Age, Activity and Rotation in Mid and Late-Type M Dwarfs from MEarth. Issue Volume 9:Issue S302(2013) (7th August 2014)

• Record Type: Journal Article
• Authors: West, Andrew A.; Weisenburger, Kolby L.; Irwin, Jonathan; Charbonneau, David; Dittmann, Jason; Berta-Thompson, Zachory K.
• Editors: Petit, Pascal; Jardine, Moira; Spruit, Hendrik C.
• Is Part Of: Proceedings of the International Astronomical Union. Volume 9:Issue S302(2013)
• Page Start: 176
• Page End: 179
• Publication Date: 2014-08-07
• Subjects: stars: activity, -- stars: low-mass, -- brown dwarfs, -- stars: late-type, -- stars: magnetic fields, -- stars: rotation, -- stars: kinematics, -- Galaxy: kinematics and dynamics; Astronomy -- Congresses; Astronomy -- Periodicals; 520
• DOI: 10.1017/S1743921314002014
• Languages: English
• ISSNs: 1743-9213

Abstract

Abstract: Using spectroscopic observations and photometric light curves of 280 nearby M dwarfs from the MEarth exoplanet transit survey, we examine the relationships between magnetic activity (quantified by Hα emission), rotation period, and stellar age (derived from three-dimensional space velocities). Although we have known for decades that a large fraction of mid-late-type M dwarfs are magnetically active, it was not clear what role rotation played in the magnetic field generation (and subsequent chromospheric heating). Previous attempts to investigate the relationship between magnetic activity and rotation in mid-late-type M dwarfs were hampered by the limited number of M dwarfs with measured rotation periods (and the fact that v sin i measurements only probe rapid rotation). However, the photometric data from the MEarth survey allows us to probe a wide range of rotation periods for hundreds of M dwarf stars (from less than one to over 100 days). Over all M spectral types we find that magnetic activity decreases with longer rotation periods, including late-type, fully convective M dwarfs. We find that the most magnetically active (and hence, most rapidly rotating) stars are consistent with a kinematically young population, while slow-rotators are less active or inactive and appear to belong to an older, dynamically heated stellar population.