J 2021

The period-gap cataclysmic variable CzeV404 Her: A link between SW Sex and SU UMa systems

KARA, J., S. ZHARIKOV, M. WOLF, Hana KUČÁKOVÁ, P. CAGAS et. al.

Basic information

Original name

The period-gap cataclysmic variable CzeV404 Her: A link between SW Sex and SU UMa systems

Authors

KARA, J., S. ZHARIKOV, M. WOLF, Hana KUČÁKOVÁ (203 Czech Republic, belonging to the institution), P. CAGAS, A.L. MEDINA RODRIGUEZ and M. MASEK

Edition

Astronomy & Astrophysics, FR - Francouzská republika, 2021, 0004-6361

Other information

Language

English

Type of outcome

Článek v odborném periodiku

Field of Study

10308 Astronomy

Country of publisher

France

Confidentiality degree

není předmětem státního či obchodního tajemství

References:

RIV identification code

RIV/47813059:19630/21:A0000155

Organization unit

Institute of physics in Opava

UT WoS

000683516700006

Keywords in English

novae; cataclysmic variables;stars: fundamental parametersstars: individual: CzeV404 Her;methods: observational;stars: dwarf novae

Tags

Tags

International impact, Reviewed
Změněno: 28/3/2022 12:12, Mgr. Pavlína Jalůvková

Abstract

V originále

We present a new study of the eclipsing cataclysmic variable CzeV404 Her (P-orb = 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 M-WD = 1.00(2) M-circle dot, a mass ratio of q = 0.16, and a relatively hot secondary with an effective temperature T-2 = 4100(50) K. The system inclination is i = 78.8 degrees. 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.