PX Andromedae and the SW Sextantis phenomenon

Details PX Andromedae and the SW Sextantis phenomenon PX Andromedae and the SW Sextantis phenomenon

Aug 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...431l.107h&link_type=abstract

The Astrophysical Journal, vol. 431, no. 2, pt. 2, p. L107-L110

Other

55

Accretion Disks, Doppler-Fizeau Effect, Novae, White Dwarf Stars, Cataclysmic Variables, Orbital Velocity, Stellar Magnetic Fields

Scientific paper

We show that the emission-line peculiarities of PX And and other SW Sex stars can be explained by an accretion stream which overflows the initial impact with the accretion disk and continues to a later reimpact. The overflowing stream is seen projected against a brighter disk and produces the 'phase 0.5 absorption' features. Emission from the reimpact site produces the high-velocity line wings which alternate from red to blue on the orbital cycle. We conclude that substantial disk overflow is the property distinguishing SW Sex stars from other cataclysmic variables.

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