Physics
Scientific paper
Jan 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...276..667i&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 276, Jan. 15, 1984, p. 667-676.
Physics
81
Flow Stability, Radiative Transfer, Shock Waves, Stellar Mass Accretion, Stellar Models, White Dwarf Stars, Bremsstrahlung, Cooling, Oscillations, Shock Wave Propagation, Thermal Conductivity
Scientific paper
Attention 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.
Durisen Richard H.
Imamura James N.
Wolff Michael Thomas
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