The origin and structure of clumps along molecular outflows: the test case of CB3

Abstract

We investigate the origin of the small, chemically rich molecular clumps observed along the main axis of chemically rich outflows such as CB3 and L1157. We develop a chemical model where we explore the chemical evolution of these clumps, assuming they are partially pre-existing to the outflow, or alternatively newly formed by the impact of the outflow on the surrounding medium. The effects of the impact of the outflow are reproduced by density and temperature changes in the clump. We find that the observed abundances of CH3OH, SO and SO2 are best reproduced by assuming a scenario where the dense molecular gas observed is probably pre-existing in the interstellar medium before the formation of their exciting (proto)stars and that the clumpiness and the rich chemistry of the clumps are a consequence of a pre-existing density enhancement and of its interaction with the outflow.

arXiv comment11 pages, 5 figures, accepted by MNRAS; corrected label in figure 5

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• The B1 shock in the L1157 outflow as seen at high spatial resolution
• Organic species in Infrared Dark Clouds
• Molecular shock tracers in NGC 1068: SiO and HNCO
• 6.7GHz Methanol Maser Associated Outflows: An evolutionary sequence
• A study of methyl formate in astrochemical environments
• CSO and CARMA Observations of L1157. II. Chemical Complexity in the Shocked Outflow
• The Molecular Condensations Ahead of Herbig-Haro Objects. III. Radiative and dynamical perturbations of the HH 2 condensation
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• Class I methanol masers in low-mass star formation regions
• A detailed modelling of the chemically rich clumps along the CB3 outflow
• First images of phosphorus molecules towards a proto-Solar analog
• An observational survey of molecular emission ahead of Herbig-Haro objects
• Chemical and radiative transfer modeling of the ISO-LWS Fabry-Perot spectra of Orion-KL water lines