Computer Science
Scientific paper
Feb 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007noao.prop..581s&link_type=abstract
NOAO Proposal ID #2007A-0581
Computer Science
Scientific paper
Our recent discovery of 2M0535-05-an eclipsing binary system in the Orion Nebula Cluster comprising two young brown dwarfs-provides the first direct, accurate measurements of the masses and radii of young sub-stellar objects. Surprisingly, our measurement of the temperature ratio in this system, based on an analysis of the eclipse light curve at 0.8 (mu)m, indicates that the less-massive brown dwarf is the hotter of the pair. This result is contrary to the predictions of all current theoretical models of coeval brown dwarfs. One interpretation is that there is no true temperature reversal, and that our analysis at 0.8 (micron) is being fooled by the complexity of brown-dwarf spectra and uncertainties in the bolometric corrections of young brown dwarfs. However, if the temperature reversal is confirmed by light-curve observations at multiple wavelengths, a second interpretation is that cool spots on the more massive brown dwarf cause its surface to have a lower effective temperature than predicted by the models. Here we propose to use GMOS on Gemini North and South in concert to obtain a precise light curve of 2M0535-05 at 0.45 (mu)m. Combined with our additional light curves at 1.2 and 2.2 (mu)m, this will permit a detailed multi-wavelength light-curve analysis in order to (1) definitively establish the temperature ratio of the system and, if the temperature reversal is confirmed, to (2) test the hypothesis that the more massive brown dwarf is heavily spotted. Until the true nature of the temperature reversal in 2M0535-05 is resolved, its utility as a fundamental benchmark for testing theoretical brown-dwarf formation and evolution models will be limited.
Mathieu Robert
Stassun Keivan G.
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