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Rotation Periods of Nearby, Mid-to-late M Dwarfs from the MEarth Project

Published online by Cambridge University Press:  27 January 2016

Elisabeth R. Newton ,
Jonathan Irwin ,
David Charbonneau ,
Zachary K. Berta-Thomspon  and
Andrew A. West
Elisabeth R. Newton*
Affiliation:
Harvard-Smithsonian Center for Astrophysics
Jonathan Irwin
Affiliation:
Harvard-Smithsonian Center for Astrophysics
David Charbonneau
Affiliation:
Harvard-Smithsonian Center for Astrophysics
Zachary K. Berta-Thomspon
Affiliation:
Massachusetts Institute of Technology
Andrew A. West
Affiliation:
Boston University
*
*email: enewton@cfa.harvard.edu
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Abstract

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Field stars provide important constraints for the late stages of stars' angular momentum evolution. We measured rotation periods ranging from 0.1 to 150 days for approximately 450 mid-to-late M dwarfs using photometry from the MEarth transiting planet survey. We use parallaxes, proper motions, and radial velocities to calculate galactic kinematics for these solar neighborhood M dwarfs. The velocity dispersions increase towards longer rotation periods, indicating that there is a relationship between rotation and age for these stars.

Keywords

stars: low-massstars: rotationstars: kinematics and dynamics

Information

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S314: Young Stars & Planets Near the Sun , November 2015 , pp. 124 - 125
Copyright
Copyright © International Astronomical Union 2016 

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