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Structure and evolution of irradiated accretion disks. I - Static thermal equilibrium structure. II - Dynamical evolution of a thermally unstable torusThe thermal equilibrum structure and dynamical behavior of externally irradiated accretion disks are investigated. For radiative disks only the surface layer is heated, while for convective disks the heat penetrates deeply into the disk. For sufficiently strong radiation and given irradiation flux F(irr), the disk is completely stabilized against thermal instabilities of the sort invoked to explain dwarf novae. For moderately strong irradiation there is still an unstable branch in the thermal equilibrium curve. In typical soft X-ray transients, the disk is unstable against the dwarf-nova type instability. Fixed F(irr) on accretion disk annuli reduces the amplitude and the quiescent times and increases the outburst duration of the resultant light curves. Varying F(irr) in proportion to the mass accretion rate at the disks's inner edge results in light curves with a plateau in the decay from outbursts. In the case when irradiation is suddenly switched on, a temperature inversion results which leads to the formation of an accretion corona.
Document ID
19900056915
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Tuchman, Y.
(Texas Univ. Austin, TX, United States)
Mineshige, S.
(Texas Univ. Austin, TX, United States)
Wheeler, J. C.
(Texas, University Austin, United States)
Date Acquired
August 14, 2013
Publication Date
August 10, 1990
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 359
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
90A43970
Funding Number(s)
CONTRACT_GRANT: DE-FG05-80ET-53088
CONTRACT_GRANT: NSG-7232
CONTRACT_GRANT: NSF AST-87-17166
Distribution Limits
Public
Copyright
Other

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