Stationary spherical accretion into black holes - The transition from the optically thin to the optically thick regime

Details Stationary spherical accretion into black holes - The transition from the optically thin to the optically thick regime Stationary spherical accretion into black holes - The transition from the optically thin to the optically thick regime

Dec 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...116..111s&link_type=abstract

Astronomy and Astrophysics, vol. 116, no. 1, Dec. 1982, p. 111-116.

Astronomy and Astrophysics

Astronomy

8

Astronomical Models, Black Holes (Astronomy), Magnetohydrodynamic Flow, Optical Thickness, Radiative Transfer, B Stars, Mass Transfer, O Stars, Schwarzschild Metric, Ultraviolet Radiation

Scientific paper

Models are developed for the spherical accretion of fully ionized and unmagnetized hydrogen gas onto a Schwarzschild black hole with a mass (M) in the range from 1 to 1000 solar masses. It is assumed that the gas far from the black hole (i.e., at infinity) remains ionized, is maintained at a temperature of 10,000 K by UV radiation from nearby OB stars, and has a density (n) in the range from 1 per cu cm to (10 billion/M) per cu cm. It is found that, as n is increased through the specified range, the gas undergoes a transition from being optically thin everywhere to having a photosphere between the black hole's event horizon and the accretion radius and then a transition to being optically thick everywhere. The accretion rate, the luminosity of the infalling gas, and the radiation temperature are evaluated as functions of the baryon number density at infinity for a black hole of 1 solar mass.

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