kazuhiro Nakazawa, Shin'ichiro Uno, Ken Ebisawa, Satoshi Eguchi, Satoru Katsuda, Aya Kubota, Naomi Ota, Atsushi Tanimoto, Yuichi Terashima, Yohko Tsuboi, Yuusuke Uchida, Hideki Uchiyama, Shigeo Yamauchi, Tomokage Yoneyama, Satoshi Yamada, Nagomi Uchida, Matt Holland, Michael Loewenstein, Eric D. Miller, Tahir Yaqoob, Robert S. Hill, Trisha F. Doyle, Efrain Perez-Solis, Morgan D. Waddy, Mark Mekosh, Joseph B. Fox
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray 235-235 2024年8月21日  
  • Yukikatsu Terada, Megumi Shidatsu, Makoto Sawada, Takashi Kominato, So Kato, Ryohei Sato, Minami Sakama, Takumi Shioiri, Yuki Niida, Chikara Natsukari, Makoto S. Tashiro, Kenichi Toda, Hironori Maejima, Katsuhiro Hayashi, Tessei Yoshida, Shoji Ogawa, Yoshiaki Kanemaru, Akio Hoshino, Kotaro Fukushima, Hiromitsu Takahashi, Masayoshi Nobukawa, Tsunefumi Mizuno, Kazuhiro Nakazawa, Shin'ichiro Uno, Ken Ebisawa, Satoshi Eguchi, Satoru Katsuda, Aya Kubota, Naomi Ota, Atsushi Tanimoto, Yuichi Terashima, Yohko Tsuboi, Yuusuke Uchida, Hideki Uchiyama, Shigeo Yamauchi, Tomokage Yoneyama, Satoshi Yamada, Nagomi Uchida, Shin Watanabe, Ryo Iizuka, Rie Sato, Chris Baluta, Matt Holland, Michael Loewenstein, Eric D. Miller, Tahir Yaqoob, Robert S. Hill, Trisha F. Doyle, Efrain Perez-Solis, Morgan D. Waddy, Mark Mekosh, Joseph B. Fox, Toshihiro Takagi, Yugo Motogami, Katja Pottschmidt, Teruaki Enoto, Takaaki Tanaka
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray 61-61 2024年8月21日  
  • Katsuhiro Hayashi, Makoto S. Tashiro, Yukikatsu Terada, Tessei Yoshida, Shoji Ogawa, Yoshiaki Kanemaru, Kotaro Fukushima, Akio Hoshino, Hiromitsu Takahashi, Masayoshi Nobukawa, Tsunefumi Mizuno, Kazuhiro Nakazawa, Shin'ichiro Uno, Ken Ebisawa, Satoshi Eguchi, Satoru Katsuda, Takao Kitaguchi, Aya Kubota, Naomi Ota, Megumi Shidatsu, Atsushi Tanimoto, Yuichi Terashima, Yohko Tsuboi, Yuusuke Uchida, Hideki Uchiyama, Shigeo Yamauchi, Tomokage Yoneyama, Satoshi Yamada, Nagomi Uchida, Seiko Sakurai, Shin Watanabe, Ryo Iizuka, Rie Sato, Chris Baluta, Takayuki Tamura, Yasushi Fukazawa, Hirokazu Odaka, Tsubasa Tamba, Ryohei Sato, Sou Kato, Minami Sakama, Takumi Shioiri, Yuki Niida, Natsuki Sakamoto, Noboru Nemoto, Yuki Omiya, Nari Suzuki, Toshihiro Takagi, Yugo Motogami, Matt Holland, Michael Loewenstein, Eric D. Miller, Tahir Yaqoob, Robert S. Hill, Trisha F. Doyle, Efrain Perez-Solis, Morgan D. Waddy, Mark Mekosh, Joseph B. Fox, Matteo Guainazzi, Jan-Uwe Ness, Hironori Maejima, Kenichi Toda, Chikara Natsukari
    Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray 60-60 2024年8月21日  

MISC

 287
