ROTATION PERIODS OF 34,030 KEPLER MAIN-SEQUENCE STARS: THE FULL AUTOCORRELATION SAMPLE

By A. McQuillan, T. Mazeh, Suzanne Aigrain. 2014

604 citations recorded by the source corpus.

We analyzed three years of data from the Kepler space mission to derive rotation periods of main-sequence stars below 6500 K. Our automated autocorrelation-based method detected rotation periods between 0.2 and 70 days for 34,030 (25.6%) of the 133,030 main-sequence Kepler targets (excluding known eclipsing binaries and Kepler Objects of Interest), making this the largest sample of stellar rotation periods to date. In this paper we consider the detailed features of the now well-populated period–temperature distribution and demonstrate that the period bimodality, first seen by McQuillan et al. in the M-dwarf sample, persists to higher masses, becoming less visible above 0.6 M☉. We show that these results are globally consistent with the existing ground-based rotation-period data and find that the upper envelope of the period distribution is broadly consistent with a gyrochronological age of 4.5 Gyr, based on the isochrones of Barnes, Mamajek, & Hillenbrand and Meibom et al. We also performed a detailed comparison of our results to those of Reinhold et al. and Nielsen et al., who measured rotation periods of field stars observed by Kepler. We examined the amplitude of periodic variability for the stars with detection rotation periods, and found a typical range between ∼950 ppm (5th percentile) and ∼22,700 ppm (95th percentile), with a median of ∼5600 ppm. We found typically higher amplitudes for shorter periods and lower effective temperatures, with an excess of low-amplitude stars above ∼5400 K.

Subfields: Astronomy and Astrophysics, Education, Instrumentation

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Citations in the corpus

THE APOKASC CATALOG: AN ASTEROSEISMIC AND SPECTROSCOPIC JOINT SURVEY OF TARGETS IN THE KEPLER FIELDS (2014, background): “Time-series data from Kepler can also measure the surface rotation rates of stars through starspot modulation of their light curves (Basri et al. 2011; Garćıa et al. 2014; McQuillan et al. 2014).”
Revised Stellar Properties of Kepler Targets for the Q1-17 (DR25) Transit Detection Run (2016, background): “…et al. 2016) of subgiants and red giants, the detection of surface rotation and its relation to ages of solar-like stars (e.g. García et al. 2014; McQuillan et al. 2014; Ceillier et al. 2016; van Saders et al. 2016), as well as the measurement of magnetic activity of main-sequence stars (e.g.…”
Calibrating gyrochronology using Kepler asteroseismic targets (2015, background): “All stars in the asteroseismic sample with rotation periods published by McQuillan et al. (2014), also appear in the rotation period catalogue of Garcia et al. (2014).”
THE MASS-DEPENDENCE OF ANGULAR MOMENTUM EVOLUTION IN SUN-LIKE STARS (2014, background): “The best current example is the measurement of 34,000 ro- tation periods in the Kepler mission field of view, by Mcquillan et al. (2014).”
Revised Radii of Kepler Stars and Planets Using Gaia Data Release 2 (2018, background): “The revised classifications presented here will thus aid in increasing cool dwarf samples for studies of stellar rotation and activity (e.g. McQuillan et al. 2014; Angus et al. 2016; Davenport 2016) and red giants for asteroseismology (e.g. Hekker et al. 2011; Mosser et al. 2012; Stello et al.…”
Rotation and magnetism of Kepler pulsating solar-like stars : Towards asteroseismically calibrated age-rotation relations (2014, background): “We first compare our results with those obtained by McQuillan et al. (2014), who determined the Prot of many main-sequence stars – without binaries – by studying the ACF of their PDC lightcurves.”
The Habitability of Planets Orbiting M-dwarf Stars (2016, background): “M dwarfs of a given mass (provided it is above the convective limit) exhibit a coherent spin-down (McQuillan et al., 2013, 2014).”
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).”
Inferring probabilistic stellar rotation periods using Gaussian processes (2017, background): “We compare our results to those of the Tel Aviv team in Aigrain et al. (2015), who used the ACF method described in McQuillan et al. (2014) and Aigrain et al. (2015).”
THE KEPLER CATALOG OF STELLAR FLARES (2016, methodology): “From the final sample of 4041 flare stars, 402 targets had rotation periods of at least 0.1 days measured from the ensemble analysis of McQuillan et al. (2014).”
Spacing of Kepler Planets: Sculpting by Dynamical Instability (2015, background): “Gyro-chronology studies, the dating of stars using their stellar rotation periods, reveal that stars in the Kepler field, at least ones that have measurable rotation periods, have typical ages of a couple Gyrs (Walkowicz & Basri 2013; McQuillan et al. 2014).”
WATER VAPOR IN THE SPECTRUM OF THE EXTRASOLAR PLANET HD 189733b. I. THE TRANSIT (2014, background): “As such, it is photometrically more variable than ∼95% of stars in the Kepler sample (McQuillan et al. 2014; Ciardi et al. 2011; cf. also Figure 5 of McQuillan et al. 2012).”
THE Hα EMISSION OF NEARBY M DWARFS AND ITS RELATION TO STELLAR ROTATION (2016, methodology): “For stars more massive than 0.25 M , a negative correlation is seen between variability amplitude and rotation period for periods > 30 days (Hartman et al. 2011; McQuillan et al. 2014; Newton et al. 2016).”
Improved angular momentum evolution model for solar-like stars II. Exploring the mass dependence (2015, neutral): “The largest set of rotational periods has been recently obtained by McQuillan et al. (2014) for a sample of more than 34 000 ﬁeld stars using the Kepler satellite.”
Rotation, differential rotation, and gyrochronology of active Kepler stars (2015, methodology): “3.1–3.3) we compared our measurements to the state-of-the-art rotation periods from McQuillan et al. (2014) in Fig.”