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

@article{37372,
   author = {Wolf, Marek and Zasche, Petr and Kučáková, Hana and Mašek, Martin and Hoňková, Kateřina and Juryšek, Jakub and Paschke, Anton and Šmelcer, Ladislav and Zejda, Miloslav},
   article_number = {1},
   doi = {http://dx.doi.org/10.32023/0001-5237/69.1.5},
   keywords = {binaries: eclipsing; Stars: fundamental parameters; Stars: individual: V0345 Lac - YY Sgr - and DR Vul},
   language = {eng},
   issn = {0001-5237},
   journal = {Acta Astronomica},
   title = {Triple Eccentric Systems V0345 Lac, YY Sgr, and DR Vul},
   url = {http://acta.astrouw.edu.pl/Vol69/n1/a_69_1_5.html},
   volume = {69},
   year = {2019}
}

TY  - JOUR
ID  - 37372
AU  - Wolf, Marek - Zasche, Petr - Kučáková, Hana - Mašek, Martin - Hoňková, Kateřina - Juryšek, Jakub - Paschke, Anton - Šmelcer, Ladislav - Zejda, Miloslav
PY  - 2019
TI  - Triple Eccentric Systems V0345 Lac, YY Sgr, and DR Vul
JF  - Acta Astronomica
VL  - 69
IS  - 1
SP  - 63-78
EP  - 63-78
SN  - 00015237
KW  - binaries: eclipsing
KW  - Stars: fundamental parameters
KW  - Stars: individual: V0345 Lac - YY Sgr - and DR Vul
UR  - http://acta.astrouw.edu.pl/Vol69/n1/a_69_1_5.html
L2  - http://acta.astrouw.edu.pl/Vol69/n1/a_69_1_5.html
N2  - 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_Sun, 0.8 M_Sun, and 7.2 M_Sun, respectively.
ER  - 

WOLF, Marek, Petr ZASCHE, Hana KUČÁKOVÁ, Martin MAŠEK, Kateřina HOŇKOVÁ, Jakub JURYŠEK, Anton PASCHKE, Ladislav ŠMELCER a Miloslav ZEJDA. Triple Eccentric Systems V0345 Lac, YY Sgr, and DR Vul. \textit{Acta Astronomica}. 2019, roč.~69, č.~1, s.~63-78. ISSN~0001-5237. Dostupné z: https://dx.doi.org/10.32023/0001-5237/69.1.5.