Solar Dynamo Surface Waves in the Presence of a Primordial Magnetic Field: an Upper Estimate of the Field in the Solar Core.

Details Solar Dynamo Surface Waves in the Presence of a Primordial Magnetic Field: an Upper Estimate of the Field in the Solar Core. Solar Dynamo Surface Waves in the Presence of a Primordial Magnetic Field: an Upper Estimate of the Field in the Solar Core.

Jan 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phdt.........9b&link_type=abstract

Thesis (PH.D.)--THE UNIVERSITY OF CHICAGO, 1995.Source: Dissertation Abstracts International, Volume: 56-05, Section: B, page: 2

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Scientific paper

Helioseismological measurements have recently shown that the vertical gradient in angular velocity is confined to a thin layer in the overshoot region just below the convective zone of the sun. A solar dynamo operating in this configuration exhibits surface (or interface) wave properties and is confined primarily to just below the convective/shear boundary. A fixed primordial magnetic field bound to the radiative core is observed to be modified at the solar surface by the dynamo and found to be a sensitive function of the shear layer thickness h. If the solar dynamo operates as an alphaomega surface dynamo, then based on current observations of solar cycle asymmetry and allowing for the present uncertainty in the value for h, an upper bound of 0.15 to 0.5 Gauss for the primordial magnetic field magnitude at the bottom of the convective zone is calculated. By comparing the age of the sun with the solar decay time for a magnetic field initially trapped in the solar core we estimate the magnetic field in the interior of the sun's core to have an upper magnitude of around 32 Gauss.

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