Solar Magnetic Fields and the Intensity of the Green Coronal Line

Details Solar Magnetic Fields and the Intensity of the Green Coronal Line Solar Magnetic Fields and the Intensity of the Green Coronal Line

Aug 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004arep...48..678b&link_type=abstract

Astronomy Reports, vol. 48, Issue 8, p.678-687

Astronomy and Astrophysics

Astronomy

5

Scientific paper

Synoptic maps of the intensity of the λ530.5 nm FeXIV green coronal line and maps of computed coronal magnetic fields for the period 1977 2001 are compared. For quantitative comparisons, the correlation coefficients r for the correlation between these two parameters at corresponding points of the synoptic maps are calculated. This coefficient exhibits cyclic variations in the spot-formation zone, ±30° and the zone above 30° and is in antiphase in these two zones. In the low-latitude zone, the correlation coefficient is always positive, reaches its maximum at activity minimum, and strongly decreases by activity maximum. Above 30°, r reaches maximum positive values at activity maximum and then gradually decreases, passing through zero near the beginning of the phase of activity minimum and becoming negative during this phase. A Fourier analysis of r as a function of time reveals a wavelike variation with a period close to 1.3 yr (known also from helioseismological data for the tachoclinic region of magnetic-field generation), as well as a pronounced wave with a period of about 5 yr. The latitude dependence of r seems to be related to variations in the contributions from local, large-scale, and global fields. Our analysis suggests an approach to studying the complex problem of mechanisms for coronal heating.

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