Low-Mass Stellar Mass-Luminosity-Radius Relation: Candidate M-dwarf Eclipsing Binary Stars in Open Clusters

Details Low-Mass Stellar Mass-Luminosity-Radius Relation: Candidate M-dwarf Eclipsing Binary Stars in Open Clusters Low-Mass Stellar Mass-Luminosity-Radius Relation: Candidate M-dwarf Eclipsing Binary Stars in Open Clusters

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...205.1801h&link_type=abstract

American Astronomical Society Meeting 205, #18.01; Bulletin of the American Astronomical Society, Vol. 36, p.1368

Astronomy and Astrophysics

Astronomy

Scientific paper

Open clusters, which have age, abundance, and extinction information from studies of main-sequence turn off stars, are the ideal location in which to determine the main sequence mass-luminosity-radius (M-L-R) relation for low-mass stars. We have undertaken a photometric monitoring survey of open clusters in the Galaxy designed to detect M-dwarf eclipsing binary systems through variations in their relative light curves. Our aim is to provide an improved calibration of the M-L-R relation for low-mass stars, to test stellar structure and evolution models, and to help quantify the contributin of low-mass stars to the global mass census in the Galaxy.
We have thus far detected two candidate M-dwarf type eclipsing systems in the open clusters. We are in the process of performing follow-up observations to confirm their binary nature and cluster membership and to obtain high time resolution light curves and radial velocity curves for these objects. If confirmed, the light curve information combined withe the radial velocity curves will allow for derivation of the masses and radii of the two components of the binary.

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