On The Accretion Rates of SW Sextantis Nova-Like Variables

Abstract

We present accretion rates for selected samples of nova-like variables having IUE archival spectra and distances uniformly determined using an infrared method by Knigge (2006). A comparison with accretion rates derived independently with a multi-parametric optimization modeling approach by Puebla et al.(2007) is carried out. The accretion rates of SW Sextantis nova-like systems are compared with the accretion rates of non-SW Sextantis systems in the Puebla et al. sample and in our sample, which was selected in the orbital period range of three to four and a half hours, with all systems having distances using the method of Knigge (2006). Based upon the two independent modeling approaches, we find no significant difference between the accretion rates of SW Sextantis systems and non-SW Sextantis nova-like systems insofar as optically thick disk models are appropriate. We find little evidence to suggest that the SW Sex stars have higher accretion rates than other nova-like CVs above the period gap within the same range of orbital periods.

Accepted for publication by the Astrophysical Journal, 2009

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• An International Ultraviolet Explorer Archival Study of Dwarf Novae in Outburst
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• Novalike Cataclysmic Variables in the Infrared
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• Multiwavelength Photometry and Hubble Space Telescope Spectroscopy of the Old Nova V842 Centaurus
• XMM-Newton Observations of the Peculiar Cataclysmic Variable Lanning 386: X-ray evidence for a Magnetic Primary
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• Confirmation of SRGt 062340.2-265751 as a nova-like cataclysmic variable with a possible magnetic nature