Theoretical models of planetary nebulae. V - Objects of intermediate-to-high excitation

Details Theoretical models of planetary nebulae. V - Objects of intermediate-to-high excitation Theoretical models of planetary nebulae. V - Objects of intermediate-to-high excitation

Apr 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ap%26ss..83..225a&link_type=abstract

Astrophysics and Space Science, vol. 83, no. 1-2, Apr. 1982, p. 225-238.

Astronomy and Astrophysics

Astrophysics

12

Astronomical Spectroscopy, Chemical Composition, Planetary Nebulae, Spectral Line Width, Stellar Models, Error Analysis, Forbidden Bands, Gas Ionization, H Lines, Nitrogen, Oxygen Ions, Stellar Radiation

Scientific paper

Using procedures previously described, theoretical models for 15 planetary nebulae of medium-to-high excitation are calculated. Initial stellar energy distributions are adopted from Cassinelli (1971) but are subsequently modified in order to obtain the best representation of optical spectra for the selected objects. Among other adjustable parameters are the stellar radius, the nebular density, the truncation radius for the nebular shell, and the chemical composition. Excitation-sensitive ratios are in most cases well represented, as are the actual observed intensities of spectral lines. Forbidden lines deriving from 3p3 configurations pose difficulties. For this sample of nebulae, the mean abundances are seen to agree well with those found in an earlier study in which the models were used as interpolation devices (Aller, 1978). The objective here is not to use the models to derive abundances explicitly but to use them to find ionization correction factors.

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