Structure of accretion flows in the nova-like cataclysmic variable RW Tri

Abstract

We obtained photometric observations of the nova-like cataclysmic variable RW Tri and gathered all available AAVSO and other data from the literature. We determined the system parameters and found their uncertainties using the code developed by us to model the light curves of binary systems. New time-resolved optical spectroscopic observations of RW Tri were also obtained to study the properties of emission features produced by the system. The usual interpretation of the single-peaked emission lines in nova-like systems is related to the bi-conical wind from the accretion disc's inner part. However, we found that the Halpha emission profile is comprised of two components with different widths. We argue that the narrow component originates from the irradiated surface of the secondary, while the broader component's source is an extended, low-velocity region in the outskirts of the accretion disc, located opposite to the collision point of the accretion stream and the disc. It appears to be a common feature for long-period nova-like systems -- a point we discuss.

14 pages, 8 figures, Accepted to MNRAS

References in corpus (8)

• SW Sextantis stars: the dominant population of CVs with orbital periods between 3-4 hours
• The Geometry and Ionization Structure of the Wind in the Eclipsing Nova-like Variables RW Tri and UX UMa
• The structure of accretion flows in nova-like cataclysmic variables: RW Sextantis and 1RXS J064434.5+334451
• Novalike Cataclysmic Variables in the Infrared
• Analysis of spiral structure in the accretion disc of the novalike Cataclysmic Variable EC21178--5417
• A possible giant planet orbiting the cataclysmic variable LX Ser
• Doppler Tomography and Photometry of the Cataclysmic Variable 1RXS J064434.5+334451
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• The period bouncer system SDSS J105754.25+275947.5: first radial velocity study
• Structure of the accretion flow of IX Velorum as revealed by high-resolution spectroscopy