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Using the Galactic Dynamics of M7 Dwarfs to Infer the Evolution of Their Magnetic Activity

Andrew A. West et al 2006 The Astronomical Journal 132 2507-2512   doi: 10.1086/508652  Help

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Andrew A. West1,2, John J. Bochanski2, Suzanne L. Hawley2, Kelle L. Cruz3, Kevin R. Covey2, Nicole M. Silvestri2, I. Neill Reid4 and James Liebert5
1 Astronomy Department, University of California, 601 Campbell Hall, Berkeley, CA 94720-3411
2 Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195
3 Department of Astrophysics, American Museum of Natural History, Central Park West at 79th Street, New York, NY 10024
4 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218
5 Department of Astronomy and Steward Observatory, University of Arizona, Tucson, AZ 85721
E-mail: awest@astro.berkeley.edu

ABSTRACT. We present a spectroscopic study and dynamical analysis of ~2600 M7 dwarfs. We confirm our previous finding that the fraction of magnetically active stars decreases with vertical distance from the Galactic plane. We also show that the mean luminosity of the Hα emission has a small but statistically significant decrease with distance. Using space motions for ~1300 stars and a simple one-dimensional dynamical simulation, we demonstrate that the drop in the activity fraction of M7 dwarfs can be explained by thin disk dynamical heating and a rapid decrease of magnetic activity at a mean stellar age of ~6-7 Gyr.

Key words: Galaxy: kinematics and dynamics; Galaxy: structure; solar neighborhood; stars: activity; stars: late-type; stars: low-mass, brown dwarfs

Print publication: Issue 6 (2006 December)
Received 2006 June 30, accepted for publication 2006 August 25
Published 2006 November 1

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