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The dynamics of red supergiant winds

Published online by Cambridge University Press:  03 August 2017

Anita M. S. Richards ,
Raymond J. Cohen ,
Malcolm D. Gray ,
Koji Murakawa ,
Jeremy A. Yates ,
Marion Szymczak ,
John D. Monnier ,
Mike R. W. Masheder  and
Huib J. van Langevelde
Anita M. S. Richards
Affiliation:
JBO, University of Manchester, Macclesfield SK11 6TA, UK
Raymond J. Cohen
Affiliation:
JBO, University of Manchester, Macclesfield SK11 6TA, UK
Malcolm D. Gray
Affiliation:
Dept. of Physics, UMIST, PO Box 88, Manchester M60 1QD, UK
Koji Murakawa
Affiliation:
Dept. of Physical Sciences, University of Hertfordshire, AL10 9AB, UK
Jeremy A. Yates
Affiliation:
Dept. of Physical Sciences, University of Hertfordshire, AL10 9AB, UK
Marion Szymczak
Affiliation:
Torún Centre for Astronomy, ul. Gagarina 11, PL-87100, Poland
John D. Monnier
Affiliation:
Harvard-Smithsonian CfA, MS 42, Cambridge, MA, USA
Mike R. W. Masheder
Affiliation:
School of Physics, University of Bristol, Bristol, BS8 1TS, UK
Huib J. van Langevelde
Affiliation:
JIVE, Postbus 2, 7990 AA Dwingeloo, The Netherlands

Abstract

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During the red supergiant (RSG) stage of massive star evolution, emission from dust and molecules allows the copious stellar winds to be studied in great detail. This help us understand not only the evolutionary stages of the star (which are highly dependent on mass loss rates), but also the morphology of the eventual supernova remnant. Maser emission from OH and H2O has been mapped with milli-arcsec resolution (using MERLIN and the EVN/global VLBI) around RSG including VY CMa, S Per and VX Sgr. The H2O masers originate in clouds accelerating away from the star and OH mainlines masers interleave the outer parts of the H2O maser shell. Zeeman splitting of OH maser lines reveals the orientation and strength of stellar-centred magnetic fields.

Type
Part 2. Stellar Masers
Information
Symposium - International Astronomical Union , Volume 206: Cosmic Masers: From Protostars to Blackholes , 2002 , pp. 306 - 309
Copyright
Copyright © Astronomical Society of the Pacific 2002 

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