A New Detached M Dwarf Eclipsing Binary

 
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Creevey, O. L.
Benedict, G. F.
Brown, T. M.
Alonso, R.
Cargile, P.
Mandushev, G.
Charbonneau, D.
McArthur, B. E.
Cochran, W.
O'Donovan, F. T.
Jiménez-Reyes, S. J.
Belmonte, J. A.
Kolinski, D.
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https://doi.org/10.1086/431278
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Citation
Creevey, O. L., G. F. Benedict, T. M. Brown, R. Alonso, P. Cargile, G. Mandushev, D. Charbonneau, et al. 2005. “A New Detached M Dwarf Eclipsing Binary.” The Astrophysical Journal 625 (2): L127–30. https://doi.org/10.1086/431278.
Abstract
We describe a newly discovered detached M dwarf eclipsing binary system. This system was first observed by the TrES network during a long-term photometry campaign of 54 nights. Analysis of the folded light curve indicates two very similar components orbiting each other with a period of 1.12079 +/- 0.00001 days. Spectroscopic observations with the Hobby-Eberly Telescope show the system to consist of two M3e dwarfs in a near-circular orbit. Double-line radial velocity amplitudes, combined with the orbital inclination derived from light-curve fitting, yield M-total = 0.983 +/- 0.007 M-circle dot with component masses of M-1 = 0.493 +/- 0.003 M-circle dot and M-2 = The light-curve fit yields component radii of R-1 = 0.489 +/- 0.003 R-circle dot and R-2 = 0.452 +/- 0.050 R-circle dot. Although a precise parallax is lacking, broadband VJHK colors and spectral typing suggest component 0.050 absolute magnitudes of and. M (1) = 11.18 +/- 0.30 M (2) = 11.28 +/- 0.30.
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