The Solar Neighborhood XXXVII: The Mass-Luminosity Relation for Main Sequence M Dwarfs
| Autor: | Wei-Chun Jao, Phillip A. Cargile, L. H. Wasserman, S. B. Dieterich, Barbara McArthur, Todd J. Henry, Edmund P. Nelan, Otto G. Franz, Arthur L. Whipple, Arthur J. Bradley, G. F. Benedict |
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| Jazyk: | angličtina |
| Rok vydání: | 2016 |
| Předmět: |
Physics
Orbital elements 010504 meteorology & atmospheric sciences Mass–luminosity relation FOS: Physical sciences Astronomy and Astrophysics Astrophysics Astrometry Astrophysics::Cosmology and Extragalactic Astrophysics 01 natural sciences Exoplanet Radial velocity Stars Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science Observatory 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics Astrophysics::Earth and Planetary Astrophysics Low Mass 010303 astronomy & astrophysics Solar and Stellar Astrophysics (astro-ph.SR) Astrophysics::Galaxy Astrophysics 0105 earth and related environmental sciences |
| Popis: | We present a Mass-Luminosity Relation (MLR) for red dwarfs spanning a range of masses from 0.62 Msun to the end of the stellar main sequence at 0.08 Msun. The relation is based on 47 stars for which dynamical masses have been determined, primarily using astrometric data from Fine Guidance Sensors (FGS) 3 and 1r, white-light interferometers on the Hubble Space Telescope (HST), and radial velocity data from McDonald Observatory. For our HST/FGS sample of 15 binaries component mass errors range from 0.4% to 4.0% with a median error of 1.8%. With these and masses from other sources, we construct a V-band MLR for the lower main sequence with 47 stars, and a K-band MLR with 45 stars with fit residuals half of those of the V-band. We use GJ 831 AB as an analysis example, obtaining an absolute trigonometric parallax, pi_abs = 125.3 +/- 0.3 milliseconds of arc, with orbital elements yielding MA = 0.270 +/- 0.004 Msun and MB = 0.145 +/- 0.002 Msun. The mass precision rivals that derived for eclipsing binaries. A remaining major task is the interpretation of the intrinsic cosmic scatter in the observed MLR for low mass stars in terms of physical effects. In the meantime, useful mass values can be estimated from the MLR for the ubiquitous red dwarfs that account for 75% of all stars, with applications ranging from the characterization of exoplanet host stars to the contribution of red dwarfs to the mass of the Universe. Accepted to the Astronomical Journal, 16 August 2016. Revised Title to state correct running number. XXXVIII -> XXXVII. Second rev now contains correct Table 13 Mv coefficients and offset. Last rev updates Figure 24 w/ higher resolution Baraffe models |
| Databáze: | OpenAIRE |
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