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Fundamental properties of low-mass stars in eclipsing binary systems

Published online by Cambridge University Press:  25 February 2014

J.C. Morales ,
I. Ribas  and
C. Jordi
J.C. Morales
Affiliation:
LESIA-Observatoire de Paris, CNRS, UPMC Univ. Paris 06, Univ. Paris-Diderot, 5 place Jules Janssen, 92195 Meudon Cedex, France Institut d'Estudis Espacials de Catalunya (IEEC), C/ Gran Capità 2-4, 08028 Barcelona, Spain
I. Ribas
Affiliation:
Institut de Ciències de l'Espai (CSIC-IEEC), Campus UAB – Facultat de Ciències, Torre C5-parell 2a planta, 08193 Bellaterra, Spain
C. Jordi
Affiliation:
Departament d'Astronomia i Meteorologia, Institut de Ciències del Cosmos (ICC), Universitat de Barcelona (IEEC-UB), C/ Martí i Franquès 1, 08028 Barcelona, Spain
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Abstract

Eclipsing binary systems offer a unique opportunity to accurately measure the fundamental properties of stars. In the past years, masses and radii of low-mass stars in these systems have been obtained with uncertainties well below the 3% level, imposing stringent constrains on theoretical models. Several results revealed that there is a discrepancy between the radius predicted by models and that from the observations of about 5–10% depending on the mass range. On the other hand, effective temperatures are overestimated by models by about a 10%. These discrepancies have been usually attributed to stellar magnetic activity, however, the correct scenario is not yet clear. The progress in the understanding of stellar activity on low-mass stars and its relation with the radius discrepancies with models is summarized here both from the empirical and the theoretical points of view.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 64: Setting a New Standard in the Analysis of Binary Stars , 2013 , pp. 103 - 110
Copyright
© EAS, EDP Sciences, 2014

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