University of Oulu

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,

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

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Author: Subebekova, G.1; Zharikov, S.2; Tovmassian, G.2;
Organizations: 1Al-Farabi Kazakh National University, Al-Farabi Ave., 71, 050040 Almaty, Kazakhstan
2Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 877, Ensenada, 22800 Baja California, México
3Space Physics and Astronomy research unit, University of Oulu, PO Box 3000, FIN-90014 Oulu, Finland
4Astronomical Institute, Faculty of Mathematics and Physics, Charles University, V Holešovičkách 2, CZ-180 00 Praha 8, Czech Republic
5Instituto de Física y Astronomía, Universidad de Valparaíso, Av. Gran Bretaña, 1111 Valparaíso, Chile
6Astronomical Institute, Academy of Sciences, Fričova 298, CZ-251 65, Czech Republic
7Research Centre for Theoretical Physics and Astrophysics, Institute of Physics, Silesian University in Opava, Bezručovo nám. 13, CZ-746 01 Opava, Czech Republic
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Version: published version
Access: open
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Language: English
Published: Oxford University Press, 2020
Publish Date: 2020-12-04


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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Series: Monthly notices of the Royal Astronomical Society
ISSN: 0035-8711
ISSN-E: 1365-8711
ISSN-L: 0035-8711
Volume: 497
Issue: 2
Pages: 1475 - 1487
DOI: 10.1093/mnras/staa2091
Type of Publication: A1 Journal article – refereed
Field of Science: 115 Astronomy and space science
Funding: SZ and VN acknowledge the financial support from the visitor and mobility program of the Finnish Centre for Astronomy with ESO (FINCA), funded by the Academy of Finland grant no 306531. M-SH acknowledges the Fellowship for National PhD from ANID, grant number 21170070. The research of MW was supported by the project Progress Q47 Physics of the Charles University in Prague.
Copyright information: 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.