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Photospheric magnetoconvection

Published online by Cambridge University Press:  01 August 2006

Robert Cameron ,
Alexander Vögler  and
Manfred Schüssler
Robert Cameron
Affiliation:
Max-Planck Instute for Solar System Research, Katlenburg-Lindau, [email protected]
Alexander Vögler
Affiliation:
Max-Planck Instute for Solar System Research, Katlenburg-Lindau, [email protected]
Manfred Schüssler
Affiliation:
Max-Planck Instute for Solar System Research, Katlenburg-Lindau, [email protected]
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Abstract

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Magnetic fields, convective motions and radiative energy transport all strongly influence each other in the solar photosphere. Attempts to understand, at a quantitative level, the diverse phenomona seen in the photosphere have relied on increasingly powerful computers since the 1980's. This approach has been remarkably successful and some recent examples, particularly cases where all three ingredients are important, will be discussed.

Keywords

Convectionmagnetic fieldsradiative transferSun: photosphere
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S239: Convection in Astrophysics , August 2006 , pp. 475 - 481
Copyright
Copyright © International Astronomical Union 2007

References

Bercik, D.J., Nordlund, A. & Stein, R.F. 2003, GONG+ 2002. Local and Global Helioseismology: the Present and Future (ESA) SP-517 p. 201Google Scholar
Carlsson, M., Stein, R.F., Nordlund, Å. & Scharmer, G.B. 2004, Ap.J. 610, L137CrossRefGoogle Scholar
Cameron, R., Vögler, A., Schüssler, M. & Zakharov, V. 2005, 11th European Solar Physics Meeting. The dynamic Sun: Challenges for theory and observation (ESA) SP-600Google Scholar
Cameron, R., Vögler, A., Shelyag, S., & Schüssler, M. 2004, in: Sakurai, T. & Sekii, T. (eds) The Solar-B mission and the forefront of solar physics: The fifth Solar-B science meeting (ASP) 57Google Scholar
Cheung, M., 2006, PhD thesis, University of GöttingenGoogle Scholar
Keller, C.U., Schüssler, M., Vögler, A. & Zakharov, V. 2004, Ap.J., 607, L59CrossRefGoogle Scholar
Khomenko, E. V., Martínez González, M. J., Collados, M., Vögler, A., Solanki, S. K., Ruiz Cobo, B. & Beck, C., 2005, A&A, 436, L27Google Scholar
Khomenko, E. V., Shelyag, S., Solanki, S. K. & Vögler, A., 2005 A&A, 442, 1059Google Scholar
Nordlund, Å. 1982, A&A 107, 1Google Scholar
Nordlund, Å. 1982, in: Stenflo, J.O. (ed.) IAU Symp. 102. Solar and Stellar Magnetic fields: Origins and Coronal effects. 79CrossRefGoogle Scholar
Schüssler, M., Shelyag, S., Berdyugina, S., Vögler, A. & Solanki, S.K., 2003 Ap.J (Academic), 597, L173CrossRefGoogle Scholar
Schüssler, M. & Vögler, A., 2006 ApJ, 641, L73CrossRefGoogle Scholar
Stein, R. F. & Nordlund, Å., 2006 ApJ 642, 1246CrossRefGoogle Scholar
Sütterlin, P. 1998, A&A 333, 305Google Scholar
Vögler, , Shelyag, , Schüssler, , 2005, A&A 429, 335Google Scholar
Vögler, A., Shelyag, S., Schüssler, M., Cattaneo, F., Emonet, T. & Linde, T., 2005 A&A, 429, 335Google Scholar
Wedemeyer, S., Freytag, B., Steffen, M., Ludwig, H.-G. & Holweger, H., 2004, A&A, 414, 1121Google Scholar