Radiation hydrodynamics of high-luminosity accretion into black holes

Details Radiation hydrodynamics of high-luminosity accretion into black holes Radiation hydrodynamics of high-luminosity accretion into black holes

Jun 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978ap%26ss..56..191s&link_type=abstract

Astrophysics and Space Science, vol. 56, no. 1, June 1978, p. 191-218.

Astronomy and Astrophysics

Astronomy

46

Black Holes (Astronomy), Hydrodynamics, Interstellar Gas, Stellar Luminosity, Stellar Mass Accretion, Gas Density, Radiative Heat Transfer, Stellar Atmospheres, Synchrotron Radiation

Scientific paper

Previous computations of the emission of free-free and synchrotron radiation from optically thin gas accreting onto black holes are extended to the regime of nonvanishing optical depth. The problem of radiative transfer is solved in conjunction with the hydrodynamics of the gas flow by adjusting a method usually applied to the determination of radiation fields in spherically symmetric stellar atmospheres to treat transfer problems in general isotropic metrics and, in particular, the Schwarzschild metric. Primary attention is focused on those spherically symmetric configurations whose emergent photon fluxes are expected to be high; temperature stratifications, luminosities, and emergent spectra are calculated for such configurations. Numerical results are presented for black holes of 10 to 100,000 solar masses embedded in interstellar gas with varied density and temperature. The maximum luminosity that a black hole of given mass may generate by spherically symmetric accretion is determined, and the possibility of observing such accretion onto black holes is considered.

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