The outflowing regime of quasi-spherical accretion on to X-ray compact objects

Details The outflowing regime of quasi-spherical accretion on to X-ray compact objects The outflowing regime of quasi-spherical accretion on to X-ray compact objects

Feb 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993mnras.260..727i&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 260, no. 4, p. 727-764.

Astronomy and Astrophysics

Astronomy

13

Accretion Disks, Black Holes (Astronomy), Luminous Intensity, X Ray Sources, Compton Effect, Gas Flow, Stellar Mass Accretion, X Ray Binaries

Scientific paper

We study numerically the quasi-spherical accretion of matter on to a relativistic object with anisotropic X-ray luminosity which is powered by mass accretion. The X-rays heat the accreting gas through Compton scattering. When the gas temperature increases above the local escape temperature, part of the accreting gas will flow outwards as a result of the action of buoyancy force. The direction of the outflow coincides with the maximum of the X-ray luminosity. The depth of outflow as well as the velocity of the stream is correlated with the energy of X-ray quanta. The outflow exists persistently, but the mass-loss rate in the outflow is highly variable (about 50 percent). In spite of its quantum nature, Compton heating markedly affects the gas, forcing the matter outflow at X-ray luminosities as small as three orders of magnitude less than the Eddington limit. The phenomenon of hot gas outflow takes place in the case of accretion on to a wind-fed X-ray source (neutron star or black hole) in a wide binary and in the case of a supermassive black hole in an active galactic nucleus (QSO or Seyfert).

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