Solar cycle in the photosphere and corona

Details Solar cycle in the photosphere and corona Solar cycle in the photosphere and corona

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.506..831b&link_type=abstract

In: Solar variability: from core to outer frontiers. The 10th European Solar Physics Meeting, 9 - 14 September 2002, Prague, Cze

Physics

1

Sun, Magnetic Flux, Euv And X-Ray Corona, Solar Cycle

Scientific paper

EIT/SOHO data in four EUV lines and MDI/SOHO (1996-2002), and soft X-ray YOHKOH data (1991-2001) are analyzed in the form of coronal synoptic maps for the investigation of solar cycle variations of the corona and magnetic field. The evolution of coronal structures is closely related to sunspot activity, photospheric magnetic field, and topology of the large-scale magnetic field. The coronal structures visible in extreme ultraviolet and soft X-rays as extended bright loops, reflect the non-axisymmetrical magnetic structure of the Sun, changing with the solar cycle. The long-living coronal structures are related to complexes of solar activity and display the quasiperiodic behavior (impulses of coronal activity) with periods of 1.0-1.5 year in the axisymmetrical distribution of EUV and X-ray fluxes during the current cycle.

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