Coronal heating in active regions

Details Coronal heating in active regions Coronal heating in active regions

Jun 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.508..267f&link_type=abstract

In: Proceedings of the SOHO 11 Symposium on From Solar Min to Max: Half a Solar Cycle with SOHO, 11-15 March 2002, Davos, Switze

Computer Science

1

Coronal Heating, Magnetic Field, Active Regions, Euv Emission

Scientific paper

Many theoretical models of coronal heating predict a different dependence of the heating rate on the magnetic field strength. This property can be used to test these models by studying relationships between the photospheric magnetic flux and intensities of spectral lines emitted from the solar atmosphere. We use SOHO/MDI magnetograms and Extreme Ultraviolet lines recorded by the SOHO Coronal Diagnostic Spectrometer for 50 solar active regions, as they crossed the central meridian in years 1996-1998. We use two spectral lines: O V 629.7 Å (2.2×105K) and Fe XVI 360.76 Å (2.0×106K). We establish empirical power-laws between the total line intensity integrated over the active region area and the total magnetic flux, and derive the dependence of line intensities on the magnetic flux density for an average individual coronal loop. The heating rate is then derived as a function of the magnetic flux density and a comparison is made with the coronal heating models.

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