Spatial profiles of lines in active region loops

Details Spatial profiles of lines in active region loops Spatial profiles of lines in active region loops

Oct 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...88..155k&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 88, Oct. 1983, p. 155-161.

Physics

13

Coronal Loops, Line Shape, Solar Activity Effects, Solar Corona, Solar Spectra, Ultraviolet Spectra, Astronomical Models, Magnetic Field Configurations, Magnetohydrodynamic Turbulence, Plasma Turbulence, Solar Physics, Temperature Distribution

Scientific paper

From the statistical treatment of magnetohydrodynamically turbulent plasma, a steady-state density, temperature and magnetic field structure is derived for a coronal loop emitting in UV and EUV range. Spatial variation of line flux is presented for the lines C II, C III, O IV, O VI, Ne VII, and Mg X. It is found that the hotter lines which are emitted near the surface of the loop have larger spatial extents compared to the lines originating in the cool core of the loop, in agreement with the observations.

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