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A numerical study of the stability of radiative shocksAttention is given to the oscillatory instability of optically thin radiative shocks in time-dependent numerical calculations of accretion flows onto degenerate dwarfs. The present nonlinear calculations yield good quantitative agreement with the linear results obtained for oscillation frequencies, damping rates, and critical alpha-values. The fundamental mode and the first overtone in the shock radius and luminosity variations can be clearly identified, and evidence is sometimes seen for the second overtone. Time-dependent calculations are also performed which include additional physics relevant to degenerate dwarf accretion, such as electron thermal conduction, unequal electron and ion temperatures, Compton cooling, and relativistic corrections to the bremsstrahlung cooling law. All oscillatory modes are found to be damped, and hence stable, in the case of a 1-solar mass white dwarf accreting in spherical symmetry.
Document ID
19840039143
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Imamura, J. N. (Virginia, University Charlottesville, VA, United States)
Wolff, M. T. (Virginia Univ. Charlottesville, VA, United States)
Durisen, R. H. (Indiana University Bloomington, IN, United States)
Date Acquired
August 12, 2013
Publication Date
January 15, 1984
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 276
ISSN: 0004-637X
Subject Category
ASTROPHYSICS
Funding Number(s)
CONTRACT_GRANT: NAG8-362
CONTRACT_GRANT: NSF AST-80-19569
Distribution Limits
Public
Copyright
Other