The triple eccentric systems V974 Cyg, RU Mon, and V456 Oph

0510345 - FZÚ 2020 RIV PL eng J - Journal Article
Wolf, M. - Zasche, P. - Kučáková, H. - Hoňková, K. - Juryšek, Jakub - Mašek, Martin - Uhlař, R. - Urbanik, M.
The triple eccentric systems V974 Cyg, RU Mon, and V456 Oph.
Acta Astronomica. Roč. 67, č. 3 (2017), s. 257-271. ISSN 0001-5237. E-ISSN 0001-5237
R&D Projects: GA MŠMT LM2015038; GA MŠMT LG15014; GA MŠMT EF16_013/0001402
EU Projects: European Commission(XE) 283783 - GLORIA
Grant - others:OP VVV - AUGER-CZ(XE) CZ.02.1.01/0.0/0.0/16_013/0001402
Institutional support: RVO:68378271
Keywords : eclipsing binaries * individual stars V974 Cyg, RU Mon, V456 Oph * stars: fundamental parameters
OECD category: Astronomy (including astrophysics,space science)
Impact factor: 3.667, year: 2017
Method of publishing: Limited access
https://doi.org/10.32023/0001-5237/67.3.4

We present results of a long-term program for timing the eclipses of eccentric eclipsing binaries. About 40 new precise mid-eclipse times were measured for the eclipsing binary V974 Cyg, RU Mon and V456 Oph. Based on current O-C diagrams, we found in all cases that times of minima besides the typical apsidal motion show additional cyclical changes caused very probably by the third bodies orbiting the eclipsing pair. The periods of apsidal motion are 1470 yr, 361 yr and 22.6 yr, respectively. The period of V456 Oph this is one of the shortest known apsidal-motion periods. The relativistic contributions to the total apsidal-motion rate are significant for V974 Cyg (about 30%) and negligible for RU Mon and V456 Oph (1-2.5%). The third-body orbital periods are relatively short: 30.6 yr, 59.8 yr and 7.4 yr, and their minimal masses are 0.40 M-circle dot, 1.6 M-circle dot, and 0.27 M-circle dot, respectively.
Permanent Link: http://hdl.handle.net/11104/0300865