Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989esasp.296..683w&link_type=abstract
In ESA, The 23rd ESLAB Symposium on Two Topics in X Ray Astronomy. Volume 1: X Ray Binaries p 683-688 (SEE N90-25711 19-89)
Astronomy and Astrophysics
Astronomy
Cataclysmic Variables, Hydrodynamics, Shock Waves, Stellar Models, Stellar Radiation, White Dwarf Stars, Star Formation Rate, Stellar Mass Accretion, Stellar Oscillations, X Ray Astronomy
Scientific paper
The stability properties of radiative shocks in spherically symmetric accretion flows onto white dwarfs is discussed. Accretion rates that result in shock thicknesses ranging from thin to settling solutions are investigated. Models for white dwarf masses from 0.3 to 1.2 of the solar mass are presented. The effects of unequal ion and electron temperatures, electron thermal conduction, bremsstrahlung, and Compton cooling are included. It is shown that thick two-temperature shocks are unstable to oscillations in the fundamental mode for white dwarf mass up to and including 1.0 of the solar mass. The possibility that the 0.3 to 1.0 Hz optical Quasi-Periodic Oscillations (QPOs) observed in four AM Her type cataclysmic binaries are due to the first overtone instability. Low accretion rate shock instabilities may be responsible for the tens of seconds to several minute X-ray QPOs observed in some AM Her objects.
Gardner John H.
Imamura James N.
Wolff Michael Thomas
Wood Kent S.
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