Other
Scientific paper
Nov 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000ign..confe..45p&link_type=abstract
Ionized Gaseous Nebulae. Mexico City November 21- 24, 2000, meeting abstract
Other
Scientific paper
The far infrared spectra of planetary nebulae have several important advantages. First, these spectral lines originate from levels so close to the ground level that the electron temperature (and possible temperature fluctuations) is unimportant. The resultant ionic abundances are thus independent of temperature. Second,there are many ions present which are not found in other observed spectral regions. Used in conjunction with the visual and ultraviolet observations, many more ions of a given element are present. This reduces the necessity to use 'ionization correction factors'. For several elements they are unimportant. This makes abundance determinations much more reliable. When both infrared lines and optical or UV lines of the same ion are present, both the ion abundance and the average electron temperature for that particular ion can be determined. In this way a plot of the electron temperature against ionization potential can be made, which helps greatly in determining abundances of ions not represented in the infrared. Results are given for seven nebulae, and are compared to other recent abundance determinations. It is shown that earlier determinations are sometimes in error: sometimes by a factor 1.5 to 2, occasionally by almost an order of magnitude.
Beintema Douwe A.
Pottasch Stuart R.
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