Computer Science
Scientific paper
Oct 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.505..353b&link_type=abstract
In: SOLMAG 2002. Proceedings of the Magnetic Coupling of the Solar Atmosphere Euroconference and IAU Colloquium 188, 11 - 15 Jun
Computer Science
Solar Corona, Photospheric Magnetic Field, Solar Cycle
Scientific paper
The EIT/SOHO data in four EUV lines (1996-2001 yrs) and soft X-ray YOHKOH data (1991-2001 yrs) were analyzed in the form of coronal synoptic maps. Two types of the bright structures have been detected. The structures of the first type migrate equatorward as the solar cycle progresses. They are related to complexes of sunspot activity and display a "butterfly"-type distribution. The structures of the second type migrate polarward and are associated with footpoints of giant coronal loops in EUV, which magnetically couple the polar regions and the following parts of the active complexes. These structures of coronal activity are also pronounced in the soft X-ray maps. However, the whole structure of the giant polar loops is visible in X-rays, and reveal connections to the mid-latitude coronal structures. These structures appear during the rising phase of the solar cycle and its maximum, and show quasiperiodic impulsive variations with 1-1.5-year period. For the low- and mid-latitude structures we have studied the relationship between the soft X-ray intensity and the photospheric magnetic flux and found that it can be represented by the power law. However, the power index is higher for the period of the declining phase and minimum of solar activity than for its rising phase and maximum. This indicates that coronal heating has different characteristics at different phases of the solar cycle, and depends not only on the magnetic flux, but probably also on structural properties of the magnetic field.
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