Astronomy and Astrophysics – Astrophysics – Galaxy Astrophysics
Scientific paper
2009-01-13
Astrophys.J.695:149-155,2009
Astronomy and Astrophysics
Astrophysics
Galaxy Astrophysics
7 pages, 4 figures, accepted for publication in ApJ
Scientific paper
10.1088/0004-637X/695/1/149
We present the first results of the expected variations of the molecular line emission arising from material recently affected by C-shocks (shock precursors). Our parametric model of the structure of C-shocks has been coupled with a radiative transfer code to calculate the molecular excitation and line profiles of shock tracers such as SiO, and of ion and neutral molecules such as H13CO+ and HN13C, as the shock propagates through the unperturbed medium. Our results show that the SiO emission arising from the early stage of the magnetic precursor typically has very narrow line profiles slightly shifted in velocity with respect to the ambient cloud. This narrow emission is generated in the region where the bulk of the ion fluid has already slipped to larger velocities in the precursor as observed toward the young L1448-mm outflow. This strongly suggests that the detection of narrow SiO emission and of an ion enhancement in young shocks, is produced by the magnetic precursor of C-shocks. In addition, our model shows that the different velocity components observed toward this outflow can be explained by the coexistence of different shocks at different evolutionary stages, within the same beam of the single-dish observations.
Caselli Paola
Jiménez-Serra Izaskun
Martín-Pintado Jesús
Rodriguez-Franco Arturo
Viti Serena
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