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“Negative magnetic buoyancy” effects and reconstruction of toroidal field in the solar convection zone

Published online by Cambridge University Press:  01 August 2006

Valery N. Krivodubskij
Valery N. Krivodubskij*
Affiliation:
Astronomical Observatory of Kyiv National Taras Shevchenko UniversityObservatorna Street 3, Kyiv, 04053, Ukraine, email: krivod1@observ.univ.kiev.ua
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Abstract

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This investigation is devoted to study the turbulent convective transport of mean (large-scale) magnetic field in the solar convection zone (SCZ). For the SCZ model by Stix (1989) the reconstruction of the toroidal field was calculated as a result of the balance of mean-field magnetic buoyancy and two “negative magnetic buoyancy” effects: i) macroscopic turbulent diamagnetism and ii) the ∇ρ effect. It is shown that at high latitudes negative buoyancy effects block the magnetic fields, about 3000 – 4000 G, near the bottom of the SCZ. This may be the most plausible reason why a deep-seated field here could not become as apparent at the solar surface as sunspots. However, at the near equatorial domain in the deep layers the ∇ρ effect, with allowance for rotation, causes the upward magnetic transport, that facilitates penetration of strong fields to the surface where they emerge as sunspot patters in the “royal zone”.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S239: Convection in Astrophysics , August 2006 , pp. 502 - 504
Copyright
Copyright © International Astronomical Union 2007

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