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arXiv · 1403.7526

Stellar rotation--planetary orbit period commensurability in the HAT-P-11 system

Bence Béky·Matthew J. Holman·David M. Kipping·Robert W. Noyes
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Abstract

A number of planet-host stars have been observed to rotate with a period equal to an integer multiple of the orbital period of their close planet. We expand this list by analyzing Kepler data of HAT-P-11 and finding a period ratio of 6:1. In particular, we present evidence for a long-lived spot on the stellar surface that is eclipsed by the planet in the same position four times, every sixth transit. We also identify minima in the out-of-transit lightcurve and confirm that their phase with respect to the stellar rotation is mostly stationary for the 48-month timeframe of the observations, confirming the proposed rotation period. For comparison, we apply our methods to Kepler-17 and confirm the findings of Bonomo & Lanza (2012) that the period ratio is not exactly 8:1 in that system. Finally, we provide a hypothesis on how interactions between a star and its planet could possibly result in an observed commensurability for systems where the stellar differential rotation profile happens to include a period at some latitude which is commensurable to the planetary orbit.

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Bence Béky, Matthew J. Holman, David M. Kipping, Robert W. Noyes. 2014-03-28. Stellar rotation--planetary orbit period commensurability in the HAT-P-11 system. https://doi.org/10.1088/0004-637x/788/1/1

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