Spectrum and chemical analysis of the double-ring planetary nebula IC 1297

Details Spectrum and chemical analysis of the double-ring planetary nebula IC 1297 Spectrum and chemical analysis of the double-ring planetary nebula IC 1297

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...311..930a&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 311, Dec. 15, 1986, p. 930-936.

Other

11

Abundance, Line Spectra, Planetary Nebulae, Plasma Diagnostics, Spectrum Analysis, Astronomical Models, Astronomical Spectroscopy, Ultraviolet Spectra, Visible Spectrum

Scientific paper

The double-ring planetary nebula IC 1297 resembles NGC 7662 in appearance, although it is of much lower surface brightness. What is remarkable is the great strength of the dielectronic recombination O V line. Although this line is seen as a P Cygni feature in a number of planetary nebulae, it is in those instances accompanied by a strong continuum and other easily recognized features of stellar origin. No star is visible on CCD images of IC 1297. Optical region measurements are supplemented by IUE observations. The following logarithmic abundance values are found: log N(He) = 11.065; log N(forbidden C) = 8.6; log N(N) = 8.1; log N(O) = 8.74; log N(Ne) = 8.16; log N(S) = 7.0; log N(Cl) = 5.4; log N(Ar) = 6.2. The nebula shows no dramatic pattern of nucleogenesis events.

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