V850 Cyg: An eclipsing binary with a giant  γ  Dor pulsator

Çakırlı, Ö.; İbanoǧlu, C.; Sipahi, E.; Akan, Mustafa

doi:10.1016/j.newast.2016.10.008

Cited by 6 publications

(1 citation statement)

References 53 publications

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“…These systems must have gone through sufficient AM transfer and have synchronized the stellar interior. Recently, in addition to the known γ Dor EBs in literature (Kurtz et al 2015;C ¸akırlı 2015;C ¸akırlı et al 2017;Guo et al 2016Guo et al , 2017He lminiak et al 2017a, b;Lee 2016;Lee & Park 2018;Zhang et al 2018;Li et al 2019b), Gaulme & Guzik (2019) did a systematic search for pulsating EBs and reported 119 γ Dor in EBs, and these are promising targets for searching for period spacing patterns and measuring internal rotation rates and near-core mixings. Such measurements to a large sample of binaries with different orbital periods, eccentricities and evolutionary stages will enable us to calibrate the timescale of tidal circularization/synchronization and the angular momentum transfer inside stars.…”

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confidence: 99%

A Mass-accreting Gamma Doradus Pulsator with a Synchronized Core in Kepler Eclipsing Binary KIC 7385478

Guo

2019

ApJL

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The short-period (P ≈ 1.7 d), Algol-type eclipsing binary KIC 7385478 consists of an F-type primary star (M 1 ≈ 1.71M ) and an evolved K-type secondary (M 2 ≈ 0.37M ) (Ozdarcan & Ali Dal 2017). We study the variability of the Kepler light curve and attribute many frequency peaks in the Fourier spectrum to the spot modulation. These frequencies are in the form of orbital harmonics and are highly variable in amplitude. They are most likely from the mass-accreting primary star. In addition, we identify a series prograde dipole g-modes from the primary star which show a quasi-linear period spacing pattern and are very stable in amplitude. The period spacing pattern reveals an asymptotic period spacing value in agreement with fundamental parameters of the primary star and also implies that the near-convective-core rotation rate is almost the same as the orbital period. Thus both the surface and the core of this Gamma Dor pulsator have synchronized with the binary orbit. We find that a lower stellar mass ≈ 1.50M and higher effective temperature are needed in order to be compatible with the asteroseismic constraints from single star evolutionary models.

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