Volume 497, Number 1, April I 2009
|Page(s)||145 - 153|
|Section||Interstellar and circumstellar matter|
|Published online||09 February 2009|
Shocks in dense clouds
II. Dust destruction and SiO formation in J shocks
Institut d'Astrophysique Spatiale (IAS), Bâtiment 121, Université Paris-Sud 11 and CNRS, 91405 Orsay, France e-mail: email@example.com
Accepted: 28 January 2009
Context. Observations of SiO line emission in shocks in star-forming regions indicate that silicate dust destruction must be occurring in these dense regions. Current models rely on predictions for dust destruction by sputtering in C-type shock waves. However, J-type shocks may also be relevant for interpreting the widely-observed optical line emission from species such as O I and Fe II.
Aims. In this work we explore, for the first time, dust destruction in J-type shocks slower than 50 km s-1.
Methods. We follow the dust trajectories throughout the shock using a model for the dust dynamics that allows us to solve the shock structure and at the same time calculate the degree of dust processing. We include the effects of sputtering in gas-grain collisions, and vaporisation and shattering in grain-grain collisions.
Results. We find that the amount of silicon released into the gas phase is a few percent. The dominant destructive process is vaporisation, not sputtering. The degree of dust destruction increases with the shock velocity but decreases as the preshock density increases.
Conclusions. Our results compare well with that of C-type shock models. J-type shocks are therefore reasonable candidates for an interpretation of SiO line emission in molecular outflows and jets.
Key words: shock waves / magnetohydrodynamics (MHD) / dust, extinction / ISM: clouds / ISM: jets and outflows / ISM: evolution
© ESO, 2009
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