Possible companions in low-mass eclipsing binaries: V380 Dra, BX Tri, and V642 Vir

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F20%3A00534854" target="_blank" >RIV/67985815:_____/20:00534854 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/68378271:_____/20:00534854

Výsledek na webu

<a href="http://hdl.handle.net/11104/0313016" target="_blank" >http://hdl.handle.net/11104/0313016</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.31577/caosp.2020.50.2.637" target="_blank" >10.31577/caosp.2020.50.2.637</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Possible companions in low-mass eclipsing binaries: V380 Dra, BX Tri, and V642 Vir

Popis výsledku v původním jazyce

We present the new results of our long-term observational project to analyze the orbital period variations of low-mass eclipsing binaries. More then 200 new precise mid-eclipse times recorded with a CCD were obtained for three eclipsing binaries with short orbital periods: V380 Dra (P = 0(d).49), BX Tri (0(d).19), and V642 Vir (0(d). 52). Observed-minus-calculated diagrams of the stars were analyzed using all reliable timings, and new parameters of the light-time effect were obtained. We derived for the first time the short orbital periods of possible third bodies of 10-20 years for these objects. We calculated that the minimum masses of the third component are close to 0.2 M-circle dot, which corresponds to the mass of M4 - M5 red dwarfs. The multiplicity of these systems also plays an important role in the precise determination of their physical parameters.

Název v anglickém jazyce

Possible companions in low-mass eclipsing binaries: V380 Dra, BX Tri, and V642 Vir

Popis výsledku anglicky

We present the new results of our long-term observational project to analyze the orbital period variations of low-mass eclipsing binaries. More then 200 new precise mid-eclipse times recorded with a CCD were obtained for three eclipsing binaries with short orbital periods: V380 Dra (P = 0(d).49), BX Tri (0(d).19), and V642 Vir (0(d). 52). Observed-minus-calculated diagrams of the stars were analyzed using all reliable timings, and new parameters of the light-time effect were obtained. We derived for the first time the short orbital periods of possible third bodies of 10-20 years for these objects. We calculated that the minimum masses of the third component are close to 0.2 M-circle dot, which corresponds to the mass of M4 - M5 red dwarfs. The multiplicity of these systems also plays an important role in the precise determination of their physical parameters.

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

2020

Kód důvěrnosti údajů

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

Název periodika

Contributions of the Astronomical Observatory Skalnate Pleso

ISSN

1336-0337

e-ISSN

—

Svazek periodika

50

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

SK - Slovenská republika

Počet stran výsledku

5

Strana od-do

637-641

Kód UT WoS článku

000523574300058

EID výsledku v databázi Scopus

2-s2.0-85087059629