研究者業績

堂谷 忠靖

ドウタニ タダヤス  (Tadayasu Dotani)

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
東京工業大学 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

論文

 215
  • G HASINGER, M VANDERKLIS, K EBISAWA, T DOTANI, K MITSUDA
    ASTRONOMY & ASTROPHYSICS 235(1-2) 131-146 1990年8月  査読有り
  • T DOTANI, K MITSUDA, H INOUE, Y TANAKA, N KAWAI, Y TAWARA, K MAKISHIMA, J VANPARADIJS, W PENNINX, M VANDERKLIS, J TAN, WHG LEWIN
    ASTROPHYSICAL JOURNAL 350(1) 395-407 1990年2月  査読有り
  • J VANPARADIJS, T DOTANI, Y TANAKA, T TSURU
    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 42(5) 633-660 1990年  査読有り
    We report on a Ginga observation of the globular-cluster source 4U 2129+11 in M15, during which we detected a very energetic X-ray burst. This burst showed a precursor, separated from the main event by approximately 6 s, which indicates that strong expansion of the neutron star photosphere occurred. During the first 30 s of the main part of the burst a series of slow radius oscillations were observed, whose termination may signify the transition from an outflowing neutron star wind to a static extended (but very slowly shrinking) envelope. From a time-resolved spectral analysis of the burst data we find evidence for deviations of the burst spectra from a blackbody, which cannot be described in terms of a spectral hardening alone. We show that, in principle, the results of the analysis may be used to derive information on the mass and radius of the neutron star, as well as on the anisotropy of the burst emission (as long as this remains the same during the burst). The applicability of this method is presently limited by uncertainties in the interpretation of the burst spectra.
  • Shunji Kitamoto, Hiroshi Tsunemi, Sigenori Miyamoto, Koujun Yamashita, Seiko Mizobuchi, Michio Nakagawa, Tadayasu Dotani, Fumiaki Makino
    Nature 342(6249) 518-520 1989年  
    TRANSIENT X-ray sources are generally considered to comprise accreting binary systems containing either a black hole or a neutron star1-5. The transient X-ray emission is thought to result from episodic mass transfer to the compact star if this is so, transient sources should provide information on the mass-accretion mechanism. On 21 May 1989, the All-Sky Monitor6 (ASM) onboard the satellite Ginga7 discovered an unusual bright X-ray transient source, GS2023+338, in the constellation of Cygnus8. The ASM and Large-Area Counters9 (LAC), also on Ginga, have since monitored the source. Here we report the light curves and spectral evolution observed by the ASM and LAC. From 21 May to 1 June, the intensity varied by up to a factor of 500 on timescales from a few seconds to a few days10. Subsequently the rapid variations persisted, whereas slower ones disappeared. The spectral data fit a power-law model with a photon index of 0.0 to -2.5 and an absorption column density of 1021.7-1022.8 H atoms cm-2. This unusual behaviour remains to be explained. © 1989 Nature Publishing Group.
  • KS WOOD, P HERTZ, JP NORRIS, BA VAUGHAN, PF MICHELSON, K MITSUDA, T DOTANI
    PROCEEDINGS OF THE 23RD ESLAB SYMPOSIUM ON TWO TOPICS IN X-RAY ASTRONOMY, VOLS 1 AND 2 296 689-692 1989年  査読有り
  • JP NORRIS, P HERTZ, KS WOOD, BA VAUGHAN, PF MICHELSON, K MITSUDA, T DOTANI
    PROCEEDINGS OF THE 23RD ESLAB SYMPOSIUM ON TWO TOPICS IN X-RAY ASTRONOMY, VOLS 1 AND 2 296 557-561 1989年  査読有り
  • T DOTANI, K MITSUDA, K MAKISHIMA, MH JONES
    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 41(3) 577-589 1989年  査読有り
  • MJL TURNER, HD THOMAS, BE PATCHETT, DH READING, K MAKISHIMA, T OHASHI, T DOTANI, K HAYASHIDA, H INOUE, H KONDO, K KOYAMA, K MITSUDA, Y OGAWARA, S TAKANO, H AWAKI, Y TAWARA, N NAKAMURA
    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 41(3) 345-372 1989年  査読有り
  • K MAKISHIMA, M ISHIDA, T OHASHI, T DOTANI, H INOUE, K MITSUDA, Y TANAKA, MJL TURNER, R HOSHI
    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 41(3) 531-555 1989年  査読有り
  • K MITSUDA, T DOTANI
    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 41(3) 557-575 1989年  査読有り
  • N NAKAMURA, T DOTANI, H INOUE, K MITSUDA, Y TANAKA, M MATSUOKA
    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 41(3) 617-639 1989年  査読有り
  • S MIYAMOTO, S KITAMOTO, K MITSUDA, T DOTANI
    NATURE 336(6198) 450-452 1988年12月  査読有り
  • K. Makishima, T. Ohashi, T. Sakao, T. Dotani, H. Inoue, K. Koyama, F. Makino, K. Mitsuda, F. Nagase, H. D. Thomas, M. J.L. Turner, T. Kii, Y. Tawara
    Nature 333(6175) 746-748 1988年  
    X-ray pulsars1,2 are magnetized, spinning neutron stars accreting matter from their binary companions. Their pulse periods P, ranging over four orders of magnitude, increase and decrease in complex ways1,3,4. The more luminous ones tend to show faster spin-up1,5. A puzzle is that the spin-up timescales of many X-ray pulsars are much shorter than their binary-evolution timescales, thus apparently violating the steady-state condition. It has there-fore been suspected6 that there exist many 'turned-off X-ray pulsars currently spinning down undetected. An excellent test for this hypothesis became available using the X-ray pulsar GX1 +4, which used to show the fastest spin-up over a decade1,7-10and then faded away11. Using the X-ray satellite Ginga12, we detected GX1+4 at ∼1/40 the previous intensity, and found that it now has an average spin-down trend. This discovery apparently supports the above hypothesis. © 1988 Nature Publishing Group.
  • T DOTANI, K HAYASHIDA, H INOUE, M ITOH, K KOYAMA, F MAKINO, K MITSUDA, T MURAKAMI, M ODA, Y OGAWARA, S TAKANO, Y TANAKA, A YOSHIDA, K MAKISHIMA, T OHASHI, N KAWAI, M MATSUOKA, R HOSHI, S HAYAKAWA, T KII, H KUNIEDA, F NAGASE, Y TAWARA, HATSUKADE, I, S KITAMOTO, S MIYAMOTO, H TSUNEMI, K YAMASHITA, M NAKAGAWA, M YAMAUCHI, MJL TURNER, KA POUNDS, HD THOMAS, GC STEWART, AM CRUISE, BE PATCHETT, DH READING
    NATURE 330(6145) 230-231 1987年11月  査読有り
  • N SATO, S HAYAKAWA, F NAGASE, K MASAI, T DOTANI, H INOUE, F MAKINO, K MAKISHIMA, T OHASHI
    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 38(5) 731-750 1986年  査読有り

