Open AccessSoft state of Cygnus X‐1: stable disc and unstable corona
Author(s) -
Churazov E.,
Gilfanov M.,
Revnivtsev M.
Publication year - 2001
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2001.04056.x
Subject(s) - physics , astrophysics , accretion (finance) , corona (planetary geology) , aperiodic graph , accretion disc , amplitude , spectral line , flux (metallurgy) , thin disk , black hole (networking) , power law , astronomy , galaxy , optics , computer network , routing protocol , statistics , materials science , mathematics , routing (electronic design automation) , combinatorics , astrobiology , venus , computer science , metallurgy , link state routing protocol
Two‐component X‐ray spectra (soft multicolour black‐body and harder power law) are frequently observed from accreting black holes. These components are presumably associated with the different parts of the accretion flow (optically thick and optically thin respectively) in the vicinity of the compact source. Most of the aperiodic variability of the X‐ray flux on the short time‐scales is associated with the harder component. We suggest that drastically different amplitudes of variability of these two components are simply related to the very different viscous time‐scales in the geometrically thin and geometrically thick parts of the accretion flow. In the geometrically thin discs, variations of viscosity or mass accretion rate occurring at large radius from the black hole on the local dynamical or thermal time‐scales do not cause any significant variations of the mass accretion rate at smaller radii because of a very long diffusion time. Any variations on the time‐scales shorter than the diffusion time‐scale are effectively dampened. On the contrary such variations can easily survive in the geometrically thick flows and as a result the mass accretion rate in the innermost region of the flow will reflect modulations of the mass accretion rate added to the flow at any distance from the black hole. Therefore if primary instabilities operate on the short time‐scales then the stability of the soft component (originating from the geometrically thin and optically thick flow) and variability of the hard component (coming from the geometrically thick and optically thin flow) are naturally explained. For Cygnus X‐1, the overall shape of the power density spectra (PDS) in the soft and hard spectral states can be qualitatively explained if the geometrically thin disc is sandwiched by the geometrically thick corona extending in a radial direction up to a large distance from the compact object. In the hard state the thin disc is truncated at some distance from the black hole followed by the geometrically thick flow. The break in the PDS is then associated with the characteristic frequencies in the accretion flow at the thin disc truncation radius.