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Time variations of water masers

Published online by Cambridge University Press:  03 August 2017

Tarja Liljeström  and
Carl R. Gwinn
Tarja Liljeström
Affiliation:
Helsinki University of Technology, Metsähovi Radio Observatory, Otakaari 5.A, FIN-02150 Espoo, Finland
Carl R. Gwinn
Affiliation:
University of California, Physics Department, Broida Hall Santa Barbara, CA 93106, USA

Abstract

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The strong water maser line at 22 GHz is an excellent tool for studying shocked and turbulent interstellar regions, especially, if simultaneous single-dish and VLBI data are available. After a brief review of 22 GHz time variation studies, we focus on effects caused by magnetic field pressure on observed properties of water masers. We use the powerful and rich maser cluster W49N as an example. Furthermore, we point out the connection between postshock wave damping and observed excess in single-dish flux density and line width.

Keywords

ISM: individual (W49N)ISM: magnetic fieldsmasersshock wavesturbulencewaves
Type
Part 1. Star Formation
Information
Symposium - International Astronomical Union , Volume 206: Cosmic Masers: From Protostars to Blackholes , 2002 , pp. 43 - 50
Copyright
Copyright © Astronomical Society of the Pacific 2002 

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