The chemistry of protoplanetary nebulae

Details The chemistry of protoplanetary nebulae The chemistry of protoplanetary nebulae

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005esasp.577..229m&link_type=abstract

In: Proceedings of the dusty and molecular universe: a prelude to Herschel and ALMA, 27-29 October 2004, Paris, France. Ed. by A

Astronomy and Astrophysics

Astronomy

1

Protoplanetary Nebulae, Astrochemistry

Scientific paper

We discuss three recent attempts at modelling the chemical evolution of the post-AGB phase of stellar evolution, concentrating mostly on the short-lived protoplanetary nebula (PPNe) phase. Although the three models discussed differ in their physical description of PPN, all agree that the high densities, temperatures and UV fluxes can drive a complex organic chemistry on a very short timescale. For instance, O atoms liberated from CO, either by photodissociation or by shock waves, can be converted into OH and H2O, thereby producing oxygen-bearing molecules in a carbon-rich environment. However, once the molecular region becomes transparent to UV radiation, caused by geometrical dilution if this region is expanding, molecules are quickly destroyed; only the most photo-resistant species, and those which may exist in dense clumps, can survive to the planetary nebula phase.

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