Accretion and radiation spectrum of the gas debris of a star disrupted by the tidal forces of a massive black hole

Details Accretion and radiation spectrum of the gas debris of a star disrupted by the tidal forces of a massive black hole Accretion and radiation spectrum of the gas debris of a star disrupted by the tidal forces of a massive black hole

Jun 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....86..315g&link_type=abstract

Astronomy and Astrophysics, vol. 86, no. 3, June 1980, p. 315-320.

Astronomy and Astrophysics

Astronomy

26

Black Holes (Astronomy), Gravitational Effects, Interstellar Gas, Stellar Mass Accretion, Stellar Mass Ejection, Stellar Spectra, Galactic Nuclei, Stellar Radiation, Tides

Scientific paper

When the sustenance of the black hole of a mass Mh situated at the centre of the galactic nucleus is provided mainly by tidal disruptions of surrounding stars (this holds if 103-104 Msun < Mh < 3 108 Msun) the accretion of the gas debris of a star proceeds in a disk regime if Mh is smaller than some critical value Mcr ≍ 105 Msun. In this case the viscous evolution time-scale of the disk is smaller than the time interval between two successive star breakups, and the accretion has a non-stationary character. On the basis of the non-stationary disk model, first considered by Lynden-Bell and Pringle (1974), the main parameters of the disk debris of a disrupted star are obtained as a function of time, including the accretion luminosity of the disk. During a significant part of its evolution the disk is strongly heated by viscous energy dissipation and should be seen as an intense source of X-ray radiation.
As an example of the possible use of the non-stationary model developed, we apply it to obtain a new upper limit to the mass of a black hole presumed located at the centre of our Galaxy. Comparing the X-ray luminosity of the disk with the upper limit to the X-ray flux from the "point" source at the Galactic centre, we find that the mass of the black hole does not exceed about 6 102 Msun.

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