Convective overshoot at the base of the sun's convection zone

Details Convective overshoot at the base of the sun's convection zone Convective overshoot at the base of the sun's convection zone

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...157..338p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 157, no. 2, March 1986, p. 338-340.

Astronomy and Astrophysics

Astrophysics

25

Atmospheric Circulation, Convective Heat Transfer, Solar Atmosphere, Astronomical Models, Magnetic Flux, Magnetic Storage, Mixing Length Flow Theory, Solar Magnetic Field

Scientific paper

The non-local form of mixing length theory, as proposed by Shaviv and Salpeter (1973), is applied to the deeper part of the solar convection zone. The result is a layer of convective overshoot (with inward convective heat transport) which extends over a few tenths of a scale height, and has a boundary layer at its base where the temperature gradient suddenly changes from nearly adiabatic to the radiative value. The overshoot layer is part of a (slightly) sub-adiabatic region, of approximately one scale height thickness. The authors argue that this region should be capable to store sufficient magnetic flux, in the form of thin toroidal flux tubes, to account for the flux observed at the solar surface.

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