Structure of accretion flows in the nova-like cataclysmic variable RW Tri
Subebekova, G.; Zharikov, S.; Tovmassian, G.; Neustroev, V.; Wolf, M.; Hernandez, M.-S.; Kučáková, H.; Khokhlov, S. (2020-07-20)
G Subebekova, S Zharikov, G Tovmassian, V Neustroev, M Wolf, M-S Hernandez, H Kučáková, S Khokhlov, Structure of accretion flows in the nova-like cataclysmic variable RW Tri, Monthly Notices of the Royal Astronomical Society, Volume 497, Issue 2, September 2020, Pages 1475–1487, https://doi.org/10.1093/mnras/staa2091
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
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https://urn.fi/URN:NBN:fi-fe2020120499521
Tiivistelmä
Abstract
We obtained photometric observations of the nova-like (NL) 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 NL systems is related to the bi-conical wind from the accretion disc’s inner part. However, we found that the Hα 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 NL systems — a point we discuss.
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