Hot donors in cataclysmic variables: The case of EI Psc
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F25%3A10511271" target="_blank" >RIV/00216208:11320/25:10511271 - isvavai.cz</a>
Result on the web
<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=c.F-beV9sZ" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=c.F-beV9sZ</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1051/0004-6361/202553970" target="_blank" >10.1051/0004-6361/202553970</a>
Alternative languages
Result language
angličtina
Original language name
Hot donors in cataclysmic variables: The case of EI Psc
Original language description
Context. We present results of time-resolved optical spectroscopy and photometry of the short-orbital period dwarf nova EI Psc.Aims. This study aims to determine fundamental system parameters of EI Psc, study properties of accretion structures in the system, and investigate its origin and current evolution state. Methods. We analyse newly obtained time-resolved spectroscopic and photometric observations as well as archival data. We used light curve modelling, Doppler tomography, and MESA evolutionary models to study the characteristics of EI Psc. Results. The system contains a relatively low temperature (Teff = 6130 K) white dwarf with mass of MWD = 0.70(4) M-circle dot. The mass of the warm (T-2 = 4440 K) secondary is M-2 = 0.13 M-circle dot. The inclination of the system is i = 44.degrees 5(7). The mass accretion rate is approximate to 4 x 10(-13) M-circle dot year(-1). The long-term light curve of the system shows outbursts and superoutbursts. The quiescence light curve is double-humped and is formed by the combination of radiation from the Roche lobe filling the hot secondary and the hot spot. The radius of the outer disc is about two times smaller than the tidal truncation radius. Most of the disc's emission consists of emission lines and radiation from the hot spot at the stream-disc impact region. Conclusions. These types of systems are formed from progenitors with a low mass WD MWD less than or similar to 0.6 M-circle dot and relatively massive secondaries 1.1 - 1.5 M-circle dot with initial orbital periods on a scale of days. The number of similar systems is expected to be significantly lower than the usual CVs due to a lower forming rate of their relatively massive progenitors.
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
2025
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Astronomy & Astrophysics
ISSN
0004-6361
e-ISSN
1432-0746
Volume of the periodical
699
Issue of the periodical within the volume
cerven
Country of publishing house
FR - FRANCE
Number of pages
18
Pages from-to
A81
UT code for WoS article
001520623700001
EID of the result in the Scopus database
2-s2.0-105010357068