Physics
Scientific paper
Aug 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999pcim.conf..395c&link_type=abstract
The Physics and Chemistry of the Interstellar Medium, Proceedings of the 3rd Cologne-Zermatt Symposium, held in Zermatt, Septemb
Physics
Scientific paper
The gas phase composition of regions surrounding star forming sites is strongly differentiated from that of cold interstellar clouds. Along the jets driven by young stellar objects, molecules such as SiO, NH _3, and CH _3 OH have fractional abundances highly enhanced relative to those in cold clouds. The hot and dense molecular cores surrounding newly formed massive stars give evidence of chemical processes in which complex organic molecules such as ethyl cyanide and methyl formate form. These peculiarities may be understood in terms of interaction between the gas and dust grains in those regions where shocks are able to destroy dust particles, and where the heating produced by embedded stars allows the grain mantles to evaporate and return to the gas phase. I will review recent work done in this field, in particular: (i) grain-grain collisions and sputtering in oblique C-type shocks, two efficient grain destruction mechanisms which inject refractory material and ice mantles into the gas phase along protostellar outflows; (ii) gas-grain chemical models in hot cores, where thermal effects can deeply affect the composition of grain mantles and gas phase abundances. Finally, problems related with current gas-grain chemical models are presented.
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