Hydrogen line emission from optically thin accretion disks

Details Hydrogen line emission from optically thin accretion disks Hydrogen line emission from optically thin accretion disks

Mar 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...326..738w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 326, March 15, 1988, p. 738-750.

Mathematics

Probability

30

Accretion Disks, Cataclysmic Variables, H Lines, Nonequilibrium Thermodynamics, Stellar Radiation, Balmer Series, Dwarf Novae, Helium, Hydrogen Atoms

Scientific paper

The results of a non-LTE accretion disk model for the calculation of hydrogen line emission from regions of a disk which are optically thin in the continuum are presented. Each model calculated would apply to only one annulus radially outward in a real accretion disk. The vertical density structure in the disk is treated properly, and the transfer of line radiation is done using the escape probability formalism. The results indicate that the observed Balmer decrements are functions of the density in the disk. Flat Balmer decrements from the disk as a whole are still expected, however, as the decrements are near unity as the disk becomes optically thick in the continuum. Line profiles are presented and show that a double-peaked structure is expected even for disks viewed face-on.

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