Chemistry in a protoplanetary nebula

Details Chemistry in a protoplanetary nebula Chemistry in a protoplanetary nebula

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.255..217h&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 255, March 15, 1992, p. 217-226.

Astronomy and Astrophysics

Astronomy

21

Interstellar Chemistry, Planetary Nebulae, Protoplanets, Red Giant Stars, Stellar Winds, Astronomical Models, Interstellar Gas, Stellar Evolution

Scientific paper

Gas-phase chemistry in the remnant 'superwind' of a carbon-rich red giant star during its transition to a planetary nebula is investigated by means of the interacting stellar winds model. It is found that during the first few hundred years of transition, significant abundances of a few small molecules and ions may occur in the thin, dense, shocked shell of gas predicted by this model, but that most molecules observed in protoplanetary nebulae will be rapidly destroyed, through photodissociation by strong UV from the central star. The results support the view that the large abundances of heavy molecules observed in the young transition objects are either survivors from the red-giant superwind or produced by non-gas-phase processes, such as desorption from grains. If they are relics of the red-giant era, it is predicted that the abundances of such species in CRL 618 will fall, perhaps on a time scale of decades.

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