The overshoot layer at the base of the solar convective zone and the problem of magnetic flux storage

Details The overshoot layer at the base of the solar convective zone and the problem of magnetic flux storage The overshoot layer at the base of the solar convective zone and the problem of magnetic flux storage

Sep 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...113...99v&link_type=abstract

Astronomy and Astrophysics, vol. 113, no. 1, Sept. 1982, p. 99-112. Research supported by the Nederlandse Organisatie voor Zuiv

Physics

124

Convective Heat Transfer, Magnetic Flux, Solar Magnetic Field, Solar Physics, Coriolis Effect, Entropy, Layers, Solar Flux, Stellar Structure, Velocity Distribution

Scientific paper

Possibilities for storing a horizontal magnetic field in the overshoot layer at the base of the solar convective zone, or in the radiative zone below it, are studied using a one-dimensional model of the overshoot layer. The convective energy flux is estimated using a linear mode analysis. The thickness of the overshoot layer is found to be a few tenths of the pressure scale height, with an abrupt temperature gradient change at the base of the layer. Neutrally buoyant horizontal flux tubes, with an equipartition field strength greater than or about equal to 10 to the fourth Gauss, could be stabilized in the overshoot layer, but an additional force is needed to counteract the buoyancy force from an inflow of heat into the tubes. The Coriolis force on a mass flow along the toroidal flux with a flow velocity of 8 m/s may hold tubes with an equipartition field strength of about 10 to the fourth Gauss in the overshoot layer, and such flux tubes may be stable for solar cycle periods.

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