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Flux Transport Dynamos: From Kinematics to Dynamics

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Abstract

Over the past several decades, Flux-Transport Dynamo (FTD) models have emerged as a popular paradigm for explaining the cyclic nature of solar magnetic activity. Their defining characteristic is the key role played by the mean meridional circulation in transporting magnetic flux and thereby regulating the cycle period. Most FTD models also incorporate the so-called Babcock-Leighton (BL) mechanism in which the mean poloidal field is produced by the emergence and subsequent dispersal of bipolar active regions. This feature is well grounded in solar observations and provides a means for assimilating observed surface flows and fields into the models in order to forecast future solar activity, to identify model biases, and to clarify the underlying physical processes. Furthermore, interpreting historical sunspot records within the context of FTD models can potentially provide insight into why cycle features such as amplitude and duration vary and what causes extreme events such as Grand Minima. Though they are generally robust in a modeling sense and make good contact with observed cycle features, FTD models rely on input physics that is only partially constrained by observation and that neglects the subtleties of convective transport, convective field generation, and nonlinear feedbacks. Here we review the formulation and application of FTD models and assess our current understanding of the input physics based largely on complementary 3D MHD simulations of solar convection, dynamo action, and flux emergence.

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Notes

  1. The solutions are typically matched to an exterior potential field (Dikpati and Choudhuri 1995). A radial field surface boundary condition can also be used when matching with a surface flux transport model (see, e.g., Jiang et al. 2013).

  2. Note that Balbus and Schaan (2012) attribute the solar differential rotation to a meridional flow induced by centrifugal distortion of the base of the CZ. However, though this can influence the Ω profile, it cannot establish the equatorward Ω gradient observed in the Sun. For a discussion of this issue see the Appendix of Miesch et al. (2012).

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Acknowledgements

We wish to thank ISSI and its staff for their hospitality and a most stimulating workshop in November 2013. J.J. acknowledges the financial support by the National Natural Science Foundations of China (No. 11173033). M.S.M. is supported in part through grants MMH09AK14I, NNX11AJ36G, and NNX13AG18G. The National Center for Atmospheric Research is sponsored by the National Science Foundation of the U.S.A. P.C. is supported by the National Sciences and Engineering Research Council of Canada. The research of A.R.C. is supported by a JC Bose Fellowship awarded by the Department of Science and Technology of India.

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Authors and Affiliations

  1. NORDITA, KTH Royal Institute and Stockholm University, Roslagstullsbacken 23, 10691, Stockholm, Sweden

    Bidya Binay Karak

  2. Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, China

    Jie Jiang

  3. High Altitude Observatory, NCAR, Boulder, CO, 80307-3000, USA

    Mark S. Miesch

  4. Département de Physique, Université de Montréal, Montréal, QC, H3C-3J7, Canada

    Paul Charbonneau

  5. Department of Physics, Indian Institute of Sciences, Bangalore, 560012, India

    Arnab Rai Choudhuri

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Correspondence to Paul Charbonneau.

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Karak, B.B., Jiang, J., Miesch, M.S. et al. Flux Transport Dynamos: From Kinematics to Dynamics. Space Sci Rev 186, 561–602 (2014). https://doi.org/10.1007/s11214-014-0099-6

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