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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

References

Drobyshevskij, E.M. 1977 Astrophys. Space Sci. 46, 41–49.CrossRefGoogle Scholar
Kitchatinov, L.L. 1982 Magnitnaja Hidrodinamika (Riga) 3, 67–73.Google Scholar
Kitchatinov, L.L. 1991 Astron. Astrophys. 243, 483–491.Google Scholar
Kitchatinov, L.L. & Pipin, V.V. 1993 Astron. Astrophys. 274, 647–652.Google Scholar
Kitchatinov, L.L. & Rüdiger, G. 1992 Astron. Astrophys. 260, 494–498.Google Scholar
Krivodubskij, V.N. 2005 Astron. Nachr. 326, 64–71.CrossRefGoogle Scholar
Stix, M. 1989 The Sun, p. 200. Verlag, Berlin.CrossRefGoogle Scholar
Vainshtein, S.I. 1983 Magnitnye Polia v Kosmose, Nauka, Moscow.Google Scholar
Zeldovich, Y.B. 1956 Zh. Eksp. Teor. Fiz. (Moscow) 31, 154.Google Scholar
Zeldovich, Y.B., Ruzmaikin, A.A., & Sokoloff, D.D 1983 Magnetic Fields in Astrophysics, Gordon and Breach, New York.Google Scholar