We discovered a so called high-temperature blackbody (HBB) component, found in the 15 – 40 keV range, in the broad-band X-ray energy spectra of black hole (BH) candidate sources. A detailed study of this spectral feature is presented using data from five of the Galactic BH binaries, Cyg X–1, GX 339–4, GRS 1915+105, SS 433 and V4641 Sgr in the low/hard, intermediate, high/soft and very soft spectral states (LHS, IS, HSS and VSS, respectively) and spectral transitions between them using RXTE, INTEGRAL and BeppoSAX data. In order to fit the broad-band energy spectra of these sources we used an additive XSPEC model, composed of the Comptonization component and the Gaussian line component. In particular, we reveal that the IS spectra have the HBB component which color temperature, kTHBB is in the range of 4.5 – 5.9 keV. This HBB feature has been detected in some spectra of these five sources only in the IS (for the photon index Γ > 1.9) using different X-ray telescopes. We also demonstrate that a timescale of the HBB-feature is of orders of magnitude shorter than the timescale of the iron line and its edge. That leads us to conclude that these spectral features are formed in geometrically different parts of the source and which are not connected to each other. Laurent & Titarchuk (2018) demonstrated a presence of a gravitational redshifted annihilation line emission in a BH using the Monte-Carlo simulations and therefore the observed HBB hump leads us to suggest this feature is a gravitational redshifted annihilation line observed in these black holes. 1 Astro Space Center, Lebedev Physical Institute, Russian Academy of Sciences, Profsouznay ul. 84/32, Moscow 117997, Russia; ltitarchuk@asc.rssi.ru; titarchuk@fe.infn.it Lomonosov Moscow State University/Sternberg Astronomical Institute, Universitetsky Prospect 13, Moscow, 119992, Russia; seif@sai.msu.ru LAPTh, Universite Savoie Mont Blanc, CNRS, B.P. 110, Annecy-le-Vieux F-74941, France; All-Russian Institute of Scientific and Technical Information, RAS, Usievich st. 20, Moscow, 125190, Russia ar X iv :2 01 2. 10 64 5v 1 [ as tr oph .H E ] 1 9 D ec 2 02 0 – 2 – Subject headings: accretion, accretion disks—black hole physics—stars:individual (Cyg X–1, GX 339–4, GRS 1915+105, SS 433, V4641 Sgr):radiation mechanisms: non-thermal—physical data and processes

中文翻译：

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检测黑洞光谱中的高温黑体驼峰。强红移湮灭线

我们在黑洞 (BH) 候选源的宽带 X 射线能谱中发现了一种所谓的高温黑体 (HBB) 分量，它位于 15 – 40 keV 范围内。使用来自五个银河系 BH 双星、Cyg X–1、GX 339–4、GRS 1915+105、SS 433 和 V4641 Sgr 的低/硬、中、高/软的数据提供了对该光谱特征的详细研究和非常软的光谱状态（分别为 LHS、IS、HSS 和 VSS）以及使用 RXTE、INTEGRAL 和 BeppoSAX 数据的它们之间的光谱转换。为了拟合这些源的宽带能谱，我们使用了一个加性 XSPEC 模型，该模型由 Comptonization 分量和高斯线分量组成。特别是，我们发现 IS 光谱具有 HBB 分量，其色温 kTHBB 在 4.5 – 5.9 keV 的范围内。仅在 IS（对于光子指数 Γ > 1.9）使用不同的 X 射线望远镜在这五个源的某些光谱中检测到了这种 HBB 特征。我们还证明了 HBB 特征的时间尺度比铁线及其边缘的时间尺度短几个数量级。这使我们得出结论，这些光谱特征是在源的几何不同部分形成的，并且彼此不相连。Laurent & Titarchuk (2018) 使用蒙特卡罗模拟证明了 BH 中存在引力红移湮灭线发射，因此观察到的 HBB 驼峰使我们认为该特征是在这些黑洞中观察到的引力红移湮灭线。1 天文空间中心，列别杰夫物理研究所，俄罗斯科学院，Profsouznay ul。84/32，莫斯科 117997，俄罗斯；ltitarchuk@asc.rssi.ru; titarchuk@fe.infn.it 罗蒙诺索夫莫斯科国立大学/斯腾堡天文研究所，Universitetsky Prospect 13，莫斯科，119992，俄罗斯；seif@sai.msu.ru LAPTh, Universite Savoie Mont Blanc, CNRS, BP 110, Annecy-le-Vieux F-74941, France; 全俄科学技术信息研究所，RAS，Usievich st。20, Moscow, 125190, Russia ar X iv :2 01 2. 10 64 5v 1 [ as troph .HE ] 1 9 D ec 2 02 0 – 2 – 主题标题：吸积、吸积盘—黑洞物理学—恒星：个体（Cyg X–1、GX 339–4、GRS 1915+105、SS 433、V4641 Sgr）：辐射机制：非热——物理数据和过程 msu.ru LAPTh, Universite Savoie Mont Blanc, CNRS, BP 110, Annecy-le-Vieux F-74941, France; 全俄科学技术信息研究所，RAS，Usievich st。20, Moscow, 125190, Russia ar X iv :2 01 2. 10 64 5v 1 [ as troph .HE ] 1 9 D ec 2 02 0 – 2 – 主题标题：吸积、吸积盘—黑洞物理学—恒星：个体（Cyg X–1、GX 339–4、GRS 1915+105、SS 433、V4641 Sgr）：辐射机制：非热——物理数据和过程 msu.ru LAPTh, Universite Savoie Mont Blanc, CNRS, BP 110, Annecy-le-Vieux F-74941, France; 全俄科学技术信息研究所，RAS，Usievich st。20, Moscow, 125190, Russia ar X iv :2 01 2. 10 64 5v 1 [ as troph .HE ] 1 9 D ec 2 02 0 – 2 – 主题标题：吸积、吸积盘—黑洞物理学—恒星：个体（Cyg X–1、GX 339–4、GRS 1915+105、SS 433、V4641 Sgr）：辐射机制：非热——物理数据和过程