The Kepler Eclipsing System KIC 5621294 and its Substellar Companion

TL;DR

This study analyzes the Kepler eclipsing binary KIC 5621294, revealing a third substellar companion likely a brown dwarf, and discusses period variations caused by additional companions and stellar activity.

Contribution

First detailed analysis of KIC 5621294 combining light and timing variations, identifying a substellar third body and complex period modulations.

Findings

Eclipsing system is a classical Algol-type with specific parameters.

Detected a third body with a mass suggesting a brown dwarf.

Orbital period shows sinusoidal and parabolic variations, indicating multiple companions.

Abstract

We present the physical properties of KIC 5621294 showing light and timing variations from the ${\it Kepler}$ photometry. Its light curve displays partial eclipses and O'Connell effect with Max II fainter than Max I, which was fitted quite well by applying third-body and spot effects to the system. The results indicate that the eclipsing pair is a classical Algol-type system with parameters of $q$=0.22, $i$=76$^\circ$.8, and $\Delta$($T_{1}$--$T_{2}$)=4,235 K, in which the detached primary component fills about 77\% of its limiting lobe. Striking discrepancies exist between the primary and secondary eclipse times obtained with the method of Kwee \& van Woerden. These are mainly caused by surface inhomogeneities due to spot activity detected in our light-curve synthesis. The 1,253 light-curve timings from the Wilson-Devinney code were used for a period study. It was found that the orbital period of KIC 5621294 has varied due to a periodic variation overlaid on a downward parabola. The sinusoidal variation with a period of 961 d and a semi-amplitude of 22.5 s most likely arise from a light-time effect due to a third component with a mass of $M_3 \sin i_3$=46.9 M$\rm_{Jup}$, which is in good agreement with that calculated from the light curve itself. If its orbital inclination is larger than about 40$^\circ$, the mass of the circumbinary object would possibly match a brown dwarf. The parabolic variation could not be fully explained by either a mass transfer between the binary components or an angular momentum via magnetic braking. It is possible that the parabola may only be the observed part of a period modulation caused by the presence of another companion in a wider orbit.