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A Three dimensional Babcock-Leighton Solar Dynamo Model with Non-axisymmetric Convective Flows

Published online by Cambridge University Press:  27 November 2018

Gopal Hazra  and
Mark S. Miesch
Gopal Hazra
Affiliation:
Dept. of Physics, Indian Institute of Science, Bangalore - 560012, India email: [email protected]
Mark S. Miesch
Affiliation:
National Oceanic and Atmospheric Administration, Boulder -80305, Colorado, USA email: [email protected]
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Abstract

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The observed convective flows on the photosphere (e.g., supergranulation, granulation) play a key role in the Babcock-Leighton (BL) process to generate large scale polar fields from sunspots fields. In most surface flux transport (SFT) and BL dynamo models, the dispersal and migration of surface fields is modeled as an effective turbulent diffusion. We present the first kinematic 3D FT/BL model to explicitly incorporate realistic convective flows based on solar observations. The results obtained are generally in good agreement with the observed surface flux evolution and with non-convective models that have a turbulent diffusivity on the order of 3 × 1012 cm2 s−1 (300 km2 s−1). However, we find that the use of a turbulent diffusivity underestimates the dynamo efficiency, producing weaker mean fields and shorter cycle.

Keywords

Sun: interiorSun: magnetic fieldsactivitySun: Photosphere
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S340: Long-term Datasets for the Understanding of Solar and Stellar Magnetic Cycles , February 2018 , pp. 301 - 302
Copyright
Copyright © International Astronomical Union 2018 

References

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