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3D evolution of solar magnetic fields and high-speed solar wind streams near the minimum of solar cycle 23

Published online by Cambridge University Press:  01 September 2008

O. S. Yakovchouk ,
I. S. Veselovsky ,
K. Mursula  and
Yu. S. Shugai
O. S. Yakovchouk
Affiliation:
Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow 119992, Russia email: [email protected]
I. S. Veselovsky
Affiliation:
Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow 119992, Russia email: [email protected] Space Research Institute (IKI), Russian Academy of Sciences, Moscow 117997, Russia
K. Mursula
Affiliation:
Department of Physical Sciences, University of Oulu, Oulu, 90014Finland
Yu. S. Shugai
Affiliation:
Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow 119992, Russia email: [email protected]
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Abstract

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The numerical method developed by Veselovsky & Ivanov (2006), together with magnetograms of the Sun obtained at the photospheric level were used to calculate the coronal magnetic field with open, closed and intermittent topology during March-December 2007. The results of the modelling are compared with stereoscopic images and movies of the corona observed by EUV telescopes onboard STEREO and SOHO spacecraft. The sources of the permanent and transient high speed solar wind streams as well as the sector structure and the heliospheric plasma sheet observed at the Earth's orbit by the ACE and STEREO spacecraft are discussed.

Keywords

Magnetic fieldSolar windSolar cycleCoronal holes
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S257: Universal Heliophysical Processes , September 2008 , pp. 601 - 603
Copyright
Copyright © International Astronomical Union 2009

References

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Obridko, V. N., Shelting, B. D., & Kharshiladze, A. F. 2006, Geomagn. Aeron., 46, 3, 294CrossRefGoogle Scholar
Veselovsky, I. S. 2002, Adv. Space Res., 29, 10, 1532Google Scholar
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Veselovsky, I. S. & Shugay, Yu. 2008, 37th COSPAR 2008. http://www.cospar-assembly.org/abstractcd/COSPAR-2008Google Scholar