Activity of the post-nova V1363 Cygni on long timescales

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F22%3A00557956" target="_blank" >RIV/67985815:_____/22:00557956 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/68407700:21230/22:00358271

Výsledek na webu

<a href="https://doi.org/10.1093/pasj/psac017" target="_blank" >https://doi.org/10.1093/pasj/psac017</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/pasj/psac017" target="_blank" >10.1093/pasj/psac017</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Activity of the post-nova V1363 Cygni on long timescales

Popis výsledku v původním jazyce

V1363 Cyg is a cataclysmic variable (CV) and a post-nova. Our analysis of its long-term optical activity used the archival data from the AAVSO database and literature. We showed that the accretion disk of V1363 Cyg is exposed to the thermal-viscous instability (TVI) for at least part of the time. The time fraction spent in the high state or the outbursts dramatically changed on the timescale of decades. The highly variable brightness of V1363 Cyg displayed several episodes of a strong brightening (bumps in the light curve) from a cool disk in the TVI zone. This can be interpreted to mean their vastly discrepant decay rates show that only some of these bumps can be attributed to the dwarf nova outbursts without strong irradiation of the disk by the hot white dwarf. The Bailey relation of the decay rate, if ascribed to a DN outburst of V1363 Cyg, speaks in favor of its orbital period P-orb being very long for a CV, about 20-40 h. A dominant cycle length of about 435 d was present in the brightness changes all the time, even when the disk was well inside the TVI zone. We interpret it as modulation of the companion's mass outflow by differential rotation of the active region(s).

Název v anglickém jazyce

Activity of the post-nova V1363 Cygni on long timescales

Popis výsledku anglicky

V1363 Cyg is a cataclysmic variable (CV) and a post-nova. Our analysis of its long-term optical activity used the archival data from the AAVSO database and literature. We showed that the accretion disk of V1363 Cyg is exposed to the thermal-viscous instability (TVI) for at least part of the time. The time fraction spent in the high state or the outbursts dramatically changed on the timescale of decades. The highly variable brightness of V1363 Cyg displayed several episodes of a strong brightening (bumps in the light curve) from a cool disk in the TVI zone. This can be interpreted to mean their vastly discrepant decay rates show that only some of these bumps can be attributed to the dwarf nova outbursts without strong irradiation of the disk by the hot white dwarf. The Bailey relation of the decay rate, if ascribed to a DN outburst of V1363 Cyg, speaks in favor of its orbital period P-orb being very long for a CV, about 20-40 h. A dominant cycle length of about 435 d was present in the brightness changes all the time, even when the disk was well inside the TVI zone. We interpret it as modulation of the companion's mass outflow by differential rotation of the active region(s).

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

2022

Kód důvěrnosti údajů

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

Název periodika

Publications of the Astronomical Society of Japan

ISSN

0004-6264

e-ISSN

2053-051X

Svazek periodika

74

Číslo periodika v rámci svazku

3

Stát vydavatele periodika

JP - Japonsko

Počet stran výsledku

9

Strana od-do

569-577

Kód UT WoS článku

000784947900001

EID výsledku v databázi Scopus

2-s2.0-85133020815