Seismic inference of differential rotation in Procyon A
INAF – Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy e-mail: firstname.lastname@example.org
2 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
3 Dipartimento di Fisica e Astronomia, Sezione Astrofisica, Università di Catania, via S. Sofia 78, 95123 Catania, Italy
Accepted: 2 October 2006
The differential rotation of the F5V-IV star Procyon A is computed for a class of models that are consistent with recent astrometric and asteroseismic data. The rotation pattern is determined by solving the Reynolds equation for motion, including the convective energy transport, which is anisotropic owing to the Coriolis force action that produces a horizontal temperature gradient between the poles and the equator. All the models show a decrease in the rotation rate with increasing radius and solar-type isorotation surfaces with the equator rotating faster than the poles, the horizontal rotational shear being much smaller for models with a less extended convective envelope. The meridional flow circulation can be either clockwise or counter-clockwise, and in some cases a double latitudinal cell appears. The rotational splittings are calculated for low-degree p-modes with , and ; and it is shown that, for modes with , the stronger the horizontal differential rotation shear, the weaker the effect on the average rotational splitting expected, whilst the opposite happens for the mode with . On the basis of the present study, a resolution of in individual oscillation frequencies seems to be necessary to test the different dynamical behaviour of the proposed models, which barely appears achievable even in the forthcoming space missions. However, the average over several observed splittings could produce the required accuracy.
Key words: stars: interiors / stars: evolution / stars: rotation / stars: oscillations / stars: individual: Procyon A
© ESO, 2007