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

@article{49323,
   author = {Subebekova, G. and Zharikov, S. and Tovmassian, G. and Neustroev, V. and Wolf, M. and Hernandez, MandS and Kučáková, Hana and Khokhlov, S.},
   article_number = {2},
   doi = {http://dx.doi.org/10.1093/mnras/staa2091},
   keywords = {binaries: spectroscopic; stars: individual: RW Tri; novae; cataclysmic variables},
   language = {eng},
   issn = {0035-8711},
   journal = {Monthly Notices of the Royal Astronomical Society},
   title = {Structure of accretion flows in the nova-like cataclysmic variable RW Tri},
   url = {https://academic.oup.com/mnras/article-abstract/497/2/1475/5873686?redirectedFrom=fulltext},
   volume = {497},
   year = {2020}
}

TY  - JOUR
ID  - 49323
AU  - Subebekova, G. - Zharikov, S. - Tovmassian, G. - Neustroev, V. - Wolf, M. - Hernandez, M-S - Kučáková, Hana - Khokhlov, S.
PY  - 2020
TI  - Structure of accretion flows in the nova-like cataclysmic variable RW Tri
JF  - Monthly Notices of the Royal Astronomical Society
VL  - 497
IS  - 2
SP  - 1475-1487
EP  - 1475-1487
SN  - 00358711
KW  - binaries: spectroscopic
KW  - stars: individual: RW Tri
KW  - novae
KW  - cataclysmic variables
UR  - https://academic.oup.com/mnras/article-abstract/497/2/1475/5873686?redirectedFrom=fulltext
N2  - 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 Ha 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.
ER  - 

SUBEBEKOVA, G., S. ZHARIKOV, G. TOVMASSIAN, V. NEUSTROEV, M. WOLF, M-S HERNANDEZ, Hana KUČÁKOVÁ and S. KHOKHLOV. Structure of accretion flows in the nova-like cataclysmic variable RW Tri. \textit{Monthly Notices of the Royal Astronomical Society}. 2020, vol.~497, No~2, p.~1475-1487, 14 pp. ISSN~0035-8711. Available from: https://dx.doi.org/10.1093/mnras/staa2091.