MISC

 200
  • 堂谷忠靖, 他LiteBIRD Joint Study Group
    日本天文学会2024年春季年会 V130a 2024年3月  筆頭著者
  • 宮城生成, 堂谷忠靖
    日本天文学会2024年春季年会 W32a 2024年3月  
  • 中嶋大, 森浩二, 冨田洋, 野田博文, 鈴木寛大, 小林翔悟, 萩野浩一, 内田裕之, 米山友景, 田中孝明, 村上弘志, 信川正順, 信川久実子, 内山秀樹, 幸村孝由, 鶴剛, 松本浩典, 小高裕和, 山内誠, 廿日出勇, 山岡和貴, 吉田鉄生, 金丸善朗, 水野恒史, 宮崎啓太郎, 楠康平, 大塚芳徳, 横須晴彦, 米丸若菜, 市川雄大, 中野瑛子, 福田将大, 朝倉一統, 善本真梨那, 大出優一, 佐藤淳矢, 袴田知宏, 青柳美緒, 青木悠馬, 伊藤耶馬斗, 青木大輝, 藤澤海斗, 清水康行, 樋口茉由, 東竜一, 寺農夏樹, 阪本菜月, OKAJIMA Takashi, 石田学, 前田良知, 平賀純子, 尾崎正伸, 堂谷忠靖, 常深博, 林田清
    日本天文学会年会講演予稿集 2024 2024年  
  • 信川久美子, 森浩二, 森浩二, 冨田洋, 中嶋大, 中嶋大, 野田博文, 林田清, 鈴木寛大, 小林翔悟, 内田裕之, 萩野浩一, 青木悠馬, 伊藤耶馬斗, 金丸善朗, 宮崎啓太郎, 楠康平, 大塚芳徳, 横須晴彦, 米丸若菜, 市川雄大, 中野瑛子, 中村彰太郎, 亀井貴光, 朝倉一統, 善本真梨那, 大出優一, 佐藤淳矢, 袴田知宏, 青柳美緒, 角町駿, 土居俊輝, 青木大輝, 藤澤海斗, 清水康行, 畠中大介, 田中孝明, 村上弘志, 信川正順, 内山秀樹, 吉田鉄生, 米山友景, 幸村孝由, 鶴剛, 松本浩典, OKAJIMA Takashi, 石田学, 前田良知, 山内誠, 廿日出勇, 平賀純子, 山岡和貴, 尾崎正伸, 堂谷忠靖, 常深博
    日本天文学会年会講演予稿集 2023 2023年  
  • 野田博文, 森浩二, 森浩二, 冨田洋, 中嶋大, 中嶋大, 林田清, 鈴木寛大, 小林翔悟, 内田裕之, 萩野浩一, 金丸善朗, 宮崎啓太郎, 楠康平, 大塚芳徳, 横須晴彦, 米丸若菜, 市川雄大, 中野瑛子, 中村彰太郎, 亀井貴光, 朝倉一統, 善本真梨那, 大出優一, 佐藤淳矢, 袴田知宏, 青柳美緒, 青木悠馬, 伊藤耶馬斗, 角町駿, 土居俊輝, 青木大輝, 藤澤海斗, 清水康行, 畠中大介, 田中孝明, 村上弘志, 信川正順, 信川久実子, 内山秀樹, 吉田鉄生, 米山友景, 幸村孝由, 鶴剛, 松本浩典, OKAJIMA Takashi, 石田学, 前田良知, 山内誠, 廿日出勇, 平賀純子, 山岡和貴, 尾崎正伸, 堂谷忠靖, 常深博
    日本物理学会講演概要集(CD-ROM) 78(1) 2023年  

共同研究・競争的資金等の研究課題

 15

● 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)