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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&apos;s inner part.

  • Czech name

  • Czech description

Classification

  • Type

    J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database

  • CEP classification

  • OECD FORD branch

    10308 - Astronomy (including astrophysics,space science)

Result continuities

  • Project

  • 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