DGp.2.08 — V and K-band Mass-Luminosity Relations for M Dwarf Stars

Date & Time

Aug 10th at 6:00 PM until 6:00 PM




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Author(s): George Frederick Benedict4, Todd J Henry3, Barbara E McArthur4, Otto Franz2, Larry H Wasserman2, Sergio Dieterich1

Institution(s): 1. Carnegie Institution of Washington, 2. Lowell Observatory, 3. RECONS Institute, 4. University of Texas

Applying Hubble Space Telescope Fine Guidance Sensor astrometric techniques developed to establish relative orbits for binary stars (Franz et al. 1998, AJ, 116, 1432), determine masses of binary components (Benedict et al. 2001, AJ, 121, 1607), and measure companion masses of exoplanet host stars (McArthur et al. 2010, ApJ, 715, 1203), we derive masses with an average 2% error for 28 components of 14 M dwarf binary star systems. With these and other published masses we update the lower Main Sequence V-band Mass-Luminosity Relation first shown in Henry et al. 1999, ApJ, 512, 864. We demonstrate that a Mass-Luminosity Relation in the K-band has far less scatter. These relations can be used to estimate the masses of the ubiquitous red dwarfs (75% of all stars) to an accuracy of better than 5%.