The Magnetic Field and EUV Line Intensities in Solar Active Regions

Details The Magnetic Field and EUV Line Intensities in Solar Active Regions The Magnetic Field and EUV Line Intensities in Solar Active Regions

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003csss...12..220f&link_type=abstract

The Future of Cool-Star Astrophysics: 12th Cambridge Workshop on Cool Stars , Stellar Systems, and the Sun (2001 July 30 - Augus

Astronomy and Astrophysics

Astrophysics

2

Sun, Active Regions, Corona, Transition Region, Coronal Heating, Magnetic Field, Euv Emission

Scientific paper

Relationships between the photospheric magnetic flux and intensities of spectral lines emitted from the solar atmosphere have been extensively studied by several authors. Power-law relations have been found between the total magnetic flux and total intensities of the chromospheric, transition region and coronal emission lines in active regions. This approach is applied to extreme ultraviolet lines recorded by the Coronal Diagnostic Spectrometer (CDS) on SOHO for 50 solar active regions, as they crossed the central meridian in years 1996-1998. Four spectral lines are examined: ion{He}{1} 584.3 Å (2× 104 K), ion{O}{5} 629.7 Å (2.2 × 105 K), ion{Mg}{9} 368.06 Å (9.5 × 105 K), and ion{Fe}{16} 360.76 Å (2.0 × 106 K). In particular, the ion{Fe}{16} 360.76 Å line, seen only in areas of enhanced heating in active regions or bright points, has not been used before for this analysis. Empirical relations are established between the total active region intensity in ion{Fe}{16} and ion{O}{5} lines, and the total magnetic flux and between the spatially-averaged intensities and the magnetic flux density. The dependence of the coronal loop heating rate on the magnetic flux density is derived and its implications for the coronal heating models are discussed.

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