| Issue |
A&A
Volume 426, Number 1, October IV 2004
|
|
|---|---|---|
| Page(s) | 297 - 307 | |
| Section | Stellar atmospheres | |
| DOI | https://doi.org/10.1051/0004-6361:20035930 | |
| Published online | 05 October 2004 | |
The angular sizes of dwarf stars and subgiants*
Surface brightness relations calibrated by interferometry
1
LESIA, UMR 8109, Observatoire de Paris-Meudon, 5 place Jules Janssen, 92195 Meudon Cedex, France e-mail: Pierre.Kervella@obspm.fr
2
European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, Vitacura, Santiago 19, Chile
3
Observatoire de la Côte d'Azur, BP 4229, 06304 Nice Cedex 4, France
4
European Southern Observatory, Karl-Schwarzschild-str. 2, 85748 Garching, Germany
5
Observatoire de Genève, 1290 Sauverny, Switzerland
Received:
22
December
2003
Accepted:
17
June
2004
The availability of a number of new interferometric measurements of
Main Sequence and subgiant stars makes it possible to
calibrate the surface brightness relations of these stars
using exclusively direct angular diameter measurements. These empirical laws make it possible to
predict the limb darkened angular diameters 
of dwarfs and subgiants
using their dereddened Johnson magnitudes, or their effective temperature.
The smallest intrinsic dispersions of 
in are obtained
for the relations based on the K and L magnitudes, for instance
or 
.
Our calibrations are valid between the spectral types A0 and M2 for dwarf stars
(with a possible extension to later types when using the effective temperature),
and between A0 and K0 for subgiants.
Such relations are particularly useful for estimating the angular sizes of calibrators for
long-baseline interferometry from readily available broadband photometry.
Key words: stars: fundamental parameters / techniques: interferometric
© ESO, 2004
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