Main sequence stars as calibrators for interferometry

Details Main sequence stars as calibrators for interferometry Main sequence stars as calibrators for interferometry

Oct 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004spie.5491.1174k&link_type=abstract

New Frontiers in Stellar Interferometry, Proceedings of SPIE Volume 5491. Edited by Wesley A. Traub. Bellingham, WA: The Intern

Physics

Scientific paper

We present in this paper new and accurate calibrations of the surface brightness-color relations that can be used to predict accurately the angular diameter of dwarf stars and subgiants. These stars present significant advantages as calibrators for interferometric observations. In many cases, they are more stable than giants and supergiants, as they are steadily burning their hydrogen. They are present in large numbers in the solar neighborhood, and offer a broad variety of colors. Their proximity allows to minimize the problems related to interstellar extinction in estimating their true magnitudes and colors. Excluding multiple stars, fast rotators and highly variable stars, it is possible to select reliable calibrators from spectro-photometric observations. Moreover, as opposed to the giant and supergiant stars, the photospheric diameter of dwarf stars is well defined and less sensitive to the assumed atmosphere models. In particular, the limb darkening related problems are alleviated at infrared wavelengths.

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