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2001MNRAS.321..759C - Mon. Not. R. Astron. Soc., 321, 759-766 (2001/March-2)
Soft state of Cygnus X-1: stable disc and unstable corona.
CHURAZOV E., GILFANOV M. and REVNIVTSEV M.
Abstract (from CDS):
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.
Abstract Copyright: 2001, Royal Astronomical Society
Journal keyword(s): accretion, accretion discs - stars: individual: Cygnus X-1 - X-rays: general
Simbad objects: 4
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