Statistics – Computation
Scientific paper
Jan 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.224..425t&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 224, Jan. 15, 1987, p. 425-434. Research supported by t
Statistics
Computation
21
Computational Astrophysics, Cyclotron Radiation, Emission Spectra, Stellar Mass Accretion, White Dwarf Stars, Absorptivity, Electron Distribution, Maxwell-Boltzmann Density Function, Velocity Distribution
Scientific paper
The cyclotron absorption coefficient for a Maxwellian velocity distribution of electrons are calculated over a wide range of temperatures and frequencies following the method described by Chanmugam (1980). These results are used to determine the range of parameters for a white dwarf accretion column in which a simple steady-state bombardment solution can be found, where the dominant radiative-loss mechanism is optically thick cyclotron radiation. It is shown that for an acceptable choice of accretion parameters a bombardment solution exists with a temperature of about 10 keV, somewhat lower than the shock temperature T(s) of about 30 keV. It is also demonstrated that for parameters for which a simple bombardment model is not valid, the electron temperature (and therefore the observed temperature) will never reach the shock temperature. This leads to a lower hard/soft X-ray ratio than that obtained from the adiabatic shock model - and could thus ease the soft X-ray problem associated with AM Herculis stars.
Cawthorne Timothy V.
Thompson Maggie A.
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