General relativistic radiative transfer in spherical flows

Details General relativistic radiative transfer in spherical flows General relativistic radiative transfer in spherical flows

Dec 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988mnras.235.1273t&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 235, Dec. 15, 1988, p. 1273-1285. Research supported by

Statistics

Computation

25

Computational Astrophysics, Numerical Integration, Radiative Transfer, Relativistic Effects, Accretion Disks, Black Holes (Astronomy), Gas Flow, Luminosity, Photosphere

Scientific paper

An analysis of Thorne's (1981) structure equations governing radiation field moments is presented in the case of stationary spherically symmetric flows. It is shown that the truncated system of moment equations must be solved subject to boundary conditions, and a number of critical points equal to the truncation order l(max) arise. The moment formalism can be made tractable by introducing a suitable closure assumption for moments of order higher than l(max), which gives a satisfactory description of the radiation field in the whole range of optical depth even for small values of l(max). A sample numerical integration of the moment equations is performed for a spherical accreting flow with an assigned velocity and temperature profile.

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