UV line diagnostics of accretion disk winds in cataclysmic variables

Details UV line diagnostics of accretion disk winds in cataclysmic variables UV line diagnostics of accretion disk winds in cataclysmic variables

Feb 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992llnl.rept.....v&link_type=abstract

Final Report, 1 Sep. 1990 - 29 Feb. 1992 Lawrence Livermore National Lab., CA. Physics Dept.

Physics

Accretion Disks, Cataclysmic Variables, Line Spectra, Photoionization, Solar Wind, Stellar Mass Accretion, Ultraviolet Spectra, Boundary Layers, Cygnus Constellation, Data Bases, Eclipses, Emission Spectra, Iue, Mass Distribution, Radiative Transfer, Rotation, Solar Spectra

Scientific paper

The IUE data base is used to analyze the UV line shapes of cataclysmic variables RW Sex, RW Tri, and V Sge. Observed lines are compared to synthetic line profiles computed using a model of rotating bi-conical winds from accretion disks. The wind model calculates the wind ionization structure self-consistently including photoionization from the disk and boundary layer and treats 3-D line radiation transfer in the Sobolev approximation. It is found that winds from accretion disks provide a good fit for reasonable parameters to the observed UV lines which include the P Cygni profiles for low inclination systems and pure emission at large inclination. Disk winds are preferable to spherical winds which originate on the white dwarf because they (1) require a much lower ratio of mass loss rate to accretion rate and are therefore more plausible energetically, (2) provide a natural source for a bi-conical distribution of mass outflow which produces strong scattering far above the disk leading to P Cygni profiles for low inclination systems, and pure line emission profiles at high inclination with the absence of eclipses in UV lines, and (3) produce rotation broadened pure emission lines at high inclination.

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