3-D structure of the complexes of solar activity

Details 3-D structure of the complexes of solar activity 3-D structure of the complexes of solar activity

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh13a..02b&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SH13A-02

Physics

2162 Solar Cycle Variations (7536), 7509 Corona, 7524 Magnetic Fields, 7536 Solar Activity Cycle (2162), 7549 Ultraviolet Emissions

Scientific paper

The typical complex of the solar activity persists on all levels of the solar atmosphere and consists of sunspots and surrounding plages in photosphere and chromosphere with arcades of loops visible in corona in Extreme Ultraviolet Emission and Soft X-ray. These coronal loops are the tracers of the lines of the magnetic field strength connected the magnetic areas with opposite polarities because of the complexes of solar activity are bipolar. The results of investigations of the evolution and the topology of the long-lived complexes of solar activity using SOHO/MDI and SOHO/EIT data for the period from 1996 to 2004 years are presented . We are discussing the nature of the existence of the long-lived complexes of solar activity.

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