A numerical MHD model for the solar tachocline with meridional flow

Details A numerical MHD model for the solar tachocline with meridional flow A numerical MHD model for the solar tachocline with meridional flow

Jul 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005a%26a...437.1061s&link_type=abstract

Astronomy and Astrophysics, Volume 437, Issue 3, July III 2005, pp.1061-1067

Astronomy and Astrophysics

Astrophysics

11

Magnetohydrodynamics (Mhd), Sun: Interior, Sun: Magnetic Fields, Sun: Rotation

Scientific paper

There are successful approaches to explain the formation of the tachocline by a poloidal magnetic
field in the solar core. We present here the first MHD simulations of the solar tachocline which
self-consistently include the meridional circulation. We show that the meridional flow
significantly changes the shape and the characteristics of the tachocline. We find that after
the inclusion of the meridional circulation, a tachocline can be formed even when the poloidal
field lines are crossing the boundary between the radiative zone and the convection zone. We
also discuss the effects of the magnetic Prandtl number as well as of the magnetic Reynolds
number on the properties of the tachocline. The tachocline is much thinner for higher magnetic
Reynolds numbers and/or lower magnetic Prandtl numbers. We expect that a poloidal magnetic seed
field of around 1 G will be sufficient to produce the tachocline of the Sun. However, the model
requires the initial magnetic field to be in a narrow range to satisfy tachocline solutions. The
simulations including a stable temperature gradient produce a shallower as well as slower
meridional circulation than the ones without it, as required from the lithium abundance at the
solar surface.

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