Be Stars Visibility Curve Constraints from Measurements with the CHARA Array Long Baseline Interferometer

Details Be Stars Visibility Curve Constraints from Measurements with the CHARA Array Long Baseline Interferometer Be Stars Visibility Curve Constraints from Measurements with the CHARA Array Long Baseline Interferometer

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.5711t&link_type=abstract

American Astronomical Society, AAS Meeting #211, #57.11; Bulletin of the American Astronomical Society, Vol. 39, p.832

Astronomy and Astrophysics

Astronomy

Scientific paper

Be stars are hot, non supergiant, B-spectral type stars that are rapidly rotating and ejecting mass into a circumstellar disk. These disks vary in time and have low densities that are responsible for the emission lines seen in the Be stars spectra. We will present the first results on Be stars from observations made with the long baseline CHARA/FLUOR interferometer at the Mount Wilson Observatory, obtained mainly for gamma Cas and zeta Tau in the K'-band. The projected baselines were 106 and 255 meters with position angles of 82 and 7 degrees respectively for gamma Cas, and 104 meters with a position angle of 88 degrees for zeta Tau. Our model of the interferometric visibilities predicts a base density of 7 x 10-11 g cm-3 for gamma Cas, and 2 x 10-10 g cm-3 for zeta Tau, which are comparable to results from IRAS measurments. Finally, we will present the result of including the effect of electron scattering (in addition to the bound-free and free-free opacity) on the visibility curves that are constrained by the observational data. Research at the CHARA Array is supported by the College of Arts and Sciences at Georgia State University and by the National Science Foundation through NSF Grants AST 0606958 and AST 0606861.

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