Computer Science
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006noao.prop..164c&link_type=abstract
NOAO Proposal ID #2006B-0164
Computer Science
Scientific paper
Determining accurate masses of Pre-Main-Sequence (PMS) stars is fundamental to our understanding of stellar formation and evolution. With only four sub-solar PMS masses of eclipsing binary stars presently known, the evolutionary tracks for low-mass stars, which dominate the Galactic stellar population, remain largely uncalibrated by empirical mass determinations. We have an intensive observing program underway to substantially increase the sample of low-mass PMS eclipsing binaries. Our program has produced three of the four sub-solar masses derived from eclipsing binaries including the first empirical mass measurement of the members of a brown dwarf binary system. We have recently identified a new low-mass eclipsing binary system, SM2654, in the Orion star-forming region. Our preliminary measurements provide evidence that this system is composed of at least two members with masses of M_primary=0.43M_sun +/- 0.04 and M_secondary=0.39M_sun +/- 0.04. We propose here to obtain the necessary observations for a complete photometric and spectroscopic analyze of this new PMS eclipsing binary system. Specifically we request high- resolution spectra using the HET/HRS providing a precise double-lined orbit.
Cargile Phillip
Mathieu Robert
Stassun Keivan G.
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