  • 金田 英宏, 田代 信, 牧島 一夫, 石崎 欣尚, 高橋 忠幸, 窪 秀利, 大橋 隆哉
    日本物理学会講演概要集. 秋の分科会 1995(1) 141-141 1995年9月12日  
  • 大林 均, 深沢 泰司, 牧島 一夫, 田代 信, 粟木 久光, 寺島 雄一, 三原 建弘, 大橋 隆哉, 鶴 剛
    日本物理学会講演概要集. 秋の分科会 1995(1) 142-142 1995年9月12日  
  • 田原 譲, 田代 信, 小谷 太郎
    天文月報 88(6) 264-265 1995年6月  
  • 岡田 京子, 牧島 一夫, 田代 信, 池辺 靖, 石崎 欣尚, 三原 建弘
    日本物理学会講演概要集. 年会 50(1) 131-131 1995年3月16日  
  • 金田 英宏, 牧島 一夫, 田代 信, 松崎 恵一, 杉崎 睦, 田中 靖郎, 山内 茂雄, 山崎 典子
    日本物理学会講演概要集. 年会 50(1) 132-132 1995年3月16日  
  • 田村 隆幸, 金田 英宏, 杉崎 睦, 田代 信, 牧島 一夫, 高橋 忠幸, 釜江 常好, 村上 敏夫, HXT Working Group
    日本物理学会講演概要集. 年会 50(1) 33-33 1995年3月16日  
  • 田代 信, 牧島 一夫, 金田 英宏, 高橋 忠幸, 窪 秀利, 石崎 欣尚, 大橋 隆哉
    日本物理学会講演概要集. 年会 50(1) 133-133 1995年3月16日  
  • 伊予本 直子, 牧島 一夫, 深沢 泰司, 田代 信, 大塚 貴徳, 大橋 隆哉
    日本物理学会講演概要集. 年会 50(1) 133-133 1995年3月16日  
  • M TASHIRO, K MAKISHIMA, T OHASHI, M INDAKOIDE, A YAMASHITA, T MIHARA, Y KOHMURA
    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 47(2) 131-140 1995年  
    The BL Lac object PKS 0548-322 was observed in X-rays with Ginga five times between 1990 January and 1991 March. The 2-20 keV flux varied by a factor of 2.5, and the spectral energy index a showed a significant change of between 0.8+/-0.02 and 1.03+/-0.04. No simple relation has been found between the flux and the spectral index. An upper limit for the equivalent width of the iron K line is 83 eV at 90% confidence. Based on the spectral results, we propose a simple scheme to interpret the variation of the X-ray spectrum in terms of the synchrotron emission. This gives new constraints on the properties of the emission region.
  • KC GENDREAU, R MUSHOTZKY, AC FABIAN, SS HOLT, T KII, PJ SERLEMITSOS, Y OGASAKA, Y TANAKA, MW BAUTZ, Y FUKAZAWA, Y ISHISAKI, Y KOHMURA, K MAKISHIMA, M TASHIRO, Y TSUSAKA, H KUNIEDA, GR RICKER, RK VANDERSPEK
    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 47(2) L5-L9 1995年  
    We present initial results from ASCA on the spectrum of the Cosmic X-ray Background from 0.4 to 10 keV. About 250 ks of deep survey data has been collected from the performance verification phase of ASCA. About 110 ks of dark-earth data are used to assess the internal background. A single power-law describes the X-ray background very well in the 1 to 10 keV with no evidence for a steepening in the 1 to 3 keV range. At 1 keV, the intensity of the X-ray background is 9.6 keV s(-1) cm(-2) sr-l keV(-1). Our data clearly show an excess above the extrapolation of the single power law model below 1 keV. At least part of this excess can be accounted for with a thermal component as there is evidence for O VII and O VIII emission.
