Kinematic solar dynamo models with a deep meridional flow

Details Kinematic solar dynamo models with a deep meridional flow Kinematic solar dynamo models with a deep meridional flow

2004-02-04

arxiv.org/abs/astro-ph/0402097v1

Mon.Not.Roy.Astron.Soc. 350 (2004) 317

Astronomy and Astrophysics

Astrophysics

7 pages, 6 figures, to be published in MNRAS

Scientific paper

10.1111/j.1365-2966.2004.07655.x

We develop two different solar dynamo models to verify the hypothesis that a deep meridional flow can restrict the apperance of sunspots below 45 degrees, proposed by Nandy & Choudhuri (2002). In the first one, a single polytropic approximation for the density profile was taken, for both radiative and convective zones. In the second one, two polytropes were used to distinguish between both zones Pinzon & Calvo-Mozo (2001). The magnetic buoyancy mechanism proposed by Dikpati & Charbonneau (1999) was chosen in both models. We, actually, have obtained that a deep meridional flow pushes the maxima of toroidal magnetic field toward the solar equator, but in contrast to Nandy & Choudhuri (2002) a second zone of maximal fields remains at the poles. The second model, although closely resembling the solar standard model of Bahcall, Pinsonneault & Wasserbug (1995); Bahcall, Pinsonneault & Basu (2001), gives solar cyles three times longer than observed.

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