other query modes : |
Identifier query |
Coordinate query |
Criteria query |
Reference query |
Basic query |
Script submission |
TAP |
Output options |
Object types |
Help |
2006MNRAS.371.1216D - Mon. Not. R. Astron. Soc., 371, 1216-1230 (2006/September-3)
Disc-corona energetics in the very high state of Galactic black holes.
DONE C. and KUBOTA A.
Abstract (from CDS):
However, it is often assumed that the tail is produced by Compton scattering, in which case its shape in these spectra requires that the Comptonizing region is marginally optically thick (τ ∼ 2-3), and covers a large fraction of the inner disc. This will distort our view of the disc, especially of the hottest-temperature material. We build a theoretical model of a Comptonizing corona over an inner disc, and fit this to the data, but find that it still requires a large increase in inner disc radius for a standard disc emissivity. Instead, it seems more probable that the disc emissivity changes in the presence of the corona. We implement the specific inner disc-corona coupling model of Svensson & Zdziarski, in which some fraction f of the accretion power is dissipated in the corona, leaving only a fraction 1 - f to be dissipated in the optically thick disc. We show that this can explain the low-temperature/high-luminosity disc emission seen in the very high state with only a small increase in radius of the disc. While this inferred disc truncation is probably not significant, given the model uncertainties, it is consistent with the low-frequency quasi-periodic oscillation and gives continuity of properties with the low/hard-state spectra.
Abstract Copyright: 2006 The Authors. Journal compilation © 2006 RAS
Journal keyword(s): accretion, accretion discs - black hole physics - radiation mechanisms: thermal - radiative transfer - X-rays: binaries - X-rays: individual: XTE J1550-564
Simbad objects: 2
To bookmark this query, right click on this link: simbad:2006MNRAS.371.1216D and select 'bookmark this link' or equivalent in the popup menu