  • 石崎 欣尚, 窪 秀利, 高橋 忠幸, 田代 信, 池辺 靖, 牧島 一夫, 上田 佳弘, 小賀坂 康志, 紀伊 恒男, 井上 一, 山崎 典子, あすかチーム
    日本物理学会講演概要集. 秋の分科会 1994(1) 171-171 1994年9月12日  
  • 窪 秀利, 石崎 欣尚, 高橋 忠幸, 田代 信, 池辺 康, 牧島 一夫, 上田 佳弘, 小賀坂 康志, 紀伊 恒男, 井上 一, 山崎 典子
    日本物理学会講演概要集. 秋の分科会 1994(1) 172-172 1994年9月12日  
  • 伊予本 直子, 深沢 泰司, 田代 信, 牧島 一夫, 大橋 隆哉, 山崎 典子, 武藤 勝弥
    日本物理学会講演概要集. 秋の分科会 1994(1) 168-168 1994年9月12日  
  • 田代 信, 山下 朗子, 紀伊 恒男, 大橋 隆哉, 牧島 一夫, 伊予本 直子, 出沢 恵理子
    日本物理学会講演概要集. 秋の分科会 1994(1) 170-170 1994年9月12日  
  • 岡田 京子, 牧島 一夫, 田代 信, 池辺 靖, 石碕 欣尚, 三原 建弘
    日本物理学会講演概要集. 年会 49(1) 177-177 1994年3月16日  
  • 大橋 隆哉, 深沢 泰司, 渡辺 靖, 石崎 欣尚, 上条 俊介, 金田 英広, 香村 芳樹, 牧島 一夫, 松下 恭子, 中川 健一郎, 田代 信, 石田 学, 井上 一, 槙野 文明, 村上 敏夫, 小笠原 嘉明, 田中 靖郎, 上田 佳宏, 三原 建弘, 竹島 敏明, 鶴 剛, 海老沢 研
    日本物理学会講演概要集. 年会 49(1) 167-167 1994年3月16日  
  • 深沢 泰司, 中川 健一郎, 田村 隆幸, 田代 信, 牧島 一夫, 大橋 隆哉, 山崎 典子
    日本物理学会講演概要集. 年会 49(1) 177-177 1994年3月16日  
  • M INDA, K MAKISHIMA, Y KOHMURA, M TASHIRO, T OHASHI, P BARR, K HAYASHIDA, GGC PALUMBO, G TRINCHIERI, M ELVIS, G FABBIANO
    ASTROPHYSICAL JOURNAL 420(1) 143-151 1994年1月  
    X-ray properties of the radio galaxy 3C 390.3 were investigated using the EXOSAT and Ginga satellites. Long-term, large-amplitude X-ray intensity changes were detected over a period extending from 1984 through 1991, and high-quality X-ray spectra were obtained especially with Ginga. The X-ray continuum spectra were described with power-law model with photon slope in the range 1.5-1.8, and the slope flattened as the 2-20 keV luminosity decreased by 40%. There was a first detection of the iron emission line from this source at the 90% confidence level. An upper limit was derived on the thermal X-ray component. X-ray emission mechanisms and possible origins of the long-term variation are discussed.
  • K MAKISHIMA, R FUJIMOTO, Y ISHISAKI, T KII, M LOEWENSTEIN, R MUSHOTZKY, P SERLEMITSOS, T SONOBE, M TASHIRO, T YAQOOB
    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 46(3) L77-& 1994年  
    The spectra and images of the nearby jet galaxy NGC 4258 (M106) obtained with ASCA indicate presence of several distinct X-ray emission components. The emission above 3 keV is pointlike and coincident in position with the optical nucleus, exhibiting a hard (photon index approximately 1.78) and absorbed (N(H) approximately 1.5 x 10(23) cm-2) spectrum. This provides clear evidence that NGC 4258 hosts an obscured active nucleus of low luminosity, about 4 x 10(40) ergs s-1 in 2-10 keV after removing the absorption. Iron K-line emission with an equivalent width 0.25 +/- 0.10 keV was detected. The emission below 1 keV is dominated by an extended (approximately 4') thin-thermal component with a temperature approximately 0.5 keV exhibiting atomic emission lines, possibly associated with the jet. There exists a third continuum component with an intermediate spectral hardness, which is brightest at approximately 1' south-east of the nucleus.
