Volume 433, Number 3, April III 2005
|Page(s)||1023 - 1030|
|Section||Stellar structure and evolution|
|Published online||29 March 2005|
Differential rotation of main sequence F stars
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany e-mail: firstname.lastname@example.org
Accepted: 30 November 2004
The differential rotation of a 1.2 zero age MS star (spectral type F8) is computed and the results are compared with those from a similar model of the Sun. The rotation pattern is determined by solving the Reynolds equation including the convective energy transport. The latter is anisotropic due to the Coriolis force causing a horizontal temperature gradient of 7 K between the poles and the equator. Comparison of the transport mechanisms of angular momentum (the eddy viscosity, the -effect and the meridional flow) shows that for the F star the -effect is the most powerful transporter for rotation periods of 7 d or less. In the limit of very fast rotation the -effect is balanced by the meridional flow alone and the rotation is nearly rigid. The rotation pattern found for the F star is very similar to the solar rotation law, but the horizontal shear is about twice the solar value. As a function of the rotation period, the total equator-pole difference of the angular velocity has a (slight) maximum at a period of 7 d and (slowly) vanishes in both the limiting cases of very fast and very slow rotation. A comparison of the solar models with those for the F-type star shows a much str onger dependence of the differential surface rotation on the stellar luminosity r ather than on the rotation rate (see Fig. 6).
Key words: Sun: rotation / stars: rotation / convection
© ESO, 2005
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