论文标题
Seyfert 1 Galaxy WKK 4438中的截短内盘
A truncated inner disc in the Seyfert 1 galaxy WKK 4438
论文作者
论文摘要
理解积聚光盘是否延伸到最内向的稳定圆形轨道（ISCO）是否很重要，因为它是测量黑洞旋转的基本假设。在这里，我们检查了狭窄的Seyfert 1 Galaxy，WKK 4438的2013年和2018年Nustar和Swift数据（0.5-50 KEV）。X射线发射可以很好地拟合，该X射线发射可与描述Corona和模糊的模型一起拟合，并模糊地反射，该反射来自围绕Low Spin（A* 〜0）黑色孔的光盘。但是，这样的模型导致某些参数的非常规值（例如，倒发率和高冠状高度）。另外，如果将圆盘在〜10 rg处截断并且黑洞以索恩极限旋转（a* = 0.998），则可以实现同样好的拟合。在这些情况下，模型参数与电晕位于靠近黑洞并在较大距离的圆盘上的解释是一致的。
Understanding if and when the accretion disc extends down to the innermost stable circular orbit (ISCO) is important since it is the fundamental assumption behind measuring black hole spin. Here, we examine the 2013 and 2018 NuSTAR and Swift data (0.5 - 50 keV) of the narrow-line Seyfert 1 galaxy, WKK 4438. The X-ray emission can be fitted well with models depicting a corona and blurred reflection originating from a disc around a low spin (a* ~ 0) black hole. However, such models result in unconventional values for some of the parameters (e.g. inverted emissivity profile and high coronal height). Alternatively, equally good fits can be achieved if the disc is truncated at ~10 rg and the black hole is spinning at the Thorne limit (a* = 0.998). In these cases, the model parameters are consistent with the interpretation that the corona is centrally located close to the black hole and illuminating the disc at a larger distance.
