Magnetic Flux Transport at the Solar Surface

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 J. Jiang Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China E-mail: [email protected] D. H. Hathaway NASA/MSFC, Huntsville, AL 35812, USA E-mail: [email protected] R. H. Cameron Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany E-mail: [email protected] S. K. Solanki Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany and School of Space Research, Kyung Hee University,Yongin, Gyeonggi-Do,446-701, Korea E-mail: [email protected] L. Gizon Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany and Georg-August-Universität Göttingen, Institut für Astrophysik, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany E-mail: [email protected] L. Upton Vanderbilt University, Nashville, TN 37235 USA The University of Alabama in Huntsville, Huntsville, Al 35899 USA E-mail: [email protected]