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We present the physical properties of the eclipsing binary V2281 Cyg, whichshows a light-time effect due to a supposed tertiary component from its eclipsetiming variation according to the $Kepler$ observations. The high-resolutionspectra and $BVR$ photometric data of the system were obtained at BohyunsanOptical Astronomy Observatory and Mount Lemmon Optical Astronomy Observatory,respectively. To determine the fundamental parameters of the eclipsing pair andits circumbinary object, we simultaneously analyzed the radial velocities,light curves, and eclipse times including the $Kepler$ data. The masses andradii for the primary and secondary stars were determined with accuracy levelsof approximately 2\% and 1\%, respectively, as follows: $M_{1} = 1.61 \pm 0.04$M$_\odot$ and $M_{2} = 1.60 \pm 0.04$ M$_\odot$, $R_{1} = 1.94 \pm 0.02$R$_\odot$ and $R_{2} = 1.93 \pm 0.02$ R$_\odot$. If its orbit is coplanar withthe eclipsing binary, the period and semimajor axis of the third body werecalculated to be $P_{3b}=4.1$ years and $a_{3b}=4.06$ au, respectively, and itsmass is $M_{3b}=0.75$ M$_\odot$. The evolutionary state of the system wasinvestigated by comparing the masses and radii with theoretical models. Theresults demonstrate that V2281 Cyg is a detached eclipsing binary, whichconsists of twin main-sequence stars with an age of 1.5 Gyr.

The Kepler Eclipsing Binary V2281 Cygni with Twin Stars