STELLAR ROTATION PERIODS OF THE KEPLER OBJECTS OF INTEREST: A DEARTH OF CLOSE-IN PLANETS AROUND FAST ROTATORS

By A. McQuillan, T. Mazeh, Suzanne Aigrain. 2013

160 citations recorded by the source corpus.

We present a large sample of stellar rotation periods for Kepler Objects of Interest, based on three years of public Kepler data. These were measured by detecting periodic photometric modulation caused by star spots, using an algorithm based on the autocorrelation function of the light curve, developed recently by McQuillan, Aigrain & Mazeh (2013). Of the 1919 main-sequence exoplanet hosts analyzed, robust rotation periods were detected for 737. Comparing the detected stellar periods to the orbital periods of the innermost planet in each system reveals a notable lack of close-in planets around rapid rotators. It appears that only slowly spinning stars with rotation periods longer than 5–10 days host planets on orbits shorter than 2 or 3 days, although the mechanism(s) that lead(s) to this is not clear.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/9edd64dff002f6ff6541622f2b25f43110159bf3

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Citations in the corpus

A STELLAR-MASS-DEPENDENT DROP IN PLANET OCCURRENCE RATES (2014, background): “Ages of stars in the Kepler sample are not well determined, though gyrochronology has provided estimates for a subsample of them (McQuillan et al. 2013, 2014).”
Rotation, differential rotation, and gyrochronology of active Kepler stars (2015, background): “This incident was first detected by McQuillan et al. (2013a) for the Kepler M dwarf periods, and confirmed later that the bimodality extends to hotter stars (Reinhold et al. 2013; McQuillan et al. 2014).”
Rotation and magnetism of Kepler pulsating solar-like stars : Towards asteroseismically calibrated age-rotation relations (2014, methodology): “2 in McQuillan et al. 2013a).”
ROTATION PERIODS OF 34,030 KEPLER MAIN-SEQUENCE STARS: THE FULL AUTOCORRELATION SAMPLE (2014, methodology): “See McQuillan et al. (2013a) for a detailed comparison of the ACF method with Fourier-based approaches.”
Inferring probabilistic stellar rotation periods using Gaussian processes (2017, methodology): “A comparison of our GP rotation period measurements to those of McQuillan et al. (2013a).”