Abstract
The spectral composition and spatial distribution of equatorial coronal emission near 304 Å is examined. Spectral scans indicate that the predominant line is from Si xi. Comparisons of observations with calculations of intensity changes with altitude indicate that collisional excitation is important near the Sun but that photoexcitation becomes dominant beyond about 1.3 R ⊙ from the solar center. Observed and calculated intensities are in approximate agreement for abundances and electron densities that are within the range of observed values.
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Nakada, M.P., Chapman, R.D., Neupert, W.M. et al. OSO-7 results on coronal emission near 304 Å. Sol Phys 43, 337–350 (1975). https://doi.org/10.1007/BF00152358
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DOI: https://doi.org/10.1007/BF00152358