THE KEPLER CLUSTER STUDY: STELLAR ROTATION IN NGC 6811

By S. Meibom, S. Barnes, D. Latham, N. Batalha, William J. Borucki, D. Koch, G. Basri, Lucianne M. Walkowicz, K. Janes, Jon M. Jenkins and 10 more. 2011

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We present rotation periods for 71 single dwarf members of the open cluster NGC 6811 determined using photometry from NASA's Kepler mission. The results are the first from The Kepler Cluster Study, which combines Kepler's photometry with ground-based spectroscopy for cluster membership and binarity. The rotation periods delineate a tight sequence in the NGC 6811 color–period diagram from ∼1 day at mid-F to ∼11 days at early-K spectral type. This result extends to 1 Gyr similar prior results in the ∼600 Myr Hyades and Praesepe clusters, suggesting that rotation periods for cool dwarf stars delineate a well-defined surface in the three-dimensional space of color (mass), rotation, and age. It implies that reliable ages can be derived for field dwarf stars with measured colors and rotation periods, and it promises to enable further understanding of various aspects of stellar rotation and activity for cool stars.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/91639218d76e8dd9d20551124a5a8cc03bc20a81

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Citations in the corpus

Stellar winds on the main-sequence - II. The evolution of rotation and winds (2015, background): “Rotation periods for 71 stars in NGC 6811 were reported by Meibom et al. (2011), of which 51 stars are in the mass range of interest to us.”
Rotation and magnetism of Kepler pulsating solar-like stars : Towards asteroseismically calibrated age-rotation relations (2014, methodology): “Several calibrations are reported in the literature (Pace & Pasquini 2004; Barnes 2007; Mamajek & Hillenbrand 2008; Meibom et al. 2009, 2011a), but they consistently struggle to find a calibration set at old ages and long rotation periods.”
MAGNETIC WREATHS AND CYCLES IN CONVECTIVE DYNAMOS (2012, methodology): “Improved observational techniques including spot-tracking from Kepler photometry (Meibom et al. 2011; Llama et al. 2012) and ZeemanDoppler imaging (Petit et al. 2008; Gaulme et al. 2010; Morgenthaler et al. 2012) may permit measurements of the size, frequency, and magnetic flux of starspots and the…”
Improved angular momentum evolution model for solar-like stars II. Exploring the mass dependence (2015, unknown): “…decade, thanks to a number of dedicated long-term monitoring studies of nearby populations (see e.g. Irwin & Bouvier 2009; Hartman et al. 2010; Agüeros et al. 2011; Meibom et al. 2011a; Irwin et al. 2011; A ﬀ er et al. 2012, 2013; Bouvier et al. 2014; Gallet & Bouvier 2013; McQuillan et al. 2014).”
STELLAR ROTATION PERIODS OF THE KEPLER OBJECTS OF INTEREST: A DEARTH OF CLOSE-IN PLANETS AROUND FAST ROTATORS (2013, background): “Kepler’s almost uninterrupted sub-mmag precision time series photometry allows for the derivation of precise orbital parameters from transit fitting, and stellar rotation measurements from star spot modulation (e.g. Basri et al. 2011; Meibom et al. 2011; Nielsen et al. 2013).”
The Gaia–Kepler Stellar Properties Catalog. I. Homogeneous Fundamental Properties for 186,301 Kepler Stars (2020, methodology): “Cluster Ages To independently confirm our derived stellar ages, we used the 1 Gyr open cluster NGC 6811 (Meibom et al. 2011).”
Kepler Presearch Data Conditioning I—Architecture and Algorithms for Error Correction in Kepler Light Curves (2012, methodology): “…in planet detection (Borucki et al. 2010; Holman et al. 2010; Doyle et al. 2011; Fressin et al. 2011; Lissauer et al. 2011; Welsh et al. 2012; Borucki et al. 2012) and stellar astrophysics (Meibom et al. 2011; Beck et al. 2011; Stello et al. 2011; Chaplin et al. 2011) based on Kepler data.”
Improved angular momentum evolution model for solar-like stars (2013, methodology): “…constraint was relaxed for older clusters, namely Praesepe (578 Myr), the Hyades (625 Myr), and NGC 6811 (1 Gyr), for which we used 12, 7, and 31 stars, respectively, as their rotational period distribution is single peaked and exhibits little dispersion (Delorme et al. 2011; Meibom et al. 2011).”
Rotation and differential rotation of active Kepler stars (2013, background): “Whether the two period gaps are caused by a selection bias affecting our period sample, or by a predominance of certain ages in the distribution of stellar ages (potentially introduced by stellar clusters in the Kepler field, see e.g. Meibom et al. (2011)) needs to be further tested.”
PLANETARY CANDIDATES OBSERVED BY KEPLER. VI. PLANET SAMPLE FROM Q1–Q16 (47 MONTHS) (2015, background): “…et al. 2014; Bedding et al. 2011), classical pulsators (e.g., Szabó et al. 2010), eclipsing binaries (e.g., Conroy et al. 2014), ages of clusters (Meibom et al. 2011), and active galactic 21 BAERI/NASA Ames Research Center, Moffett Field, CA 94035, USA 22 Institut für Astrophysik, Universität…”
Rotation, differential rotation, and gyrochronology of active Kepler stars (2015, background): “…and Kepler satellites, measurements of stellar rotation periods have become numerous in recent years, unprecedented in their number and accuracy (Meibom et al. 2011a; Affer et al. 2012; McQuillan et al. 2013a; Nielsen et al. 2013; McQuillan et al. 2013b; Walkowicz & Basri 2013; Reinhold et al.…”
Measuring the rotation period distribution of field M dwarfs with Kepler (2013, background): “The few open clusters included in Kepler’s field-of-view are particularly important, since their ages can be estimated relatively well, and a small sample of periods has already been published for 71 members of NGC6811 (Meibom et al. 2011).”