THICK ACCRETION DISK MODEL FOR ULTRALUMINOUS SUPERSOFT SOURCES
THICK ACCRETION DISK MODEL FOR ULTRALUMINOUS SUPERSOFT SOURCES
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DOI：
10.3847/2041-8205/818/1/l4
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发表时间：
2016-01
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影响因子：
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通讯作者：
Weimin Gu;Mouyuan Sun;Youjun Lu;F. Yuan;Jifeng Liu
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作者：
Weimin Gu;Mouyuan Sun;Youjun Lu;F. Yuan;Jifeng Liu
我们提出了一个几何厚的超爱丁顿吸积盘模型，其中不需要光学厚风，以理解超铝超软源(ULSS)。对于较高的质量吸积率M·≳30M·Edd>；和不小的倾角θ≳25°？>；，其中M·Edd>；是爱丁顿吸积率，来自热的内区的硬光子可能被几何厚度的内盘遮蔽，因此只有来自外薄盘和厚盘外光球的软光子才能到达观测者。我们的模型可以很自然地解释典型热半径与热温度R_bB_∝_T_B_b_−_2？此外，厚盘模型可以统一ULSS和正常超亮度X射线源，不同的观测特征可能与倾角和质量吸积率有关。通过将我们的模型与光学厚度外流模型进行比较，我们发现我们的模型需要较低的质量吸积率。
We propose a geometrically thick, super-Eddington accretion disk model, where an optically thick wind is not necessary, to understand ultraluminous supersoft sources (ULSs). For high mass accretion rates M ˙ ≳ 30 M ˙ Edd ?> and not small inclination angles θ ≳ 25 ° ?> , where M ˙ Edd ?> is the Eddington accretion rate, the hard photons from the hot inner region may be shaded by the geometrically thick inner disk, and therefore only the soft photons from the outer thin disk and the outer photosphere of the thick disk can reach the observer. Our model can naturally explain the approximate relation between the typical thermal radius and the thermal temperature, R bb ∝ T bb − 2 ?> . Moreover, the thick disk model can unify ULSs and normal ultraluminous X-ray sources, where the different observational characteristics are probably related to the inclination angle and the mass accretion rate. By comparing our model with the optically thick outflow model, we find that a lower mass accretion rate is required in our model.