ISO observations of fine-structure atomic lines from proto-planetary nebulae

Details ISO observations of fine-structure atomic lines from proto-planetary nebulae ISO observations of fine-structure atomic lines from proto-planetary nebulae

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001esasp.460..257c&link_type=abstract

The Promise of the Herschel Space Observatory. Eds. G.L. Pilbratt, J. Cernicharo, A.M. Heras, T. Prusti, & R. Harris. ESA-SP 460

Computer Science

1

Atomic Data, Stars: Agb And Post-Agb, Stars: Circumstellar Matter, Stars: Mass-Loss, Ism: Planetary Nebulae

Scientific paper

We present ISO observations of fine-structure atomic lines from 24 evolved sources. Most of them are protoplanetary nebulae (PPNe) but we also include a few AGB stars and planetary nebulae. Data on O0, C+, N+, Si0, Si+, S0, Fe0 and Fe+ were obtained. PPNe are found to emit through low-excitation atomic lines only when the central star is hotter than ~ 10000 K. This result suggests that such lines predominantly arise from Photo-Dissociation Regions (PDRs). Our results are also 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. However, Fabry-Perot ISO observations suggest in some cases a contribution from shocked regions, in spite of their poor sensitivity and spectral resolution. The intensity of the [CII] 158 micron line has been used to measure the amount of low-excitation atomic mass in PPNe, since this transition has been found to be a useful model-independent probe to estimate the total mass of this component. In the most evolved sources the atomic mass is very high (up to ~ 1 Msun), representing in some cases the dominant nebular component.

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