Towards a self-consistent description of accretion columns. IV - Iterative scattering solution of radiative transfer and effects of bulk motion

Details Towards a self-consistent description of accretion columns. IV - Iterative scattering solution of radiative transfer and effects of bulk motion Towards a self-consistent description of accretion columns. IV - Iterative scattering solution of radiative transfer and effects of bulk motion

Oct 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...223..251m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 223, no. 1-2, Oct. 1989, p. 251-257. Research supported by DFG.

Astronomy and Astrophysics

Astrophysics

3

Accretion Disks, Pulsars, Radiative Transfer, Scattering, X Ray Binaries, Astronomical Models, Iteration, Photons, Radiation Distribution, Relativistic Effects, Stellar Mass Accretion

Scientific paper

A solution of the radiative transfer problem in relativistic flows is obtained by computing successive scatterings of photons, and a method is presented for solving the coherent, time-independent transfer equation including the relativistic motion of matter in an accretion flow. An iterative scattering algorithm (ISA) is developed for a two-dimensional geometry and full angular dependence of the radiation intensity. The method works efficiently for layers of small or moderate optical thickness. To study the consequences of bulk motion, the ISA is applied to a simplified model of an X-ray pulsar accretion column. In the model of the accretion column, isotropic scattering coefficients are used for the radiative transfer calculations. It is found that the X-rays, originally produced in the hot spot, only can escape efficiently in that energy range for which the column is optically thin. Photons scattered within the column will be dragged down with the infalling matter; thus they will be scattered back into the hot spot within a few scatterings.

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