Analysis of the exoplanet containing system Kepler 91

TL;DR

This study uses advanced modeling techniques to analyze Kepler 91, improving mass ratio estimates and exploring complex light variations caused by pulsations and potential resonances in the system.

Contribution

It introduces a refined analysis method incorporating tidal distortion effects up to the fifth power of fractional radius, enhancing mass ratio accuracy over previous studies.

Findings

Improved mass ratio estimation consistent with spectroscopic data.

Identification of non-radial pulsations affecting light curves.

Evidence suggesting possible Trojan or resonant mass concentrations.

Abstract

We have applied the graphical user interfaced close binary system analysis program WinFitter to an intensive study of Kepler 91 using all the available photometry from the NASA Exoplanet Archive (NEA) at the Caltech website: http://exoplanetarchive.ipac.caltech.edu . Our fitting function for the tidal distortion derives from the relevant Radau equation and includes terms up to the fifth power of the fractional radius. This results in a systematic improvement in the mass ratio estimation over that of Lillo Box et al (2014a) and our derived value for the mass ratio is in close agreement with that inferred from recent high-resolution spectroscopic data. It is clear that the data analysis in terms of simply an eclipsing binary system is compromised by the presence of significant other causes of light variation, in particular non-radial pulsations. We apply a low-frequency filtering procedure to separate out some of this additional light variation. Whilst the derived eccentricity appears then reduced, an eccentric effect remains in the light curve. We consider how this may be maintained in spite of likely frictional effects operating over a long time. There are also indications of the possible effects of Trojan or other period-resonant mass concentrations. Suggestions of a possible secular period variation are briefly discussed.