Volume 605, September 2017
|Number of page(s)||11|
|Section||Stellar structure and evolution|
|Published online||19 September 2017|
Surface rotation of Kepler red giant stars⋆
1 IRFU, CEA, Université Paris-Saclay, 91191 Gif-sur-Yvette, France
2 Université Paris Diderot, AIM, Sorbonne Paris Cité, CEA, CNRS, 91191 Gif-sur-Yvette, France
3 Department of Astronomy, Ohio State University, 140 W 18th Ave, OH 43210, USA
4 Center for Extrasolar Planetary Systems, Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USA
5 Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia
6 School of Physics, University of New South Wales, NSW 2052, Australia
7 Carnegie-Princeton Fellow, Carnegie Observatories, 813 Santa Barbara Street, Pasadena, California, 91101, USA
8 Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
9 Department of Astrophysics, IMAPP, Radboud University Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands
Received: 11 October 2016
Accepted: 19 July 2017
Kepler allows the measurement of starspot variability in a large sample of field red giants for the first time. With a new method that combines autocorrelation and wavelet decomposition, we measure 361 rotation periods from the full set of 17 377 oscillating red giants in our sample. This represents 2.08% of the stars, consistent with the fraction of spectroscopically detected rapidly rotating giants in the field. The remaining stars do not show enough variability to allow us to measure a reliable surface rotation period. Because the stars with detected rotation periods have measured oscillations, we can infer their global properties, e.g. mass and radius, and quantitatively evaluate the predictions of standard stellar evolution models as a function of mass. Consistent with results for cluster giants when we consider only the 4881 intermediate-mass stars, M > 2.0 M⊙ from our full red giant sample, we do not find the enhanced rates of rapid rotation expected from angular momentum conservation. We therefore suggest that either enhanced angular momentum loss or radial differential rotation must be occurring in these stars. Finally, when we examine the 575 low-mass (M< 1.1 M⊙) red clump stars in our sample, which were expected to exhibit slow (non-detectable) rotation, 15% of them actually have detectable rotation. This suggests a high rate of interactions and stellar mergers on the red giant branch.
Key words: stars: rotation / stars: activity / stars: evolution
Full Tables 1 and 2 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (220.127.116.11) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/605/A111
© ESO, 2017
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