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Shock Chemistry in Bipolar Molecular Outflows

Published online by Cambridge University Press:  25 May 2016

R. Bachiller  and
M. Pérez Gutiérrez
R. Bachiller
Affiliation:
IGN Observatorio Astronómico Nacional, Apartado 1143, E-28800 Alcalá de Henares, Spain
M. Pérez Gutiérrez
Affiliation:
IGN Observatorio Astronómico Nacional, Apartado 1143, E-28800 Alcalá de Henares, Spain

Abstract

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Chemical studies have a great potential to study the structure and evolution of the bipolar molecular outflows driven by young stellar objects. In this paper, we discuss some very recent mm-wave studies of L 1157, a bipolar molecular outflow driven by a Class 0 protostar. These observations are very useful to illustrate the chemical alterations produced by a violent highly-collimated outflow. Different molecular lines are observed to trace different components of the gas. Some molecules are abundant in the quiescent medium but are not observed in the shock (e.g. C3H2, N2H+, H13CO+, DCO+), whereas some otherwise rare molecules are very enhanced at the shocked region (e.g. SiO, CH3OH, H2CO, HCN, CN, SO, SO2). In addition, we have observed strong gradients in the chemical composition across the outflow blue lobe. We briefly discuss the chemistry of the most important molecules, devoting special attention to the species which are thought to be abundant in interstellar ice mantles.

Type
II. The Physics and Chemistry of Molecular Outflows
Information
Symposium - International Astronomical Union , Volume 182: Herbig-Haro Flows and the Birth of Low Mass Stars , 1997 , pp. 153 - 162
Copyright
Copyright © Kluwer 1997 

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