The Support of the Envelopes of be Stars

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Abstract

The nature of the support of the envelopes of Be stars is explored. The different forces that appear to deserve consideration are examined systematically and the importance of each in accounting for the observed support is estimated. Independent observational evidence concerning the dependence of the circular velocity for one of these envelopes upon distance from the parent star's rotation axis is also ex- amined, as are two arguments of a more general nature that bear upon the problem. It is concluded that the support of an envelope of this kind is centrifugal and that the viscous agent that is necessary to pro- vide the required transfer of angular momentum from the star to the envelope is one that results either from magnetic fields that couple the two or from the turbulence that is expected to develop in such a differentially rotating envelope. It is shown that turbulence can play a major role only if the turbulence is moderately supersonic; whether such turbulence can develop and is consistent with the observations is not yet clear. Magnetic field remains a prime candidate for the required viscous agent even though the case for its importance is largely circumstantial

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