How Do We See a Relativistic Accretion Disk during a Thermal Instability
How Do We See a Relativistic Accretion Disk during a Thermal Instability
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DOI：
10.1093/pasj/58.2.477
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发表时间：
2006-03
影响因子：
2.3
通讯作者：
Akihiro Kawata;Ken-ya WataraiJun Fukue
中科院分区：
文献类型：
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作者：
Akihiro Kawata;Ken-ya WataraiJun Fukue
我们计算了辐射压力驱动的热不稳定性过程中相对论性薄盘的辐射热图像。当质量吸积率超过临界吸积率时，标准吸积盘的内部区域发生爆炸，变成具有大尺度高度的细长盘状态。也就是说，盘的内部区域变得高温，并且盘的厚度由于辐射压力的增加而增加。结果发现，在爆发期间观察到的盘的图像强烈地依赖于倾斜角。也就是说，从最里面的磁盘的辐射将被掩盖的磁盘外缘为高倾角（i ;2：，70 0）。我们还计算了热不稳定性时的光谱能量分布。由于几何厚度的影响，高倾角谱的Wien峰比低倾角谱的Wien峰变得更软。从这些事实来看，即使在黑洞候选者中发生了爆发，当倾斜角很大时，我们也可能观察不到爆发。我们可能认为，在我们的银河系中仍然隐藏着许多发光的黑洞候选者。
We calculated bolometric images of relativistic slim disks during a radiation-pressure-driven thermal instability. When the mass-accretion rate exceeds the critical one, an inner region of the standard accretion disk bursts to change to a slim disk state having a large scale height. That is, the inner region of the disk becomes high temperature, and the thickness of the disk increases due to an increase of the radiation pressure. As a result, we found that the observed image of the disk during the burst strongly depends on the inclination angle. That is, radiation from the innermost disk would be occulted by the disk outer rim for high inclination angles (i ;2:, 70 0 ). We also calculated the spectral energy distribution during a thermal instability. The Wien peak of the spectrum of high inclination angles becomes softer than that of low inclination angles due to the geometrical thickness. From these facts, even if a burst occurs in a black-hole candidate, we may not observe the burst when the inclination angle is large. We may suggest that numerous luminous black-hole candidates are still hidden in our Galaxy.