Planetary nebulae. VI

Details Planetary nebulae. VI Planetary nebulae. VI

Apr 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984s%26w....23..178g&link_type=abstract

Sterne und Weltraum (ISSN 0039-1263), vol. 23, April 1984, p. 178-183. In German.

Computer Science

Emission Spectra, Line Spectra, Planetary Nebulae, Carbon, Chemical Composition, Cosmic Gases, Electron Density Profiles, Electron Energy, Excitation, Helium, Hydrogen, Nitrogen, Stellar Evolution

Scientific paper

The use of spectral lines to characterize the shells of planetary nebulae is reviewed and illustrated. Features discussed include electron temperature (usually 9000-16,000 K), electron density (1000-20,000/cu cm), and chemical composition (mainly H, with somewhat increased amounts of He and C and/or N relative to the theoretical cosmic frequency distribution of the elements). It is pointed out that the number of lines available for diagnostic purposes has been significantly increased in the far IR and far UV ranges by improved instrumentation and satellite observatories.

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