Mid-infrared spectroscopy of planetary nebulae

Details Mid-infrared spectroscopy of planetary nebulae Mid-infrared spectroscopy of planetary nebulae

Dec 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984abas.symp..224s&link_type=abstract

In NASA. Ames Research Center Airborne Astron. Symp. p 224-232 (SEE N85-17848 08-89)

Astronomy and Astrophysics

Astronomy

1

Astronomical Spectroscopy, Flux (Rate), Infrared Spectra, Infrared Spectroscopy, Line Spectra, Planetary Nebulae, Stellar Spectra, C-141 Aircraft, Ions, Kinetic Energy, Molecular Excitation, Photons, Tables (Data), Temperature

Scientific paper

The application of infrared spectral lines observed in part of the broadened spectral range (18 to 36 microns) to planetary nebula studies is discussed. Infrared spectral lines in the mid-infrared supply information about planetary nebulae which both supplement and complement optical results. Their utility lies mainly in the insensitivity of the line intensities to temperature variations or uncertainties, in contrast to the behavior of optical emission. This in turn leads to more accurate ionic abundances than presently available from optical lines. Although densities from optical line ratios are not very sensitive to temperature, the lines are weighted toward regions of higher temperatures. A comparison with infrared densities from the same ions therefore provide clues to the density and/or temperature variations within nebulae. Temperatures from OIV and NeV ions show a part of high-excitation nebulae previously inaccessible. They verify the picture of physical processes in the HeIII zone.

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