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Magnetic Flux Transport at the Solar Surface

  • Chapter
The Solar Activity Cycle

Part of the book series: Space Sciences Series of ISSI ((SSSI,volume 53))

  • 1434 Accesses

Abstract

After emerging to the solar surface, the Sun’s magnetic field displays a complex and intricate evolution. The evolution of the surface field is important for several reasons. One is that the surface field, and its dynamics, sets the boundary condition for the coronal and heliospheric magnetic fields. Another is that the surface evolution gives us insight into the dynamo process. In particular, it plays an essential role in the Babcock-Leighton model of the solar dynamo. Describing this evolution is the aim of the surface flux transport model. The model starts from the emergence of magnetic bipoles. Thereafter, the model is based on the induction equation and the fact that after emergence the magnetic field is observed to evolve as if it were purely radial. The induction equation then describes how the surface flows—differential rotation, meridional circulation, granular, supergranular flows, and active region inflows—determine the evolution of the field (now taken to be purely radial). In this paper, we review the modeling of the various processes that determine the evolution of the surface field. We restrict our attention to their role in the surface flux transport model. We also discuss the success of the model and some of the results that have been obtained using this model.

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Authors and Affiliations

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

    J. Jiang

  2. NASA/MSFC, Huntsville, AL, 35812, USA

    D. H. Hathaway

  3. Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077, Göttingen, Germany

    R. H. Cameron, S. K. Solanki & L. Gizon

  4. School of Space Research, Kyung Hee University, Yongin, Gyeonggi-Do, 446-701, Korea

    S. K. Solanki

  5. Institut für Astrophysik, Georg-August-Universität Göttingen, Friedrich-Hund-Platz 1, 37077, Göttingen, Germany

    L. Gizon

  6. Vanderbilt University, Nashville, TN, 37235, USA

    L. Upton

  7. The University of Alabama in Huntsville, Huntsville, AL, 35899, USA

    L. Upton

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  1. The Blackett Laboratory, Imperial College London, Hertfordshire, United Kingdom

    André Balogh

  2. Space Sciences Lab, University of California, Berkeley, California, USA

    Hugh Hudson

  3. Department of Astronomy, Eötvös University, Budapest, Hungary

    Kristóf Petrovay

  4. International Space Science Institute, Bern, Switzerland

    Rudolf von Steiger

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Jiang, J., Hathaway, D.H., Cameron, R.H., Solanki, S.K., Gizon, L., Upton, L. (2015). Magnetic Flux Transport at the Solar Surface. In: Balogh, A., Hudson, H., Petrovay, K., von Steiger, R. (eds) The Solar Activity Cycle. Space Sciences Series of ISSI, vol 53. Springer, New York, NY. https://doi.org/10.1007/978-1-4939-2584-1_17

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