The Z Camelopardalis-type Star AY Piscium: Stellar and Accretion Disk Parameters

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F23%3A10475213" target="_blank" >RIV/00216208:11320/23:10475213 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=Vssdrh9kpq" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=Vssdrh9kpq</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-4357/accd63" target="_blank" >10.3847/1538-4357/accd63</a>

Jazyk výsledku

angličtina

Název v původním jazyce

The Z Camelopardalis-type Star AY Piscium: Stellar and Accretion Disk Parameters

Popis výsledku v původním jazyce

We present a new study of the Z Cam-type eclipsing cataclysmic variable AY Piscium with the aim of determining the fundamental parameters of the system and the structure of the accretion flow therein. We use time-resolved photometric observations supplemented by spectroscopy in the standstill, to which we applied our light-curve modeling techniques and the Doppler tomography method, to update system parameters. We found that the system has a massive white dwarf M-WD = 0.90(4) M-circle dot, a mass ratio q = 0.50(3), and the effective temperature of a secondary T-2 = 4100(50) K. The system inclination is i = 74 degrees. 8(7). The orbital period of the system P-orb = 0.217320523(8) day is continuously increasing at a rate of P-orb = + 7.6(5) 10(-9) day yr(-1). The masstransfer rate varies between 2.4 x 10(-10) M-circle dot yr(-1) in quiescence up to 1.36 x 10(-8) Me yr(-1) in outburst. The accretion disk transitions from the cooler, flared, steady-state disk to a warmer state with a practically constant and relatively high disk height. The mass-transfer rate is about 1.6 x 10(-9) M-circle dot yr(-1) in the standstill. The Balmer emission lines show a multicomponent structure similar to that observed in long-orbital-period nova-like systems. Out of standstill, the system exhibits outburst bimodality, with long outbursts being more prominent. We conclude that the Balmer emission lines in AY Psc are formed by the combination of radiation from the irradiated surface of the secondary, from the outflow zone, and from winds originating in the bright spot and the disk&apos;s inner part.

Název v anglickém jazyce

The Z Camelopardalis-type Star AY Piscium: Stellar and Accretion Disk Parameters

Popis výsledku anglicky

We present a new study of the Z Cam-type eclipsing cataclysmic variable AY Piscium with the aim of determining the fundamental parameters of the system and the structure of the accretion flow therein. We use time-resolved photometric observations supplemented by spectroscopy in the standstill, to which we applied our light-curve modeling techniques and the Doppler tomography method, to update system parameters. We found that the system has a massive white dwarf M-WD = 0.90(4) M-circle dot, a mass ratio q = 0.50(3), and the effective temperature of a secondary T-2 = 4100(50) K. The system inclination is i = 74 degrees. 8(7). The orbital period of the system P-orb = 0.217320523(8) day is continuously increasing at a rate of P-orb = + 7.6(5) 10(-9) day yr(-1). The masstransfer rate varies between 2.4 x 10(-10) M-circle dot yr(-1) in quiescence up to 1.36 x 10(-8) Me yr(-1) in outburst. The accretion disk transitions from the cooler, flared, steady-state disk to a warmer state with a practically constant and relatively high disk height. The mass-transfer rate is about 1.6 x 10(-9) M-circle dot yr(-1) in the standstill. The Balmer emission lines show a multicomponent structure similar to that observed in long-orbital-period nova-like systems. Out of standstill, the system exhibits outburst bimodality, with long outbursts being more prominent. We conclude that the Balmer emission lines in AY Psc are formed by the combination of radiation from the irradiated surface of the secondary, from the outflow zone, and from winds originating in the bright spot and the disk&apos;s inner part.

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

2023

Kód důvěrnosti údajů

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

Název periodika

Astrophysical Journal

ISSN

0004-637X

e-ISSN

1538-4357

Svazek periodika

950

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

19

Strana od-do

47

Kód UT WoS článku

001005693700001

EID výsledku v databázi Scopus

2-s2.0-85162156411