Fast variation of Cygnus X-1 and related sources

Details Fast variation of Cygnus X-1 and related sources Fast variation of Cygnus X-1 and related sources

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...347.1100c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 347, Dec. 15, 1989, p. 1100-1106.

Astronomy and Astrophysics

Astrophysics

12

Accretion Disks, Stellar Radiation, Variable Stars, X Ray Binaries, Magnetohydrodynamics, Stellar Models, Stellar Rotation

Scientific paper

A new model is offered for explaining the millisecond variability of Cyg X-1 and related sources, based on the bimodal accretion model for Cyg X-1. In the region of the main energy, release action of the Parker instability leads to the formation of three to five (depending on concrete circumstances) oblong-shaped magnetic arcs within the whole azimuth. Those are the magnetic arcs which make up, consequently, an optically thin hot corona needed for explaining the 'low' state spectrum of Cyg X-1. Rapid rotation of the stretched magnetic arcs leads to fast variations of their lengths scales along the line of sight. Accordingly, the optical depth of each arc with respect to Thomson scattering, tau, will also vary, leading to the variations of spectral indices of arcs determined in terms of tau for the inverse Compton scattering. In its turn, it leads to rapid variations of photon count rates in the proper energy range. The described mechanism is effective when n = 3 (n is the number of arcs) but for n = 5 it is essentially weakened; i.e., in the latter case fast variations are actually absent.

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