Статья

THE KEPLER CLUSTER STUDY: STELLAR ROTATION IN NGC 6811

Søren MeibomHarvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USASydney A. BarnesLowell Observatory, Flagstaff, AZ 86001, USADavid W. LathamHarvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USANatalie M. BatalhaNASA Ames Research Center, Moffett Field, CA 94035, USAW. J. BoruckiNASA Ames Research Center, Moffett Field, CA 94035, USADavid KochNASA Ames Research Center, Moffett Field, CA 94035, USAGibor BasriAstronomy Department, University of California, Berkeley, CA 94720, USALucianne M. WalkowiczAstronomy Department, University of California, Berkeley, CA 94720, USAK. A. JanesDepartment of Astronomy, Boston University, Boston, MA 02215, USAJon M. JenkinsNASA Ames Research Center, Moffett Field, CA 94035, USAJeffrey Van CleveNASA Ames Research Center, Moffett Field, CA 94035, USAMichael R. HaasNASA Ames Research Center, Moffett Field, CA 94035, USASteve BrysonNASA Ames Research Center, Moffett Field, CA 94035, USAA. K. DupreeHarvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USAGábor FürészHarvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USAAndrew SzentgyorgyiHarvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USALars A. BuchhaveHarvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USABruce ClarkeSETI Institute, Mountain View, CA 94043, USAJoseph D. TwickenSETI Institute, Mountain View, CA 94043, USAElisa V. QuintanaSETI Institute, Mountain View, CA 94043, USA

2011en

ABI

Аннотация

We present rotation periods for 71 single dwarf members of the open cluster NGC6811 determined using photometry from NASA's Kepler Mission. The results are the first from The Kepler Cluster Study which combine Kepler's photometry with ground-based spectroscopy for cluster membership and binarity. The rotation periods delineate a tight sequence in the NGC6811 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 3-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.

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Идентификаторы

DOI: 10.1088/2041-8205/733/1/l9

Цитирования и источники

Цитирований: 1Использованных источников: 0

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