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The Rotation of the Be Star γ Cas

Published online by Cambridge University Press:  12 April 2016

J. B. Hutchings
J. B. Hutchings*
Affiliation:
Dominion Astrophysical Observatory, Victoria, British Columbia, Canada

Abstract

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A period of 0.7 days has been found in the peak separation and VIR ratio of the double emission profiles of Hγ and Hβ in this star. The phenomenon is believed to arise from short lived condensations near the base of an equatorially extended atmosphere, and the period to be that of rotation of the star. The deduced stellar diameter is 7 R⊙. Further considerations on the emission line profiles lead to a model of an equatorial ring extending 1-2 stellar radii with angular velocity decreasing outwards, and viewed at an axial inclination of some 60°.

Type
Part III / Stellar Rotation in Binaries, Clusters, and Special Objects. Statistics of Stellar Rotation
Information
International Astronomical Union Colloquium , Volume 4: Stellar Rotation , 1970 , pp. 283 - 286
Copyright
Copyright © Reidel 1970

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