Analysis of KIC 7023917: Spotted low-mass ratio eclipsing binary with δ Scuti pulsations

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F24%3A00598986" target="_blank" >RIV/67985815:_____/24:00598986 - isvavai.cz</a>

Výsledek na webu

<a href="https://hdl.handle.net/11104/0356556" target="_blank" >https://hdl.handle.net/11104/0356556</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-3881/ad6dd3" target="_blank" >10.3847/1538-3881/ad6dd3</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Analysis of KIC 7023917: Spotted low-mass ratio eclipsing binary with δ Scuti pulsations

Popis výsledku v původním jazyce

Times of minima of eclipsing binary KIC 7023917 show quasiperiodic anti-symmetric deviations from the calculated one with an amplitude of up to 10 minutes and a period of 200-300 days. These changes correlate with the observed variations of the light-curve maxima (amplitude and phase separation). We used photometric data obtained by Kepler and TESS missions to analyze the times of minima and determine system parameters. The phases and amplitudes of the maxima were measured to study the O'Connell effect. As an additional source of information, we performed ground-based multicolor photometric observation and determined the radial velocities of the system from our spectroscopic measurements. We could explain long-term variations of the light-curve shape and times of the eclipses using the cold star spot located on the secondary component and the modification of its size. Based on our modelling, the system consists of a primary main-sequence star of spectral type A7 and an evolved, oversized secondary component with a mass ratio of only 0.1 due to past mass transfer. Calculation of absolute parameters gives us the mass of the primary component about 1.8 M-circle dot and 0.2 M-circle dot for the secondary one, and radii of 2.2 R-circle dot of the primary star and 0.9 R-circle dot of secondary one, respectively. The studied low-mass ratio eclipsing binary is probably a progenitor of the variable star of EL CVn type. A multiple-period photometric variability was disclosed in the TESS data ranging from half to two hours due to delta Scuti-type pulsations of the primary component.

Název v anglickém jazyce

Analysis of KIC 7023917: Spotted low-mass ratio eclipsing binary with δ Scuti pulsations

Popis výsledku anglicky

Times of minima of eclipsing binary KIC 7023917 show quasiperiodic anti-symmetric deviations from the calculated one with an amplitude of up to 10 minutes and a period of 200-300 days. These changes correlate with the observed variations of the light-curve maxima (amplitude and phase separation). We used photometric data obtained by Kepler and TESS missions to analyze the times of minima and determine system parameters. The phases and amplitudes of the maxima were measured to study the O'Connell effect. As an additional source of information, we performed ground-based multicolor photometric observation and determined the radial velocities of the system from our spectroscopic measurements. We could explain long-term variations of the light-curve shape and times of the eclipses using the cold star spot located on the secondary component and the modification of its size. Based on our modelling, the system consists of a primary main-sequence star of spectral type A7 and an evolved, oversized secondary component with a mass ratio of only 0.1 due to past mass transfer. Calculation of absolute parameters gives us the mass of the primary component about 1.8 M-circle dot and 0.2 M-circle dot for the secondary one, and radii of 2.2 R-circle dot of the primary star and 0.9 R-circle dot of secondary one, respectively. The studied low-mass ratio eclipsing binary is probably a progenitor of the variable star of EL CVn type. A multiple-period photometric variability was disclosed in the TESS data ranging from half to two hours due to delta Scuti-type pulsations of the primary component.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/LTT20015" target="_blank" >LTT20015: PLATOSpec pozemní podpora vesmírných misí PLATO a TESS - nový český spektrograf ve spolupráci s Evropskou jižní observatoří</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2024

Kód důvěrnosti údajů

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

Název periodika

Astronomical Journal

ISSN

0004-6256

e-ISSN

1538-3881

Svazek periodika

168

Číslo periodika v rámci svazku

4

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

11

Strana od-do

171

Kód UT WoS článku

001318992000001

EID výsledku v databázi Scopus

2-s2.0-85205365547