  • Y KOHMURA, K MAKISHIMA, M TASHIRO, T OHASHI, CM URRY
    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 46(2) 131-138 1994年  
    The BL Lacertae object H0323+022 was observed in X-rays with Ginga on three occasions, in 1987 July, 1988 August, and 1991 August. In the 1987 observation, the source was relatively bright, and variable by a factor of 3 on time scales of several hours. The observed 2-20 keV energy flux ranged between 2.2 and 4.1 x 10(-11) ergs CM-2 s-1 during the variation. The X-ray spectra were well described by a power-law model without intrinsic photoelectric absorption, and the photon index varied between 1.3 and 1.9 as the intensity changed. The spectrum was much better correlated with the time derivative of the X-ray intensity than the intensity, itself, in such a way that the spectrum hardened when the intensity increased. A detailed analysis of this spectrum-intensity correlation indicates that variation in the higher-energy band (4.1-10.5 keV) precedes that in the lower-energy band (1.2-4.1 keV) by roughly 0.05 d. This supports the idea that X-ray emission from H0323+022 is of synchrotron origin. In the 1988 and 1991 observations, the source was rather faint and only marginally detected at a 2-20 keV flux level between 0.6 and 1.1 x 10(-11) ergs CM-2 S-1. On these two occasions no intensity variations were detected, and soft spectra with a photon index of more than 2.0 are indicated.
  • T YAQOOB, P SERLEMITSOS, R MUSHOTZKY, G RICKER, J WOO, K WEAVER, T KII, K MITSUDA, T KOTANI, K HAYASHIDA, S MURAKAMI, M TASHIRO
    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 46(3) L49-L53 1994年  
    We report preliminary results of an ASCA observation of 3C 273. There is no spectral variability within the ASCA observation, in contrast to the longer term behavior found with EXOSAT and Ginga which established significant changes in the spectral index of the power-law continuum on timescales of a week or more, uncorrelated with luminosity. Comparison of the ASCA data with a simultaneous ROSAT/Ginga observation in 1990 December shows that while the shape of the spectrum above approximately 1 keV is essentially the same, the flux in the soft component, below approximately 1 keV, is considerably weaker relative to the hard component in the ASCA observation. The 2-10 keV luminosity is at least a factor of approximately 1.5 greater in the ASCA observation than in the ROSAT/Ginga observation whilst the ratio of 2-10 keV luminosity to 0.4-1.0 keV luminosity increases by a factor of approximately 1.2. Thus the spectral shape of the hard component appears to be independent of the relative magnitude of the soft component and is an important constraint on emission and reprocessing models. We find no significant Fe K line-emission in this observation. The data also highlight very well some of the outstanding problems in the instrumental responses.
  • RS WARWICK, S SEMBAY, T YAQOOB, K MAKISHIMA, T OHASHI, M TASHIRO, Y KOHMURA
    MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 265(2) 412-420 1993年11月  
    We present the results of Ginga observations of three narrow emission line X-ray galaxies, NGC 7172, NGC 7582 and ESO 103-G35. In each of these galaxies the column density along the line of sight to the active nucleus is extremely high (i.e. n(H) greater-than-or-similar-to 10(23) cm-2). A comparison of the optical depth in the iron K-edge with the low-energy absorption in the X-ray spectrum indicates an apparent iron abundance in excess of the solar value in these sources. Measurements of the iron K-edge energy show that the bulk of the X-ray-absorbing gas is not strongly photoionized, with only ESO 103-G35 exhibiting an edge energy significantly above that for neutral iron. In the case of NGC7582, the line-of-sight column density may have increased by a factor of approximately 3 over an interval of about 4 yr. The implications of these results for current models of the state and distribution of gaseous material in low-luminosity active galactic nuclei are briefly discussed.
