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

May 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...280..734s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 280, May 15, 1984, p. 734-743.

Mathematics

Logic

24

Binary Stars, K Lines, Stellar Mass Accretion, White Dwarf Stars, X Ray Spectra, Albedo, Bremsstrahlung, Cyclotron Radiation, Monte Carlo Method, Optical Polarization, Stellar Luminosity

Scientific paper

Phenomenological fits to the hard X-ray spectrum of AM Hercules have failed to explain the high equivalent width (0.8 + or - 0.1 keV) of Fe K-alpha emission. The scattering and fluorescent line production in a cold or partially ionized accretion column of hard X-rays emitted at the base are investigated using the Monte Carlo method. It is shown that the Fe emission equivalent width observed in the spectrum of AM Her can be explained without resorting to an overabundance of Fe in the accreting material. For sufficient optical depth across the accretion column, equivalent widths of K-alpha emission even larger than the observed values can be obtained. 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.

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