Other
Scientific paper
Feb 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975phdt.........4g&link_type=abstract
Ph.D. Thesis Arizona Univ., Tucson.
Other
6
Astronomical Spectroscopy, Atomic Excitations, Line Spectra, Nebulae, Stellar Radiation, Carbon, Fluorescence, Ions, Neon, Nitrogen, Oxygen, Recombination Reactions, Resonance, Silicon, Sulfur
Scientific paper
Weak heavy element permitted lines observed in the spectra of gaseous nebulae were investigated. First, approximations and techniques of calculation were considered for the three possible excitation mechanisms: recombination and resonance fluorescence by the starlight continuum or by other nebular emission lines. Next, permitted lines of OI were studied. It was concluded that neither recombination nor resonance fluorescence by the Lyman lines can account for the strength of alpha 8446 and the presence of the other observed OI lines. However, resonance fluorescence by starlight can account for the strength of all the observed OI lines. Thirdly, it was shown that varying combinations of recombination and resonance fluorescence by starlight and other nebula lines can account for the observed strengths in the Orion Nebula of CII, NI, NII, NIII, OII, NeII, SiII, SiIII and SIII ions. A similar analysis was performed for the lines in the spectra of the planetary nebulae NGC7662 and NGC7027.
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