Comparisons of the green-line corona brightness with the magnetic field strength and the summary sunspot area

Details Comparisons of the green-line corona brightness with the magnetic field strength and the summary sunspot area Comparisons of the green-line corona brightness with the magnetic field strength and the summary sunspot area

Jun 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007coska..37..125b&link_type=abstract

Contributions of the Astronomical Observatory Skalnaté Pleso, vol. 37, no. 2, p. 125-141.

Astronomy and Astrophysics

Astronomy

Coronal Green Line Brightness, Area Of Sunspots, Magnetic Field Strength, Mutual And Solar Cycle Relations

Scientific paper

Comparisons of the Fe XIV 530.3 nm coronal emission line brightness with the summary area of sunspots and the magnetic field strength (extrapolated from the photospheric measurements to the 1.1 R&sun; distance in the corona), are discussed. Different correlations of the coronal green line brightness (CGLB) with the large-scale coronal magnetic fields and the local fields of sunspots are found during different solar cycle phases. At the ascending phase of activity the large-scale coronal magnetic fields dominate, whereas at the descending phase a somewhat higher correlation of the CGLB with the local magnetic fields of sunspots is observed. It is shown that within the ±40° solar low-latitude zone a portion of the CGLB originating due to the large scale magnetic field amounts to 25-30% in the period of solar cycle maximum but it goes up to 85% at the cycle minimum. Impact of the local sunspot fields on the CGLB level is remarkably lesser, it provides only 8-10% of the CGLB during cycle maximum and increases to about 18% at its minimum. Results of this paper could be helpful when testifying various models of the solar corona heating.

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