Shocks in dense clouds. II. Dust destruction and SiO formation in J shocks

Details Shocks in dense clouds. II. Dust destruction and SiO formation in J shocks Shocks in dense clouds. II. Dust destruction and SiO formation in J shocks

Apr 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009a%26a...497..145g&link_type=abstract

Astronomy and Astrophysics, Volume 497, Issue 1, 2009, pp.145-153

Astronomy and Astrophysics

Astrophysics

18

Shock Waves, Magnetohydrodynamics (Mhd), Dust, Extinction, Ism: Clouds, Ism: Jets And Outflows, Ism: Evolution

Scientific paper

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.

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