Solar cycle in the photosphere and corona

E. E. Benevolenskaya, A. G. Kosovichev, P. H. Scherrer

Research output: Contribution to journalConference articlepeer-review

2 Scopus citations

Abstract

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.

Original languageEnglish (US)
Pages (from-to)831-834
Number of pages4
JournalEuropean Space Agency, (Special Publication) ESA SP
Issue number506 II
StatePublished - Dec 1 2002
Externally publishedYes
EventThe 10th European Solar Physics Meeting; Solar Variability: From Core to Outer Frontiers - Prague, Czech Republic
Duration: Sep 9 2002Sep 14 2002

All Science Journal Classification (ASJC) codes

  • Aerospace Engineering
  • Space and Planetary Science

Keywords

  • EUV and X-ray corona
  • Magnetic flux
  • Solar cycle
  • Sun

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