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

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

Mar 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009iaus..257..601y&link_type=abstract

Universal Heliophysical Processes, Proceedings of the International Astronomical Union, IAU Symposium, Volume 257, p. 601-603

Astronomy and Astrophysics

Astronomy

Magnetic Field, Solar Wind, Solar Cycle, Coronal Holes

Scientific paper

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.

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