Pulsating components of the eclipsing binaries with long period eccentric orbits

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 AE and 1.59 +/- 0.07 R AE, while their masses should be 2.59 +/- 0.09 M AE and 1.66 +/- 0.09 M AE 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 AE and 1.60 +/- 0.11 R AE, and their masses are computed as 1.64 +/- 0.09 M AE and 1.52 +/- 0.14 M AE, 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.

Automated summary

Based on the analysis of Kepler data and photometric observations, new findings about KIC 5217733 and KIC 11671429, two highly eccentric detached eclipsing binaries, are presented. The radii and masses of the primary and secondary components, as well as the dominant modes of pulsations, were estimated for both targets.