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

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F20%3A00536877" target="_blank" >RIV/67985815:_____/20:00536877 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1093/mnras/staa2091" target="_blank" >https://doi.org/10.1093/mnras/staa2091</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/staa2091" target="_blank" >10.1093/mnras/staa2091</a>

Jazyk výsledku

angličtina

Název v původním jazyce

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

Popis výsledku v původním jazyce

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.

Název v anglickém jazyce

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

Popis výsledku anglicky

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.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2020

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Monthly Notices of the Royal Astronomical Society

ISSN

1365-2966

e-ISSN

—

Svazek periodika

497

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

13

Strana od-do

1475-1487

Kód UT WoS článku

000574924500014

EID výsledku v databázi Scopus

2-s2.0-85093970755