The excitation mechanism and the line-to-continuum intensity ratio of the [Fe xiv] 5303 Å line in various coronal regions

Details The excitation mechanism and the line-to-continuum intensity ratio of the [Fe xiv] 5303 Å line in various coronal regions The excitation mechanism and the line-to-continuum intensity ratio of the [Fe xiv] 5303 Å line in various coronal regions

Oct 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993soph..147..255r&link_type=abstract

Solar Physics, Volume 147, Issue 2, pp.255-261

Physics

2

Scientific paper

The excitation mechanism of the coronal green line in various coronal regions is studied. The line-to-continuum intensity ratio is calculated using the model electron density values given by Newkirk (1961) and is compared with the observed values. Reasonably good agreement is found between the model calculations and observed values. The model calculations show that collisional excitation is more important in the innermost regions while radiative contribution progressively increases towards outer regions. The individual contributions depend strongly on the activity of the particular coronal region. An increased contribution from collisional excitation is seen in coronal active regions owing to the large electron density. A contour map of the line-to-continuum intensity ratio as derived from the observations, is plotted. At 1.10R&sun; the value is about 80 in active regions, 30 40 in coronal streamers, while it is less than 10 in polar regions.

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