A New Detached M Dwarf Eclipsing Binary

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dc.creatorCreevey, O. L.
dc.creatorBenedict, G. F.
dc.creatorBrown, T. M.
dc.creatorAlonso, R.
dc.creatorCargile, P.
dc.creatorMandushev, G.
dc.creatorCharbonneau, D.
dc.creatorMcArthur, B. E.
dc.creatorCochran, W.
dc.creatorO'Donovan, F. T.
dc.creatorJiménez-Reyes, S. J.
dc.creatorBelmonte, J. A.
dc.creatorKolinski, D.
dc.date2005-04-22
dc.date2005-05-02
dc.date.accessioned2026-07-07T11:57:10Z
dc.date.available2026-07-07T11:57:10Z
dc.descriptionWe describe a newly-discovered detached M-dwarf eclipsing binary system, the fourth such system known. 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 Mass total = 0.983 +/- 0.007 solar masses, with component masses M(1) = 0.493 +/- 0.003 and M(2) = 0.489 +/- 0.003 solar masses. The light-curve fit yields component radii of R(1) = 0.453 +/- 0.060 and R(2) = 0.452 +/- 0.050 solar radii. Though a precise parallax is lacking, broadband VJHK colors and spectral typing suggest component absolute magnitudes of M_V(1) = 11.18 +/- 0.30 and M_V(2) = 11.28 +/- 0.30.
dc.description15 pages, 3 figure, 3 tables, accepted by ApJL, additional references
dc.identifierhttps://arxiv.org/abs/astro-ph/0504490
dc.identifierhttp://arxiv.org/abs/astro-ph/0504490
dc.identifierAstrophys.J.625:L127-L130,2005
dc.identifierdoi:10.1086/431278
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/205791
dc.subjectAstrophysics
dc.titleA New Detached M Dwarf Eclipsing Binary
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