How to distinguish between different models of accretion flow in low/hard state of accreting black holes?

被引：0
|
作者：
Zycki, PT [1 ]
机构：
[1] Copernicus Astron Ctr, PL-00716 Warsaw, Poland
来源：
NEW CENTURY OF X-RAY ASTRONOMY | 2001年 / 251卷
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中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
The basic spectral properties of low/hard state (LS) of accreting black holes: the range of spectral index, amplitude of the reprocessed component, relativistic smearing of the latter, and correlations between those parameters, permit construction of a number of models for geometry/physical properties of the accretion flow. These belong to two main groups: (1) models with the standard accretion disk truncated at certain radius, with central hot, optically thin X-ray emitting flow, possibly mixed with small cloud(let)s, and (2) models with the accretion disk extending all the way to the last stable orbit, with either a relativistic outflow of the X-ray emitting plasma, or a hot skin on top of the disk. The models should be distinguishable, if their predictions, both in spectral and time variability domains are constructed, and compared with good quality data. Here, a number of examples of such predictions are presented for the "hot skin" model.
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页码：430 / 431
页数：2
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