AbstractWe have studied the solar magnetic cycle in corona using X-ray data from YOHKOH and Extreme Ultraviolet data from SOHO/EIT. Soft X-ray data last the period from after the maximum cycle 22 to the maximum cycle 23 (1991–2001). The SOHO/EIT Extreme Ultraviolet data are used for the period from 1996 to 2003. These data provide us a unique opportunity to look at the solar corona on the solar disc and to compare with the magnetic activity, directly.Our studies reveal a close relationship between the coronal emissions and the photospheric magnetic field in the axisymmetrical case. The evolution of coronal structures in X-ray and EUV can be considered as a proxy of the coronal magnetic field and demonstrates a development of the solar magnetic cycle in corona. It is shown that the most important feature of the coronal cycle is the forming of giant loops structure visible in X-ray and, partially, in EUV (284A) on the solar disk.
Solar X-ray and EUV corona and their relation to the magnetic activity
Advances in Space Research ; 39 , 9 ; 1491-1496
2007-04-05
6 pages
Aufsatz (Zeitschrift)
Elektronische Ressource
Englisch
Solar X-ray and EUV corona and their relation to the magnetic activity
Online Contents | 2007
|Connection of Structure White-Light Corona and Solar Activity
British Library Online Contents | 1997
|Measurement of magnetic helicity flux into the solar corona
Online Contents | 2003
|Measurement of Magnetic Helicity Flux Into the Solar Corona
British Library Conference Proceedings | 2003
|Measurement of magnetic helicity flux into the solar corona
Elsevier | 2003
|