Propagation of a dynamo field in the radiative interior of the Sun

Details Propagation of a dynamo field in the radiative interior of the Sun Propagation of a dynamo field in the radiative interior of the Sun

Apr 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999mnras.304..583g&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 304, Issue 3, pp. 583-588.

Astronomy and Astrophysics

Astronomy

17

Sun: Interior, Sun: Magnetic Fields

Scientific paper

Large-scale magnetic fields are believed to play an important role in the radiative zone of the Sun, in particular in the dynamical processes in the transition region between the convective and radiative zones (the tachocline). Also, they are probably responsible for the observed uniform rotation of the radiative zone. In that respect, since it has been suggested that the solar dynamo may lie near the outer edge of the tachocline, it is important to assess the question of how deep the dynamo field can penetrate, and whether it can influence significantly the dynamics of the solar interior. The magnetic cycle of the Sun is not strictly periodic, but undergoes random fluctuations in amplitude and phase. It is shown how the random fluctuations in the poloidal field diffuse into the radiative zone. An explicit solution for this diffusion process is given under certain simplifying assumptions. The result is then used together with some assumptions about the solar dynamo field to suggest that a field of order of 10^-1 G should be expected near the outer edge of the radiative zone, dropping rapidly to 10^-6 G beneath r=0.3 R_solar. This confirms the expectation that the dynamo field has a negligible effect on the dynamical processes taking place both in the tachocline and deeper in the radiative zone.

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