期刊
ASTRONOMY & ASTROPHYSICS
卷 521, 期 -, 页码 -出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201014467
关键词
black hole physics; accretion, accretion disks
资金
- Polish Ministry of Science [N203 0093/1466, N203 304035, N203 380336, N203 00832/0709]
- Department of Astronomy at Kyoto University
- Czech government [MSM 4781305903]
- French Space Agency CNES
The radiation inner edge of an accretion disk is defined as the inner boundary of the region from which most of the luminosity emerges. Similarly, the reflection edge is the smallest radius capable of producing a significant X-ray reflection of the fluorescent iron line. For black hole accretion disks with very sub-Eddington luminosities these and all other inner edges coexist at the innermost stable circular orbit (ISCO). Thus, in this case, one may rightly consider ISCO as the unique inner edge of the black hole accretion disk. However, even at moderate luminosities, there is no such unique inner edge because differently defined edges are located at different places. Several of them are significantly closer to the black hole than ISCO. These differences grow with the increasing luminosity. For nearly Eddington luminosities, they are so huge that the notion of the inner edge loses all practical significance.
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