Figure 7: The innermost part of the disk. In the Shakura–Sunyaev and Novikov–Thorne models,
the locations of the maximum pressure (a.k.a. the center) and the cusp , as well
as the sonic radius , are assumed to coincide with the ISCO. Furthermore, the angular
momentum is assumed to be strictly Keplerian outside the ISCO and constant inside it. In real
flows, , and angular momentum is super-Keplerian between
and . Image reproduced by permission from [9], copyright by ESO.
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