Pulsating components of the eclipsing binaries with long period eccentric orbits
Makaleler > Tam Makale · 2024
Yazarlar: Ezgi Yoldaş, Hasan Ali DAL, Orkun ÖZDARCAN
NEW ASTRONOMY, SCI Expanded İndekslerine Giren Dergi, Uluslararası, Scopus, 2024, cilt 107, ss 102151-102151
DOI: 10.1016/j.newast.2023.102151
Özet
Taking into account the results found by analysing the Kepler data together with our photometric observations, we present new findings about KIC 5217733 and KIC 11671429, which are two highly eccentric detached eclipsing binaries. We estimate that the radii of the primary and secondary components should be, respectively, 5.41 ± 0.07 R⊙ and 1.59 ± 0.07 R⊙, while their masses should be 2.59 ± 0.09 M⊙ and 1.66 ± 0.09 M⊙ for KIC 5217733, whose orbital period is 161.252379 days. In the case of KIC 11671429, whose orbital period is 112.463712 days, the radii of the primary and secondary components are estimated as 3.05 ± 0.07 R⊙ and 1.60 ± 0.11 R⊙, and their masses are computed as 1.64 ± 0.09 M⊙ and 1.52 ± 0.14 M⊙, respectively. The frequency analyses of the variations at out-of-eclipses reveal that both targets exhibit pulsations. In these pulsations, the g-modes are dominant for KIC 521773, while the p-modes are dominant for KIC 11671429.