Hot donors in cataclysmic variables: The case of EI Psc

Kód výsledku v 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>

Výsledek na webu

<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>

Jazyk výsledku

angličtina

Název v původním jazyce

Hot donors in cataclysmic variables: The case of EI Psc

Popis výsledku v původním jazyce

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&apos;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.

Název v anglickém jazyce

Hot donors in cataclysmic variables: The case of EI Psc

Popis výsledku anglicky

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&apos;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.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2025

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astronomy &amp; Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Svazek periodika

699

Číslo periodika v rámci svazku

cerven

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

18

Strana od-do

A81

Kód UT WoS článku

001520623700001

EID výsledku v databázi Scopus

2-s2.0-105010357068