  • S SEMBAY, RS WARWICK, CM URRY, J SOKOLOSKI, IM GEORGE, F MAKINO, T OHASHI, M TASHIRO
    ASTROPHYSICAL JOURNAL 404(1) 112-123 1993年2月  
    We present a detailed study of the hard X-ray properties of the BL Lacertae object PKS 2155-304 based on measurements made in 1988 and 1989 with the Large Area Counter (LAC) on board the Ginga satellite. The source exhibited a high degree of variability with a dynamic range of a factor 7 in the 2-6 keV band. The fastest amplitude variation was a factor 2 decline in the intensity in this band within 4 hours. The spectrum is characterized by a break which occurs at approximately 4 keV. Spectral fits to the data integrated in 6400 s time bins reveal that, in common with previous observations of BL Lacertae objects, the spectral slope is generally anticorrelated with intensity in the sense that the spectrum hardens as the intensity increases. However, the tracks of sequential points in the index-intensity plane are occasionally seen to differ during the rise and decay stages of individual flares. Furthermore, during one, or possibly two, flaring episodes the spectral index is observed to correlate with intensity variations. The X-ray properties of PKS 2155-304 are most readily interpreted in terms of direct synchrotron radiation originating within a relativistic jet, however, the X-ray emitting region is probably more complex than the geometries assumed in most standard jet models. Further development of time-dependent theoretical models will be necessary to explain some of the details of the present observations.
  • T OHASHI, M TASHIRO, K MAKISHIMA, T KII, F MAKINO, MJL TURNER, OR WILLIAMS
    ASTROPHYSICAL JOURNAL 398(1) 87-93 1992年10月  
    Two bright quasars NRAO 140 (z = 1.258) and 4C 34.47 (z = 0.206) have been studied with Ginga. The observed spectra in the energy range 2-20 keV, in the observer rest frame, are well described by power-law models. The measured 2-10 keV luminosities and energy indices are L(x) = 3.8 x 10(46) ergs s-1 and alpha = 0.72 +/- 0.11 for NRAO 140, and L(x) = 5.3 x 10(44) ergs s-1 and alpha = 0.64(-0.14)+0.17 for 4C 34.47 (H-0 = 100 km s-1 Mpc-1; q0 = 0.5); the intensity variation was less than about 10% during the approximately 1 day observation for each source. Upper limits, in the source rest frame, for iron line emission are EW < 200 and EW < 120 eV for NRAO 140 and 4C 34.47, respectively. The featureless X-ray spectra, whose slopes are flatter than those of BL Lac objects, and the high X-ray luminosities in excess of the extension of the IR-optical continuum are consistent with the synchrotron self-Compton emission accompanied by a moderate beaming toward us.
  • 牧島 一夫, 大橋 隆哉, 田代 信, 香村 芳樹, 池辺 靖, 浅沼 達彦, 石崎 欣尚, 深沢 泰司, 井上 一, 石田 学, 上田 佳宏, 村上 敏夫, 田中 靖郎, 鶴 剛, 三原 建弘, 竹島 敏明, 海老沢 研
    秋の分科会講演予稿集 1992(1) 147-147 1992年9月14日  
  • 大橋隆哉, 牧島一夫, 田代信, 井上一, 石田学, 鶴剛, 三原建弘, 竹島敏明, 海老沢研
    日本物理学会講演概要集(分科会) 1992(Autumn Pt 1) 147 1992年9月  
  • 牧島一夫, 大橋隆哉, 田代信, 深沢泰司, 井上一, 田中靖郎, 鶴剛, 三原建弘, 海老沢研
    日本物理学会講演概要集(分科会) 1992(Autumn Pt 1) 147 1992年9月  
  • 三原建弘, 大橋隆哉, 牧島一夫, 鶴剛, 石田学, 田代信, 香村芳樹, 池辺靖, 井上一
    科学衛星シンポジウム 1991 23-28 1991年10月  
  • M. Tashiro, K. Makishima, T. Ohashi, T. Sakao, A. E. Sansom
    Monthly Notices of Royal Astronomical Society 252(1) 156-162 1991年9月  
  • M TASHIRO, K MAKISHIMA, T OHASHI, T SAKAO, AE SANSOM
    MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 252(1) 156-162 1991年9月  
    Ginga observations of the X-ray binary pulsar GX301 - 2 are analysed for their temporal and spectral properties. We report the unambiguous detection of aperiodic intensity variations of 7-10 per cent rms relative amplitude over time-scales covering approximately 16 to 0.1 s. These variations are self-similar, being well fitted by a power law in power spectral density versus frequency space. The pulse period measured is 689.80 s, the shortest yet measured for this source. The fraction of X-rays which is pulsed is energy dependent, being greater at higher energies. The fractional aperiodic variability shows no such energy dependence, nor do they appear to be significantly dependent on source intensity, pulse phase or absorbing column measured. These facts strongly suggest that the aperiodic variations are not caused by absorption variations, but are intrinsic to the source. The iron-line intensity shows little pulsations, but surprisingly shows significant aperiodic variability down to a time-scale as short as several seconds, thus giving a constraint to the size of the line emission region.
