Atomic Fine-Structure Lines from Protoplanetary Nebulae

Details Atomic Fine-Structure Lines from Protoplanetary Nebulae Atomic Fine-Structure Lines from Protoplanetary Nebulae

Nov 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000esasp.456..179c&link_type=abstract

ISO beyond the peaks: The 2nd ISO workshop on analytical spectroscopy. Eds. A. Salama, M.F.Kessler, K. Leech & B. Schulz. ESA-SP

Computer Science

1

Iso, Atomic Data, Stars: Agb And Post-Agb, Stars: Circumstellar Matter, Stars: Mass-Loss

Scientific paper

We have observed atomic fine-structure lines in the far-infrared (FIR) from protoplanetary nebulae (PPNe). The sample is composed of 24 objects, also including for comparison a few planetary nebulae and AGB stars. Data on OI, CII, NII, SiI, SiII, SI, FeI, and FeII lines were obtained. PPNe are found to emit in these low-excitation atomic transitions only when the central star is hotter than ~ 10,000 K. This result suggests that such lines predominantly arise from photodissociation regions (PDRs), and not from shocked regions. The line widths determined from our Fabry-Perot data also suggest that the FIR lines arise from relatively quiescent PDR gas as opposed to shocked gas. Our results are in reasonable agreement with predictions from PDR emission models, allowing the estimation of the density of the emitting layers from comparison with the model parameters. The CII line intensity has been used to measure the mass of the low-excitation atomic component in PPNe, since this transition has been found to be a useful model-independent probe to estimate the total mass of these PDRs.

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