The Z Camelopardalis-type Star AY Piscium: Stellar and Accretion Disk Parameters
The result's identifiers
Result code in 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>
Result on the web
<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>
Alternative languages
Result language
angličtina
Original language name
The Z Camelopardalis-type Star AY Piscium: Stellar and Accretion Disk Parameters
Original language description
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's inner part.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
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Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Others
Publication year
2023
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Astrophysical Journal
ISSN
0004-637X
e-ISSN
1538-4357
Volume of the periodical
950
Issue of the periodical within the volume
1
Country of publishing house
US - UNITED STATES
Number of pages
19
Pages from-to
47
UT code for WoS article
001005693700001
EID of the result in the Scopus database
2-s2.0-85162156411