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Correlations of magnetic features and the torsional pattern

Published online by Cambridge University Press:  26 August 2011

Judit Muraközy  and
András Ludmány
Judit Muraközy
Affiliation:
Heliophysical Observatory, H-4010 Debrecen P.O.Box 30, Hungary
András Ludmány
Affiliation:
Heliophysical Observatory, H-4010 Debrecen P.O.Box 30, Hungary
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Abstract

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The striking similarity between the cyclic equatorward migration of the torsional oscillation belts and the sunspot activity latitudes inspired several attempts to seek an explanation of the torsional phenomenon in terms of interactions between flux ropes and plasma motions. The aim of the present work is to examine the spatial and temporal coincidences of the torsional waves and the emergence of sunspot magnetic fields. The locations of the shearing latitudes have been compared with the distributions of certain sunspot parameters by using sunspot data of more than two cycles. The bulges of the sunspot number and area distributions tend to be located within the ‘forward’ belts close to their poleward shearing borders. A possible geometry of the magnetic and velocity field interacion is proposed.

Keywords

Torsional wavesunspots
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S273: The Physics of Sun and Star Spots , August 2010 , pp. 394 - 398
Copyright
Copyright © International Astronomical Union 2011

References

Antia, H. M. & Basu, S. 2001, Astrophys. J., 559, L67CrossRefGoogle Scholar
Győri, L., Baranyi, T., Ludmány, A. et al. 2010 Debrecen Photoheliographic Data http://fenyi.solarobs.unideb.hu/DPD/index.htmlGoogle Scholar
Howard, R. & LaBonte, B. J. 2005, Astrophys. J., 239, L33CrossRefGoogle Scholar
Howe, R., Christensen-Dalsgaard, J., Hill, , et al. 2000, Astrophys. J., 533, L163CrossRefGoogle Scholar
Komm, R. W., Hill, F., & Howe, R. 2001, Astrophys. J., 558, 428CrossRefGoogle Scholar
Kosovichev, A. G. & Schou, J., 1997, Astrophys. J., 482 L207CrossRefGoogle Scholar
Küker, M., Rüdiger, G., & Pipin, V. V. 2005, Astron. Astrophys, 312, 615Google Scholar
LaBonte, B. J. & Howard, R. 1982, Solar Phys., 75, 161CrossRefGoogle Scholar
Petrovay, K., Forgács - Dajka E. 2002, Solar Phys., 205, 39CrossRefGoogle Scholar
Schou, J., Antia, H. M., & Basu, S., et al. 1998, Astrophys. J., 505, 390CrossRefGoogle Scholar
Schüssler, M. 1981, Astron. Astrophys, 94, L17Google Scholar
Ulrich, R. K. & Boyden, J. E. 2005, Astrophys. J., 620, L123CrossRefGoogle Scholar
Yoshimura, H. 1981, Astrophys. J., 247, 1102CrossRefGoogle Scholar
Zhao, J. & Kosovichev, A. G. 2004, Astrophys. J., 603, 776CrossRefGoogle Scholar