Accretion streams in AM HER type systems

Details Accretion streams in AM HER type systems Accretion streams in AM HER type systems

May 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988mnras.232..175m&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 232, May 1, 1988, p. 175-197.

Astronomy and Astrophysics

Astronomy

49

Companion Stars, Magnetic Stars, Stellar Mass Accretion, Stellar Models, Stellar Structure, White Dwarf Stars, Black Body Radiation, Cosmic Gases, Optical Emission Spectroscopy, Roche Limit, Stellar Magnetic Fields, Ultraviolet Spectra, X Rays

Scientific paper

The accretion stream in AM Her type systems is examined through model calculations and observations of the optical and UV emission lines. The magnetospheric radii for two specific systems, ST LMi and QQ Vul, are calculated using system parameters that have been recently obtained from observations. It is shown that the magnetosphere is well within the primary Roche lobe in QQ Vul, but is very close to the L1 point in ST LMi. The shape of the post-shock region is shown to be elongated through model calculations. The size and the blackbody temperature obtained in the models are consistent with the observational constraints available for QQ Vul and ST LMi. The properties of the optical emission lines are re-examined, and it is found that, in many systems, the emission lines have very complex structures with as many as four separate components, whose origin is discussed. The observed soft X-ray component from the white dwarf surface is shown to be sufficient to produce the strong UV emission lines in the magnetically confined stream.

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