Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...322..296c&link_type=abstract
Astronomy and Astrophysics, v.322, p.296-301
Astronomy and Astrophysics
Astrophysics
92
Interstellar Medium: Clouds, Interstellar Medium: Dust, Extinction, Physical Processes: Shock Waves, Interstellar Medium: Jets And Outflows
Scientific paper
We use a model of the dissipation regions in C-type shocks in which two grain fluids are included to evaluate the rates at which grain-grain collisions and sputtering inject elemental silicon and water into the gas phase. For physical parameters typical of star forming regions, and on the assumption that a substantial fraction of the evaporated silicon is efficiently converted in SiO, the two grain destruction mechanisms lead to gas phase SiO abundances larger than those in the quiescent gas by more than three orders of magnitude. This result is in good agreement with recent observations of SiO near stellar jets. Grain-grain collisions will dominate the return of elemental silicon to the gas phase when the hydrogen nuclei number density of the region into which the shock is propagating is n_Ho_>5x10^5^cm^-3^ and the shock speed is between about 25km/s and 35km/s. Grain-grain collisions dominate over sputtering in the return of water to the gas phase when n_Ho_>10^6^cm^-3^ and at some shock speeds below about 15km/s.
Caselli Paola
Hartquist Thomas W.
Havnes Ove
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