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NLTT 41135: a field M-dwarf + brown dwarf eclipsing binary in a triple system, discovered by the MEarth observatory

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arxiv 1006.1793 v1 pith:KCWPTN5H submitted 2010-06-09 astro-ph.SR

NLTT 41135: a field M-dwarf + brown dwarf eclipsing binary in a triple system, discovered by the MEarth observatory

Jonathan Irwin , Lars Buchhave , Zachory K. Berta , David Charbonneau , David W. Latham , Christopher J. Burke , Gilbert A. Esquerdo , Mark E. Everett
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Matthew J. Holman Philip Nutzman Perry Berlind Michael L. Calkins Emilio E. Falco Joshua N. Winn John A. Johnson J. Zachary Gazak
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classification astro-ph.SR
keywords nlttbrowndwarfsystemcompanioneclipsingm-dwarfratio
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We report the discovery of an eclipsing companion to NLTT 41135, a nearby M5 dwarf that was already known to have a wider, slightly more massive common proper motion companion, NLTT 41136, at 2.4 arcsec separation. Analysis of combined-light and radial velocity curves of the system indicates that NLTT 41135B is a 31-34 +/- 3 MJup brown dwarf (where the range depends on the unknown metallicity of the host star) on a circular orbit. The visual M-dwarf pair appears to be physically bound, so the system forms a hierarchical triple, with masses approximately in the ratio 8:6:1. The eclipses are grazing, preventing an unambiguous measurement of the secondary radius, but follow-up observations of the secondary eclipse (e.g. with the James Webb Space Telescope) could permit measurements of the surface brightness ratio between the two objects, and thus place constraints on models of brown dwarfs.

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  1. On the Eccentricity Distribution and Tidal Evolution of Transiting Brown Dwarfs

    astro-ph.EP 2026-07 conditional novelty 6.0

    Short-period (P<16 d) transiting brown dwarfs are low-eccentricity while longer-period ones are more excited; assuming a shared primordial Beta distribution, tidal evolution constrains Q_BD ≈ 10^{7.1–8.1}.