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Evolution of low-mass star and brown dwarf eclipsing binaries
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Astronomy Astrophysics manuscript no. ms c? ESO 2008
February 1, 2008
Evolution of low-mass star and brown dwarf eclipsing binaries
Gilles Chabrier, Jose? Gallardo, Isabelle Baraffe
Ecole Normale Supe?rieure de Lyon, CRAL (UMR CNRS 5574), Universite? de Lyon, France
Received/Accepted
ABSTRACT
Context. We examine the evolution of low-mass star and brown dwarf eclipsing binaries. These objects are rapid rotators
and are believed to shelter large magnetic fields.
Aims. We suggest that reduced convective efficiency, due to fast rotation and large field strengths, and/or to magnetic
spot coverage of the radiating surface significantly affect their evolution, leading to a reduced heat flux and thus larger
radii and cooler effective temperatures than for regular objects.
Methods. We have considered such processes in our evolutionary calculations, using a phenomenological approach.
Results. This yields mass-radius and effective temperature-radius relationships in agreement with the observations. We
also reproduce the effective temperature ratio and the radii of the two components of the recently discovered puzzling
eclipsing brown dwarf system.
Conclusions. These calculations show that fast rotation and/or magnetic activity may significantly affect the evolution
of eclipsing binaries and that the mechanical and thermal properties of these objects depart from the ones of non-active
low-mass objects. We find that, for internal field strengths compatible with the observed surface value of a few kiloGauss,
convection can be severely inhibited. The onset of a central radiative zone for rapidly rotating active low-mass stars
might thus occur below the usual ~ 0.35M⊙ limit.
1. Introduction
Low-mass stars (LMS), i.e., M-type stars in the present
context, represent an overwhelming fraction of the Galactic
stellar population (Chabrier 2003). Observational determi-
nation of their mass-radius relationship
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