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The Physical and Chemical Effects of C-Shocks in Molecular Outflows

Published online by Cambridge University Press:  25 May 2016

G. Pineau Des Forêts ,
D.R. Flower  and
J.-P. Chièze
G. Pineau Des Forêts
Affiliation:
DAEC, Observatoire de Paris, F-92195 Meudon Principal Cedex, France
D.R. Flower
Affiliation:
Department of Physics, University of Durham, Durham DH1 3LE UK
J.-P. Chièze
Affiliation:
DSM/DAPNIA/Service d'Astrophysique, CE-Saclay, F-91191 Gif-sur-Yvette Cedex, France

Abstract

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The bow shocks which are observed in jets associated with low-mass star formation probably have C-shock characteristics over at least part of their extent. We show that ion-neutral streaming in C-type shocks can give rise to the release of significant amounts of silicon from the refractory cores of dust grains and hence to the formation of SiO in the gas phase. The computed profiles of SiO emission lines are found to be qualitatively similar to those observed in molecular outflow regions such as L1448. The question of the validity of the stationary-state assumption, adopted in all previous studies of C-shocks in the interstellar medium, is addressed. Time-dependent calculations of the evolution of a C-type shock propagating in low-density gas suggests that steady state is unlikely to be attained under the dynamical conditions in outflows.

Type
II. The Physics and Chemistry of Molecular Outflows
Information
Symposium - International Astronomical Union , Volume 182: Herbig-Haro Flows and the Birth of Low Mass Stars , 1997 , pp. 199 - 212
Copyright
Copyright © Kluwer 1997 

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