  • 香村 芳樹, 牧島 一夫, 大橋 隆哉, 石田 学, 鶴 剛, 田代 信, 三原 建弘, 上條 俊介, 池辺 靖, 井上 一
    春の分科会講演予稿集 1991(1) 81-81 1991年3月11日  
  • 大橋隆哉, 牧島一夫, 鶴剛, 石田学, 三原建弘, 田代信, 香村芳樹, 井上一
    搭載機器基礎開発成果報告書 4 1-5 1991年3月  
  • 鶴剛, 大橋隆哉, 牧島一夫, 石田学, 田代信, 三原建弘, 井上一
    科学衛星シンポジウム 1990 43-46 1990年12月  
  • K MAKISHIMA, T MIHARA, M ISHIDA, T OHASHI, T SAKAO, M TASHIRO, T TSURU, T KII, F MAKINO, T MURAKAMI, F NAGASE, Y TANAKA, H KUNIEDA, Y TAWARA, S KITAMOTO, S MIYAMOTO, A YOSHIDA, MJL TURNER
    ASTROPHYSICAL JOURNAL 365(2) L59-L62 1990年12月  
  • T MIHARA, K MAKISHIMA, T OHASHI, T SAKAO, M TASHIRO, F NAGASE, Y TANAKA, S KITAMOTO, S MIYAMOTO, JE DEETER, PE BOYNTON
    NATURE 346(6281) 250-252 1990年7月  
  • 牧島 一夫, 坂尾 太郎, 三原 建弘, 田代 信, 石田 学, 大橋 隆哉, 長瀬 文昭, 村上 敏夫, 田中 靖郎, 吉田 篤正
    宇宙科学研究所報告. 特集 25 195-204 1990年1月  
    「てんま」, 「ぎんが」のデータにもとづき, X線パルサーのスペクトル中に観測されたサイクロトロン吸収構造とその意義を論じる。おもな結果は以下のようにまとめられる。a. X線パルサー4U1538-52での発見に続き, 「ぎんが」により, トランジェントX線パルサーX0331+53のスペクトルの28keV付近に, 新たにサイクロトロン吸収構造が発見された。このようなサイクロトロン構造は, X線パルサーにひろく見られる現象であるらしい。b. X線パルサーHer X-1のスペクトル構造は輝線ではなく, エネルギーE∿34keVの吸収線と解釈できるとわかった。これにより, 永年の論争に決着がつけられた。c. X線パルサーのスペクトルのエネルギーE=10∿20keVに見られる急な「折れ曲り」が, サイクロトロン共鳴を直接に反映していること, 従って磁場強度のよい指標になることが確実になってきた。d.上の立場にもとづいて既知のスペクトルからX線パルサーの表面磁場強度を推定してみると, いずれも(1-4)×10^<12>Gときわめて良くそろった値となる。
  • 森沢 正昭, 神部 勉, 牧島 一夫, 大橋 隆哉, 石田 学, 坂尾 太郎, 鶴 剛, 田代 信, 三原 建弘, 印田 美香, 好村 芳樹, 米倉 伸之, 高尾 英行, 十倉 好紀, 石原 正泰, 江口 徹, 守 隆夫, 長澤 弘, 東江 昭夫, 増田, 白田 由香利, 國井 利泰, Krishman Deepa, 川島 誠一郎, 渡辺 嘉久, 尾本 恵市, 伊藤 谷生, ゲラー R, 金森 審子, 北品 健, 井上 康男, 永嶺 譲忠, 山崎 敏光, 飯島 健
    東京大学理学部弘報 21(3) 21-25 1989年12月  

共同研究・競争的資金等の研究課題

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