The two eccentric eclipsing binaries in multiple systems: V539 Arae and V335 Serpentis

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F22%3A00555881" target="_blank" >RIV/67985815:_____/22:00555881 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/68378271:_____/22:00555881 RIV/00216208:11320/22:10455230 RIV/00216224:14310/22:00125358 RIV/47813059:19630/22:A0000224

Výsledek na webu

<a href="https://doi.org/10.1016/j.newast.2021.101708" target="_blank" >https://doi.org/10.1016/j.newast.2021.101708</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1016/j.newast.2021.101708" target="_blank" >10.1016/j.newast.2021.101708</a>

Jazyk výsledku

angličtina

Název v původním jazyce

The two eccentric eclipsing binaries in multiple systems: V539 Arae and V335 Serpentis

Popis výsledku v původním jazyce

We present new results of our long-term observational project to analyze the variations of the orbital period for early-type eccentric eclipsing binaries. Altogether 77 new mid-eclipse times were measured or derived for two eclipsing binaries, namely V539 Ara and V335 Ser. Based on current O - C diagrams, we found in both systems that times of minima besides the typical apsidal motion show additional cyclical changes likely caused by the third or fourth bodies orbiting the eclipsing pair. The improved periods of apsidal motion are 155 and 1080 years, respectively. For the first time we propose a third and fourth body orbiting V539 Ara, stellar companions in a hierarchical system with a minimal mass of 0.41 and 1.74 Ms. In V355 Ser we found a possible third body with a mass of 0.18 Ms orbiting this eclipsing pair. The third- and fourth-body orbital periods are relatively short: 29 and 57 yr in case of V539 Ara, and 25 yr for V335 Ser.

Název v anglickém jazyce

The two eccentric eclipsing binaries in multiple systems: V539 Arae and V335 Serpentis

Popis výsledku anglicky

We present new results of our long-term observational project to analyze the variations of the orbital period for early-type eccentric eclipsing binaries. Altogether 77 new mid-eclipse times were measured or derived for two eclipsing binaries, namely V539 Ara and V335 Ser. Based on current O - C diagrams, we found in both systems that times of minima besides the typical apsidal motion show additional cyclical changes likely caused by the third or fourth bodies orbiting the eclipsing pair. The improved periods of apsidal motion are 155 and 1080 years, respectively. For the first time we propose a third and fourth body orbiting V539 Ara, stellar companions in a hierarchical system with a minimal mass of 0.41 and 1.74 Ms. In V355 Ser we found a possible third body with a mass of 0.18 Ms orbiting this eclipsing pair. The third- and fourth-body orbital periods are relatively short: 29 and 57 yr in case of V539 Ara, and 25 yr for V335 Ser.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

Výsledek vznikl pri realizaci vícero projektů. Více informací v záložce Projekty.

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2022

Kód důvěrnosti údajů

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

Název periodika

New Astronomy

ISSN

1384-1076

e-ISSN

1384-1092

Svazek periodika

92

Číslo periodika v rámci svazku

April

Stát vydavatele periodika

NL - Nizozemsko

Počet stran výsledku

6

Strana od-do

101708

Kód UT WoS článku

000707225600002

EID výsledku v databázi Scopus

2-s2.0-85117145899