Solar Coronal Structures in Extreme Ultraviolet and Soft X-rays and Their Relation to Magnetic Flux

Details Solar Coronal Structures in Extreme Ultraviolet and Soft X-rays and Their Relation to Magnetic Flux Solar Coronal Structures in Extreme Ultraviolet and Soft X-rays and Their Relation to Magnetic Flux

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh11c0720b&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH11C-0720

Physics

7509 Corona, 7524 Magnetic Fields, 7536 Solar Activity Cycle (2162), 7549 Ultraviolet Emissions, 7554 X Rays, Gamma Rays, And Neutrinos

Scientific paper

The large-scale coronal structures are ultimately related to internal magnetic fields and thus provide important information about the solar dynamo. We have investigated the relationship between magnetic activity and coronal structures using EUV data from SOHO/EIT and X-ray data from Yohkoh/SXT, and magnetic field data from Kitt Peak and Wilcox Solar Observatories for the period 1996-2000 years. We discuss the non-uniform distribution of coronal heating and its connection with long-lived complexes of solar activity during the current cycle. EUV images reveal two sets of migrating structures of coronal activity in the time-latitudinal distribution of the EUV intensity in 171A, 195A, 284A and 304A EIT wavelength channels. The low-latitude coronal structures, migrating equatorward, correspond to photospheric sunspot activity, and the high-latitude structures migrating towards the poles reflect polar activity of the sun. The polar branches are cooler then the equatorial branches. This is reflected in the time-latitudinal distribution of the soft X-rays in two filters (Al and AlMg). We discuss the physical properties and nature of these structures of coronal activity and their role in the solar cycle.

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