Limb darkening coefficients for late-type giant model atmospheres

Details Limb darkening coefficients for late-type giant model atmospheres Limb darkening coefficients for late-type giant model atmospheres

Dec 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....61..809m&link_type=abstract

Astronomy and Astrophysics, vol. 61, no. 6, Dec. 1977, p. 809-813. Research supported by the Statens Naturvetenskapliga Forskni

Astronomy and Astrophysics

Astrophysics

66

Giant Stars, Late Stars, Limb Darkening, Stellar Atmospheres, Stellar Models, Supergiant Stars, Abundance, Atmospheric Models, Eclipsing Binary Stars, Plancks Constant, Rayleigh Distribution, Ubv Spectra

Scientific paper

Limb-darkening coefficients for UBV and uvby bandpasses have been calculated for selected late-type giant and supergiant model atmospheres from the grid given by Bell et al. (1976). These calculations have been carried out at mu values of 1.0, 0.8, 0.6, 0.4, 0.2, and 0.1; the synthetic spectra on which the colors are based were calculated at l-A resolution. The degree of limb darkening decreases with increasing temperature and with increasing wavelength. It is insensitive to surface gravity in the B and V ranges and increases slightly with gravity in the U. For effective temperatures of no more than 5000 K, the darkening increases with metal abundance, with the increase being more pronounced as one goes to shorter wavelengths. The calculations are used to study the effect of limb darkening on existing solutions for the cool giant eclipsing binaries RZ Cnc and AR Mon. Other possible applications are discussed.

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