Hostname: page-component-586b7cd67f-r5fsc Total loading time: 0 Render date: 2024-11-30T17:32:59.807Z Has data issue: false hasContentIssue false
  • English
  • Français

CM Draconis: Masses and Radii of Very Low Mass Stars

Published online by Cambridge University Press:  09 August 2007

J.C. Morales ,
I. Ribas ,
C. Jordi ,
G. Torres ,
E.F. Guinan  and
D. Charbonneau
J.C. Morales
Affiliation:
Institut d'Estudis Espacials de Catalunya, Barcelona, Spain email: [email protected] Dept. d'Astronomia i Meteorologia, Universitat de Barcelona, Barcelona, Spain email: [email protected]
I. Ribas
Affiliation:
Institut d'Estudis Espacials de Catalunya, Barcelona, Spain email: [email protected] Institut de Ciències de l'Espai – CSIC, Bellaterra, Spain email: [email protected]
C. Jordi
Affiliation:
Institut d'Estudis Espacials de Catalunya, Barcelona, Spain email: [email protected] Dept. d'Astronomia i Meteorologia, Universitat de Barcelona, Barcelona, Spain email: [email protected]
G. Torres
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA email: [email protected], [email protected]
E.F. Guinan
Affiliation:
Dept. of Astronomy, Villanova University, Villanova, PA, USA email: [email protected]
D. Charbonneau
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA email: [email protected], [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

In this work we have studied CM Draconis, one of the least massive eclipsing binaries known. Its components are very similar, with masses and radii of about 0.23 M⊙ and 0.25 R⊙. We have analysed light curves in the R and I bands to calculate the fundamental properties of this system with accuracies better than 1%. With these results we plan to carry out a thorough test of the models, which have been found to predict smaller radii and larger effective temperatures than observed for these low-mass stars. This will also be especially interesting in the case of CM Dra since the mechanism driving magnetic activity is thought to be different from that of more massive stars. In addition, the extended time-span of the observations has led to the detection of apsidal motion. This provides a further check on models through the determination of the internal structure of the stars.

Keywords

Binaries: eclipsingbinaries: spectroscopicstars: fundamental parametersstars: individual (CM Dra)techniques: photometric
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S240: Binary Stars as Critical Tools & Tests in Contemporary Astrophysics , August 2006 , pp. 628 - 630
Copyright
Copyright © International Astronomical Union 2007

References

Baraffe, I., Chabrier, G., Allard, F., Hauschildt, P.H. 1998, A&A 337, 403 Google Scholar
Chabrier, G., Küker, M. 2006, A&A 446, 1027 Google Scholar
Lacy, C.H. 1977, ApJ 218, 444 Google Scholar
Metcalfe, T.S., Mathieu, R.D., Latham, D.W., Torres, G. 1996, ApJ 456, 356 Google Scholar
Mullan, D.J., MacDonald, J. 2001, ApJ 559, 353 CrossRefGoogle Scholar
Ribas, I. 2006, astro-ph/0511431Google Scholar
Wilson, R.E., Devinney, E.J. 1971, ApJ 166, 605 Google Scholar