Rotating models of A and F stars (Perez Hernandez+, 1999)

Details Rotating models of A and F stars (Perez Hernandez+, 1999) Rotating models of A and F stars (Perez Hernandez+, 1999)

Apr 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999ycat..33460586p&link_type=abstract

VizieR On-line Data Catalog: J/A+A/346/586. Originally published in: 1999A&A...346..586P

Physics

Models: Atmosphere, Stars: A-Type, Stars: F-Type, Photometry: Uvby, Photometry: Geneva, Photometry: Ubv

Scientific paper

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 Te and ge 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 Teff=Te, g=ge 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/Ωc, where Ω is the angular velocity of the star, and Ωc2=8GM/(27R3p), where M is the mass and Rp the polar radius. (2 data files).

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