Optical spectroscopy of carbon-rich proto-planetary nebulae

Details Optical spectroscopy of carbon-rich proto-planetary nebulae Optical spectroscopy of carbon-rich proto-planetary nebulae

Jan 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...438..341h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 438, no. 1, p. 341-349

Astronomy and Astrophysics

Astronomy

79

Abundance, Asymptotic Giant Branch Stars, Carbon, Infrared Spectra, Optical Emission Spectroscopy, Planetary Nebulae, Stellar Envelopes, Absorption Spectra, Emission Spectra, G Stars, Infrared Astronomy Satellite, Stellar Spectra, Supergiant Stars

Scientific paper

In this paper, we present a medium-resolution (3 A) spectroscopic study of six proto-planetary nebulae (PPN), post-asymptotic giant branch (AGB) objects with large infrared excesses. All six are found to display the spectra of G supergiants. However, they also show molecular carbon features, C2 and in most cases C3, and strong absorption lines due to s-process elements. Other evidences of a carbon-rich nature are found in published molecular-line millimeter emissions (CO and HCN) and 3.3 micrometer features attributed to polycyclic aromatic hydrocarbons. These properties are all in accord with what one would expect in a post-AGB star in which carbon-rich materials formed in thermal pulses is dredged up to the surface of a mass-losing object. A correlation is found between the presence of molecular C2 absorption and the presence of the unidentified 21 micrometer emission feature. This strengthens the suggestion that carbon is a major component of the molecule producing this unidentified feature. Four additional proto-planetary nebulae which share some of these properties are also discussed.

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