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The Triple Eccentric Systems V974 Cyg, RU Mon, and V456 Oph

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Wolf M. , Zasche P. , Kučáková H. , Hoňková K. , Juryšek J. , Mašek M. , Uhlař R. , Urbaník M.

Acta Astronomica

2017

tom Vol. 67, No. 3

257--271

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☉, 1.6 M☉, and 0.27 M☉, respectively.

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

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Wolf M. , Zasche P. , Kučáková H. , Mašek M. , Hoňková K. , Juryšek J. , Paschke A. , Šmelcer L. , Zejda M.

Acta Astronomica

2019

tom Vol. 69, No. 1

63--78

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☉, 0.8 M☉, and 7.2 M☉, respectively.