Relationship between the brightness in the coronal green line and magnetic fields on various scales

The relationship between the brightness in the FeXIV 530.3 nm coronal green line and magnetic fields on various scales in the corona is studied quantitatively. The cross-correlations of the corresponding synoptic maps for 1977–2001 have been calculated. Maps of the brightness of the coronal green line are constructed using daily monitoring data. Maps of the magnetic field are constructed separately for fields on large and small spatial scales, based on computations in a potential approximation using photospheric observations for distances of 1.1R _⊙ carried out at the Wilcox Solar Observatory. The correlations between the brightness in the coronal green line and the magnetic-field strengths on various scales as a function of latitude have a cyclic character. The correlation coefficients in the spot-formation zone are positive. Here, the green-line brightness corresponds mainly to the strength of small-scale fields, corresponding to the sizes of large active regions and activity complexes. The correlation coefficients are sign-variable above 40° latitude, and reach their greatest positive and negative values at the cyclemaximum and minimum. Larger-scale fields influence the green-line brightness at higher latitudes and near the phase of the cycle minimum. The results obtained can be used to investigate mechanisms for heating the corona. The relationship between the results obtained and the subsurface and deep solar dynamos are also discussed.