To the problem of solar coronal heating

Details To the problem of solar coronal heating To the problem of solar coronal heating

Mar 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007astl...33..182b&link_type=abstract

Astronomy Letters, Volume 33, Issue 3, pp.182-191

Astronomy and Astrophysics

Astronomy

3

Scientific paper

We consider the adequacy of various solar coronal heating models. We show that the correlation between the intensity of the coronal Fe XIV 530.5 nm green line and the calculated magnetic field strength in the solar corona can be a useful tool for this purpose. We have established this correlation for coronal structures and magnetic fields of large spatial and temporal scales. The correlation found exhibits a strong dependence on both solar cycle phase and heliolatitude. The efficiency of a particular coronal heating mechanism is probably determined by the relative area occupied by low and high loops (including open structures). The direct current models based on slow field dissipation (DC) and the wave models based on Alfvén and magnetosonic wave dissipation (AC) are more efficient in the equatorial and polar zones, respectively.

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