Triple Eccentric Systems V0345 Lac, YY Sgr, and DR Vul

0517241 - ASÚ 2020 RIV PL eng J - Článek v odborném periodiku
Wolf, M. - Zasche, P. - Kučáková, Hana - Mašek, Martin - Hoňková, K. - Juryšek, Jakub - Paschke, A. - Šmelcer, L. - Zejda, M.
Triple Eccentric Systems V0345 Lac, YY Sgr, and DR Vul.
Acta Astronomica. Roč. 69, č. 1 (2019), s. 63-78. ISSN 0001-5237. E-ISSN 0001-5237
Grant CEP: GA ČR(CZ) GA16-01116S; GA MŠMT EF16_013/0001402; GA MŠMT LM2015038
Grant ostatní: GA ČR(CZ) GAP209/10/0715; GA ČR(CZ) GA15-02112S; OP VVV - AUGER-CZ(XE) CZ.02.1.01/0.0/0.0/16_013/0001402
Institucionální podpora: RVO:67985815 ; RVO:68378271
Klíčová slova: eclipsing binaries * stars * fundamental parameters
Obor OECD: Astronomy (including astrophysics,space science); Astronomy (including astrophysics,space science) (FZU-D)
Impakt faktor: 2.063, rok: 2019
Způsob publikování: Omezený přístup
https://doi.org/10.32023/0001-5237/69.1.5

We present more results of our long-term observational project to analyze the variations of the orbital period for early-type eccentric eclipsing binaries. About sixty new precise mid-eclipse times were measured or derived for three eclipsing binaries, namely V0345 Lac, YY Sgr, and DR Vul. Based on current O - C diagrams, we found in all cases that beside the typical apsidal motion the times of minima show additional cyclical changes likely caused by a third body orbiting the eclipsing pair. The new light curve solution of V0345 Lac results in a moderate orbital eccentricity (e = 0.26) of this binary. The periods of apsidal motion are 1580 yr, 295 yr, and 36 yr, respectively. The relativistic contributions to the total apsidal-motion rate are small for all three eccentric binaries - about 5-14%. The third-body orbital periods are relatively short: 24 yr, 19 yr and 66 yr, and the minimal masses of third bodies are: 2.0 M-circle dot, 0.8 M-circle dot, and 7.2 M-circle dot, respectively.
Trvalý link: http://hdl.handle.net/11104/0302540