Theorical values of linear limb darkening coefficients for classical stars derived from models of their atmospheres.

Results of an analysis of several methods for determining linear limb darkening coefficients for classical stars indicate that the best approximation to the limb-darkening laws of a classical-star model is the linear approximation in which the total flux from the star is retained. It is also shown that, for the correct solution of light curves of classical eclipsing systems, the limb darkening coefficient is best determined as the brightness coefficient, which describes correctly brightness distribution across the disk of an eclipsing star. On the basis of a series of contemporary nongray atmospheric models, alternative tables are obtained for these limb-darkening coefficients for different temperatures and wavelengths.