Model of bimodal behavior of Cygnus X-1

Details Model of bimodal behavior of Cygnus X-1 Model of bimodal behavior of Cygnus X-1

Aug 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986esasp.251..563c&link_type=abstract

In ESA Proceedings of the Joint Varenna-Abastumani International School and Workshop on Plasma Astrophysics p 563-568 (SEE N87-

Astronomy and Astrophysics

Astronomy

3

Accretion Disks, Black Holes (Astronomy), Cygnus Constellation, Stellar Models, X Ray Sources, Free Convection, Stellar Magnetic Fields, Stellar Mass Accretion

Scientific paper

A model of the accretion disk for Cygnus X-1 is developed. The model explains the existence of two different (high and low) states of the disk depending on accretion rate (M). It is shown that in the absence of thermal convection in the disk middle region, the matter is not able to supply a sufficiently strong large scale magnetic field to the disk inner region, thus, the field has no time to reach appreciable values. Matter accretion proceeds without magnetic field, mainly in accordance with the standard model of accretion, and the high state is realized. At decreasing M, thermal convection, having helical character, appears in the disk middle region. Therefore, large scale magnetic field generation may occur long before matter comes into the disk inner region. Under these conditions, magnetic forces in the maximum energy release region becoming strong generate Raleigh-Taylor instability. Optically thin hot corona are formed, required for the explanation of the power law spectrum of X-ray photons in the low state.

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