VizieR Online Data Catalog: Rotating models of A and F stars (Perez Hernandez+, 1999)

Magnitude differences between rotating and non-rotating copartners for a grid of models with solar metallicity are tabulated here. The results are expressed in terms of the dimensionless angular velocity w-bar- defined in Eq.(1) of the paper, the angle of inclination i and the atmospheric parameters T_e and g_e defined in Eqs.(22) and (21), respectively. To obtain the absolute magnitudes for a given rotating model, the magnitudes of a non-rotating model with T_eff=T_e, g=g_e and the same intrinsic luminosity must be added. Results are given for the filters in the Geneva, Johnson and Stroemgren systems. Eq (1): w-bar = Ω/Ω_c, where Ω is the angular velocity of the star, and Ω_c²=8GM/(27R³_p), where M is the mass and R_p the polar radius. (2 data files).