Journal
ASTRONOMICAL JOURNAL
Volume 146, Issue 3, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-6256/146/3/50
Keywords
Galaxy: stellar content; Galaxy: structure; stars: activity; stars: late-type; stars: low-mass
Categories
Funding
- Alfred P. Sloan Foundation
- National Science Foundation
- U.S. Department of Energy
- National Aeronautics and Space Administration
- Japanese Monbukagakusho
- Max Planck Society
- Higher Education Funding Council for England
- American Museum of Natural History
- Astrophysical Institute Potsdam
- University of Basel
- University of Cambridge
- Case Western Reserve University
- The University of Chicago
- Drexel University
- Fermilab
- Institute for Advanced Study
- Japan Participation Group
- The Johns Hopkins University
- Joint Institute for Nuclear Astrophysics
- Kavli Institute for Particle Astrophysics and Cosmology
- Korean Scientist Group
- Chinese Academy of Sciences (LAMOST)
- Los Alamos National Laboratory
- Max-Planck-Institute for Astronomy (MPIA)
- Max-Planck-Institute for Astrophysics (MPA)
- New Mexico State University
- Ohio State University
- University of Pittsburgh
- University of Portsmouth
- Princeton University
- United States Naval Observatory
- University of Washington
- Paul E. Gray fund
- National Science Foundation [DGE-1144469]
- NSF [AST-1109273]
- Research Corporation for Science Advancement's Cottrell Scholarship
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We analyze the magnetic activity of 59,318 M dwarfs from the Sloan Digital Sky Survey Data Release 7. This analysis explores the spatial distribution of M dwarf activity as a function of both vertical distance from the Galactic plane (Z) and planar distance from the Galactic center (R). We confirm the established trends of decreasing magnetic activity (as measured by Ha emission) with increasing distance from the mid-plane of the disk and find evidence of a trend in Galactocentric radii. We measure a non-zero radial gradient in the activity fraction in our analysis of stars with spectral types dM3 and dM4. The activity fraction increases with R and can be explained by a decreasing mean stellar age with increasing distance from the Galactic center.
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