KIC 7385478: An eclipsing binary with a γ Doradus component

Abstract

We present spectroscopic and photometric analysis of the eclipsing binary KIC\,7385478. We find that the system is formed by F1V + K4III-IV components. Combining results from analysis of spectroscopic data and $Kepler$ photometry, we calculate masses and radii of the primary and the secondary components as M${}_1$ = 1.71 $\pm$ 0.08 \Msun, M${}_2$ = 0.37 $\pm$ 0.04 \Msun~ and R${}_1$ = 1.59 $\pm$ 0.03\Rsun, R${}_2$ = 1.90 $\pm$ 0.03\Rsun, respectively. Position of the primary component in HR diagram is in the region of $\gamma$ Doradus type pulsators and residuals from light curve modeling exhibit additional light variation with a dominant period of $\sim$0.5 day. These are clear evidences of the $\gamma$ Doradus type pulsations on the primary component. We also observe occasional increase in amplitude of the residuals, where the orbital period becomes the most dominant period. These may be attributed to the cool star activity originating from the secondary component.

arXiv comment14 pages, 8 figures, 5 tables

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Cited by in corpus (3)

• Systematic search for stellar pulsators in the eclipsing binaries observed by Kepler
• A Mass-accreting Gamma Doradus Pulsator with a Synchronized Core in Kepler Eclipsing Binary KIC 7385478
• Then and now: A new look at the eclipse timing variations of hierarchical triple star candidates in the primordial $Kepler$-field, revisited by TESS