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Table · dataset · 1999

Rotating models of A and F stars

Listed in IVOA Registry (Virtual Observatory)

Magnitude differences between rotating and non-rotating copartners for a grid of models with solar metallicity are tabulated here.

Description

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 = {Omega}/{Omega}_c_, where {Omega} is the angular velocity of the star, and {Omega}_c_^2^=8GM/(27R^3^_p_), where M is the mass and R_p_ the polar radius.

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Astronomical sciences 72%
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concepts[field].local:field:astronomymapping · IVOA Registryconnector:ivoa_registry@1.0.0
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