Models of the hard X-ray spectrum of AM Herculis and implications for the accretion rate

Details Models of the hard X-ray spectrum of AM Herculis and implications for the accretion rate Models of the hard X-ray spectrum of AM Herculis and implications for the accretion rate

Dec 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983stin...8418123s&link_type=abstract

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Mathematics

Logic

Rates (Per Time), Stellar Mass Accretion, Stellar Spectra, White Dwarf Stars, X Ray Spectra, Bremsstrahlung, Emission Spectra, Fluorescence, Iron, Monte Carlo Method, Stellar Gravitation

Scientific paper

Phenomenological fits to the hard X-ray spectrum of AM Herculis left unexplained the high equivalent width (0.8 + or - 0.1 keV) of Fe K alpha emission. A purely thermal origin implies a much steeper spectrum than was observed. With Monte Carlo calculations, scattering and fluorescent line production in a cold or partially ionized accretion column of hard X-rays emitted at the base were investigated. The strength of the iron emission and the flat spectral continuum can be explained by the effects of fluorescence and absorption within the accretion column and the surface of the white dwarf on a thermal X-ray spectrum. Thomson optical depths across the column in the range 0.2 to 0.7 are acceptable. The accretion rate and gravitational power can be deduced from the optical depth across the column, if the column size is known, and, together with the observed hard X-ray and polarized light luminosities, imply a lower limit for the luminosity in the UV to soft X-ray range, for which the observations give model-dependent values. Estimates of the column size differ by a factor of 40. Small spot sizes and low luminosities would be consistent with the soft component being the expected reprocessed bremsstrahlung and cyclotron radiation, although the constraint of matching the spectrum confines one to solutions with fluxes exceeding 20% the Eddington limits.

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