Radiation-driven winds from luminous accretion discs

Details Radiation-driven winds from luminous accretion discs Radiation-driven winds from luminous accretion discs

Apr 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mnras.295..595p&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 295, p. 595

Astronomy and Astrophysics

Astronomy

115

Accretion Disks, Stellar Winds, Hydrodynamics, Radiation Pressure, Time Dependence, Cataclysmic Variables

Scientific paper

We study the 2-D, time-dependent hydrodynamics of radiation-driven winds from luminous accretion disks in which the radiation force is mediated primarily by spectral lines. The effect of a radiant central star is included both in modifying the radial temperature profile of the disk and in providing a contribution to the driving radiation field. Our hydrodynamic calculations use nonuniform grids to resolve both the subsonic acceleration zone near the disk and the large-scale global structure of the supersonic wind. We find that line-driven disk winds are produced only when the effective luminosity of the disk exceeds the Eddington limit. If the dominant contribution to the total radiation field comes from the disk, then we find that the outflow is intrinsically unsteady and characterized by large-amplitude velocity and density fluctuations.

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