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Mass-Luminosity Relations of Very Low Mass Stars

Published online by Cambridge University Press:  26 May 2016

D. Ségransan ,
X. Delfosse ,
T. Forveille ,
J.L. Beuzit ,
C. Perrier ,
S. Udry  and
M. Mayor
D. Ségransan
Affiliation:
Observatoire de Genève, 51 ch des Maillettes, CH-1290 Sauverny, Switzerland
X. Delfosse
Affiliation:
Laboratoire d'Astrophysique de Grenoble, BP 53, F-38041 Grenoble, France
T. Forveille
Affiliation:
CFHT corp., P.O. Box 1597, Kamuela, HI 96743, USA
J.L. Beuzit
Affiliation:
Laboratoire d'Astrophysique de Grenoble, BP 53, F-38041 Grenoble, France
C. Perrier
Affiliation:
Laboratoire d'Astrophysique de Grenoble, BP 53, F-38041 Grenoble, France
S. Udry
Affiliation:
Observatoire de Genève, 51 ch des Maillettes, CH-1290 Sauverny, Switzerland
M. Mayor
Affiliation:
Observatoire de Genève, 51 ch des Maillettes, CH-1290 Sauverny, Switzerland

Abstract

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We present new accurate masses at the bottom of the main sequence as well as an improved empirical mass-luminosity relation for very low mass stars in the visible and near infrared. Masses were obtained by combining very accurate radial velocities and adaptive optics images of multiple stars obtained at different orbital phases.

Type
Part 7. Atmospheres and Internal Structure
Information
Symposium - International Astronomical Union , Volume 211: Brown Dwarfs , 2003 , pp. 413 - 416
Copyright
Copyright © Astronomical Society of the Pacific 2001 

References

Baraffe, I. et al. A&A, 337, 403, 1998.Google Scholar
Delfosse, X., 2000, A&A 364, 217, 2000 Google Scholar
Ségransan, D. et al., A&A 364, 665, 2000.Google Scholar
Forveille, T. et al., A&A 351, 619, 1999.Google Scholar