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Levels of stabilization of velocity and magnetic induction in the convective zone of the Sun

Published online by Cambridge University Press:  23 December 2024

S. V. Starchenko Open the ORCID record for S. V. Starchenko [Opens in a new window]
S. V. Starchenko*
Affiliation:
IZMIRAN, Kaluzhskoe Hwy 4, Troitsk, Moscow, 108840 Russia
*
email: [email protected]
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Abstract

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The induction and momentum equations of solar dynamo are simplified to a dynamic system for the convective Root-Mean-Square (rms) velocity and the rms magnetic field in the solar convection zone. The study of stable stationary points of this system gives a minor excess of the critical level of the dynamo and, accordingly, moderate magnetic field typically about 1 T (10 kG). A significantly lower rms magnetic field may be possible at some parameters of the system. The stable rms velocity is about 100 m/sec, and the characteristic magnetic times are about the half-period of solar rotation or about an average lifetime of sunspots. Relative magnetic energy is of order 5 kJ/kg that is about the kinetic energy. The unstable stationary points could be near zero magnetic fields as in periods of very lower solar activity similar to the Maunder minimum.

Keywords

convective velocityconvective zonediffusion timeslevels of stabilizationmagnetic field valuesolar dynamo
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 19 , Symposium S365: Dynamics of Solar and Stellar Convection Zones and Atmospheres , December 2023 , pp. 364 - 367
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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