Differential rotation in stellar convective envelopes

Details Differential rotation in stellar convective envelopes Differential rotation in stellar convective envelopes

Nov 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997astl...23..731k&link_type=abstract

Astronomy Letters, Volume 23, Issue 6, November 1997, pp.731-734; Pis'ma v Astronomicheskii Zhurnal, Vol. 23, p. 838

Astronomy and Astrophysics

Astronomy

3

Scientific paper

The model for solar global circulation is used to calculate the differential rotation in stellar convective envelopes. The nonuniformity of angular velocity within the convection zone increases with rotation period and with stellar mass. For young stars that arrive at the main sequence, the model predicts a magnitude of the differential rotation of no more than 1%. As the rotation slows down with stellar age, this magnitude reaches >~ 10%. For main-sequence stars, we failed to find an example of simultaneously rapid and highly nonuniform rotation. This combination, however, can take place in giant stars of luminosity class III. Possible implications of the predictions of the model for stellar dynamo are discussed.

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