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The most well-known fitting model for Black Hole Binaries (BHBs) is the Disk BlackBody (DBB) model, in which the effective temperature profile is assumed to be T(sub eff) is proportional to r(exp -3/4), where r is the disk radius. It has two fitting parameters: the innermost disk temperature, T(sub in), and the innermost radius, r(sub in). For a non-rotating black hole, its mass can be estimated by assuming that the innermost radius coincides with r(sub in) = 3r(sub g) (proportional to M), where r(sub g) is the Schwarzschild radius. However, this conventional method does not give an accurate mass for super-critical accretion flow, in which both of the innermost radius and temperature profile are modified from those of the sub-critical flow. We, here, propose a methodology to derive a black hole mass for the super-critical accretion flow. 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On black hole mass estimation from X-ray spectra of ultraluminous X-ray sources
https://jaxa.repo.nii.ac.jp/records/38437
https://jaxa.repo.nii.ac.jp/records/3843715f2f8fe-2fdd-48bf-b11a-0fb54b5f28bc
Item type | 会議発表論文 / Conference Paper(1) | |||||
---|---|---|---|---|---|---|
公開日 | 2015-03-26 | |||||
タイトル | ||||||
言語 | en | |||||
タイトル | On black hole mass estimation from X-ray spectra of ultraluminous X-ray sources | |||||
言語 | ||||||
言語 | eng | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | ブラックホール | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 質量 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | X線スペクトル | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | スペクトル解析 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 温度分布 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | ブラックホール質量 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | Disk Blackbodyモデル | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | DBBモデル | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 大光度X線源 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | ULX | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 推定 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | X線連星 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 数学モデル | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | 数値解析 | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | カーブフィッティング | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | black hole | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | mass | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | X-ray spectrum | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | spectrum analysis | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | temperature distribution | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | black hole mass | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | disk blackbody model | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | DBB model | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | ultraluminous X ray source | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | ULX | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | estimating | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | X-ray binary | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | mathematical model | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | numerical analysis | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | curve fitting | |||||
資源タイプ | ||||||
資源タイプ識別子 | http://purl.org/coar/resource_type/c_5794 | |||||
資源タイプ | conference paper | |||||
アクセス権 | ||||||
アクセス権 | metadata only access | |||||
アクセス権URI | http://purl.org/coar/access_right/c_14cb | |||||
著者 |
Vierdayanti, Kiki
× Vierdayanti, Kiki× 渡會, 兼也× 嶺重, 慎× Vierdayanti, Kiki× Watarai, Kenya× Mineshige, Shin |
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著者所属 | ||||||
京都大学基礎物理学研究所 | ||||||
著者所属 | ||||||
大阪教育大学 天文学研究室 | ||||||
著者所属 | ||||||
京都大学基礎物理学研究所 | ||||||
著者所属(英) | ||||||
en | ||||||
Yukawa Institute for Theoretical Physics, Kyoto University | ||||||
著者所属(英) | ||||||
en | ||||||
Osaka Kyoiku University Astronomical Institute | ||||||
著者所属(英) | ||||||
en | ||||||
Yukawa Institute for Theoretical Physics, Kyoto University | ||||||
出版者 | ||||||
出版者 | 宇宙航空研究開発機構宇宙科学研究本部 | |||||
出版者(英) | ||||||
出版者 | Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA/ISAS) | |||||
書誌情報 |
宇宙圏研究会高エネルギー宇宙物理連絡会,第8回研究会集録原稿:超新星とその残骸 en : Proceedings of the 8th Workshop of High Energy AstroPhysics Association, Workshop for Space Astrophysics: Supernova and Its Remnant p. 181-186, 発行日 2007-10-17 |
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抄録(英) | ||||||
内容記述タイプ | Other | |||||
内容記述 | One of the most useful methods to estimate the black hole mass in X-ray Binaries (XBs), when the dynamical method is unavailable, is by X-ray spectral fitting. The most well-known fitting model for Black Hole Binaries (BHBs) is the Disk BlackBody (DBB) model, in which the effective temperature profile is assumed to be T(sub eff) is proportional to r(exp -3/4), where r is the disk radius. It has two fitting parameters: the innermost disk temperature, T(sub in), and the innermost radius, r(sub in). For a non-rotating black hole, its mass can be estimated by assuming that the innermost radius coincides with r(sub in) = 3r(sub g) (proportional to M), where r(sub g) is the Schwarzschild radius. However, this conventional method does not give an accurate mass for super-critical accretion flow, in which both of the innermost radius and temperature profile are modified from those of the sub-critical flow. We, here, propose a methodology to derive a black hole mass for the super-critical accretion flow. In this method, we use as a spectral fitting model, the extended DBB model, in which an effective temperature profile obeys the relation, T(sub eff) is proportional to r(exp -p), with the temperature gradient, p, being treated as a fitting parameter (in addition to two others; T(sub in) and r(sub in)). We first calculate theoretical flow structure and its spectra for given black hole mass and accretion rate, M and dot-M. Through the fitting to the theoretical spectra by the extended DBB model, we can estimate a black hole mass, M(sub x), assuming r(sub in) = 3r(sub g). We find, however, that the estimated mass deviates from that adopted in the spectral calculations, M, even for low dot-M cases. We also find that the deviations can be eliminated by introducing a new correction for the innermost radius. Using this correction, we calculate mass correction factors, M/M(sub x), in the super-critical regimes for some sets of M and dot-M, finding that a mass correction factor ranges between M/M(sub x) is approximately 1.2-1.6. The higher dot-M is, the larger the mass correction factor tends to be. Since the correction is relatively small, we can safely conclude that the black holes in ULXs (UltraLuminous X-ray sources) which Vierdayanti et al. (2006) analyzed are stellar-mass black holes with mass less than 100 solar mass. | |||||
資料番号 | ||||||
内容記述タイプ | Other | |||||
内容記述 | 資料番号: AA0063722008 |