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URL: https://iopscience.iop.org/article/10.1086/503318

⇱ First Results from the CHARA Array. IV. The Interferometric Radii of Low-Mass Stars - IOPscience

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First Results from the CHARA Array. IV. The Interferometric Radii of Low-Mass Stars

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© 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A.
The Astrophysical Journal, Volume 644, Number 1Citation D. H. Berger et al 2006 ApJ 644 475DOI 10.1086/503318

D. H. Berger

AFFILIATIONS

CHARA Array, Mount Wilson Observatory, Mount Wilson, CA 91023

Current address: University of Michigan, Department of Astronomy, 500 Church Street, 917 Dennison Building, Ann Arbor, MI 48109-1042

D. R. Gies

AFFILIATIONS

Center for High Angular Resolution Astronomy, Georgia State University, P.O. Box 3969, Atlanta, GA 30302-3969

H. A. McAlister

AFFILIATIONS

Center for High Angular Resolution Astronomy, Georgia State University, P.O. Box 3969, Atlanta, GA 30302-3969

T. A. ten Brummelaar

AFFILIATIONS

CHARA Array, Mount Wilson Observatory, Mount Wilson, CA 91023

T. J. Henry

AFFILIATIONS

Center for High Angular Resolution Astronomy, Georgia State University, P.O. Box 3969, Atlanta, GA 30302-3969

J. Sturmann

AFFILIATIONS

CHARA Array, Mount Wilson Observatory, Mount Wilson, CA 91023

L. Sturmann

AFFILIATIONS

CHARA Array, Mount Wilson Observatory, Mount Wilson, CA 91023

N. H. Turner

AFFILIATIONS

CHARA Array, Mount Wilson Observatory, Mount Wilson, CA 91023

S. T. Ridgway

AFFILIATIONS

National Optical Astronomy Observatory, P.O. Box 26732, Tucson, AZ 85726

J. P. Aufdenberg

AFFILIATIONS

National Optical Astronomy Observatory, P.O. Box 26732, Tucson, AZ 85726

A. Mérand

AFFILIATIONS

LESIA, UMR8109, Observatoire de Paris-Meudon, 5 place Jules Janssen, 92195 Meudon Cedex, France

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Dates

  1. Received 2005 September 30
  2. Accepted 2006 February 9
0004-637X/644/1/475

Abstract

We have measured the angular diameters of six M dwarfs with the CHARA Array, a long-baseline optical interferometer located at Mount Wilson Observatory. Spectral types range from M1.0 V to M3.0 V and linear radii from 0.38 to 0.69 R☉. These results are consistent with the seven other M dwarf radii measurements from optical interferometry and with those for 14 stars in eclipsing binary systems. We compare all directly measured M dwarf radii to model predictions and find that current models underestimate the true stellar radii by up to 15%-20%. The differences are small among the metal-poor stars but become significantly larger with increasing metallicity. This suggests that theoretical models for low-mass stars may be missing some opacity source that alters the computed stellar radii.

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10.1086/503318