| Issue |
A&A
Volume 652, August 2021
|
|
|---|---|---|
| Article Number | A49 | |
| Number of page(s) | 12 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361/202140958 | |
| Published online | 10 August 2021 | |
The period-gap cataclysmic variable CzeV404 Her: A link between SW Sex and SU UMa systems⋆,⋆⋆
1
Astronomical Institute, Faculty of Mathematics and Physics, Charles University, V Holešovičkách 2, 180 00 Praha 8, Czech Republic
e-mail: honza.kara.7@gmail.com
2
Universidad Nacional Autónoma de México, Instituto de Astronomía, AP 106, Ensenada, 22800 BC, México
3
Astronomical Institute, Academy of Sciences, Fričova 298, 251 65 Ondřejov, Czech Republic
4
Research Centre for Theoretical Physics and Astrophysics, Institute of Physics, Silesian University in Opava, Bezručovo nám. 13, 746 01 Opava, Czech Republic
5
Variable Star and Exoplanet Section, Czech Astronomical Society, Fričova 298, 251 65 Ondřejov, Czech Republic
6
BSObservatory, Modrá 587, 760 01 Zlín, Czech Republic
7
FZU – Institute of Physics of the Czech Academy of Sciences, Na Slovance 1999/2, Prague 182 21, Czech Republic
Received:
31
March
2021
Accepted:
17
June
2021
Context. We present a new study of the eclipsing cataclysmic variable CzeV404 Her (Porb = 0.098 d) that is located in the period gap.
Aims. This report determines the origin of the object and the system parameters and probes the accretion flow structure of the system.
Methods. We conducted simultaneous time-resolved photometric and spectroscopic observations of CzeV404 Her. We applied our light-curve modelling techniques and the Doppler tomography method to determine the system parameters and analyse the structure of the accretion disk.
Results. We found that the system has a massive white dwarf MWD = 1.00(2) M⊙, a mass ratio of q = 0.16, and a relatively hot secondary with an effective temperature T2 = 4100(50) K. The system inclination is i = 78.8°. The accretion disk spreads out to the tidal limitation radius and has an extended hot spot or line region. The hot spot or line is hotter than the remaining outer part of the disk in quiescence or in intermediate state, but does not stand out completely from the disk flux in (super)outbursts.
Conclusions. We claim that this object represents a link between two distinct classes of SU UMa-type and SW Sex-type cataclysmic variables. The accretion flow structure in the disk corresponds to the SW Sex systems, but the physical conditions inside the disk fit the behaviour of SU UMa-type objects.
Key words: novae, cataclysmic variables / stars: fundamental parameters / stars: individual: CzeV404 Her / methods: observational / stars: dwarf novae
Table 4 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/652/A49
© ESO 2021
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