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Water masers high resolution measurements of the diverse conditions in evolved star winds

Published online by Cambridge University Press:  07 February 2024

A. M. S. Richards*
Affiliation:
JBCA, Dept. Physics & Astronomy, University of Manchester, UK.
Y. Asaki
Affiliation:
JAO, Chile, NAOJ, Chile, Department of Astronomical Science, SOKENDAI, Japan
A. Baudry
Affiliation:
Université de Bordeaux, Laboratoire d’Astrophysique de Bordeaux, France
J. Brand
Affiliation:
INAF, Bologna, Italy
L. Decin
Affiliation:
Institute of Astronomy, KU Leuven, Belgium
S. Etoka
Affiliation:
JBCA, Dept. Physics & Astronomy, University of Manchester, UK.
M. D. Gray
Affiliation:
NARIT, Chiang Mai, Thailand
F. Herpin
Affiliation:
Université de Bordeaux, Laboratoire d’Astrophysique de Bordeaux, France
R. Humphreys
Affiliation:
Minnesota Institute for Astrophysics, University of Minnesota, USA
B. Pimpanuwat
Affiliation:
JBCA, Dept. Physics & Astronomy, University of Manchester, UK.
A. P. Singh
Affiliation:
Dept. of Chemistry, The University of Arizona, USA
J. A. Yates
Affiliation:
Dept. Physics & Astronomy, UCL, UK
L. M. Ziurys
Affiliation:
Dept. of Chemistry, The University of Arizona, USA
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Abstract

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We compare detailed observations of multiple H2O maser transitions around the red supergiant star VY CMa with models to constrain the physical conditions in the complex outflows. The temperature profile is consistent with a variable mass loss rate but the masers are mostly concentrated in dense clumps. High-excitation lines trace localised outflows near the star.

Type
Poster Paper
Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted re- use, distribution and reproduction, provided the original article is properly cited.
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

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