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Maser polarization simulation in an evolving star: effect of magnetic field on SiO maser in the circumstellar envelope

Published online by Cambridge University Press:  07 February 2024

M. Phetra Open the ORCID record for M. Phetra [Opens in a new window] ,
M. D. Gray Open the ORCID record for M. D. Gray [Opens in a new window] ,
K. Asanok Open the ORCID record for K. Asanok [Opens in a new window] ,
B. H. Kramer ,
K. Sugiyama Open the ORCID record for K. Sugiyama [Opens in a new window] ,
S. Etoka Open the ORCID record for S. Etoka [Opens in a new window]  and
W. Nuntiyakul
M. Phetra*
Affiliation:
Graduate School, Chiang Mai University, Chiang Mai 50200. National Astronomical Research Institute of Thailand, Chiang Mai 50180, Thailand
M. D. Gray
Affiliation:
National Astronomical Research Institute of Thailand, Chiang Mai 50180, Thailand
K. Asanok
Affiliation:
National Astronomical Research Institute of Thailand, Chiang Mai 50180, Thailand
B. H. Kramer
Affiliation:
National Astronomical Research Institute of Thailand, Chiang Mai 50180, Thailand Max Planck Institute for Radio Astronomy, Auf dem Hügel 69, Bonn 53121, Germany
K. Sugiyama
Affiliation:
National Astronomical Research Institute of Thailand, Chiang Mai 50180, Thailand
S. Etoka
Affiliation:
Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, M13 9PL, UK
W. Nuntiyakul
Affiliation:
Department of Physics and Materials Science, Faculty of Science, Chiang Mai University, Chiang Mai 50200, Thailand
*
email: montree_ph@cmu.ac.th
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Abstract

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Maser polarization changes during a pulsation in the CSE of an AGB star are related in a complicated way to the magnetic field structure. 43 GHz SiO maser transitions are useful for polarization study because of their relatively simple Zeeman splitting structure and their location. This work uses 3D maser simulation to investigate the effect of the magnetic field on maser polarization with different directions. The results show that linear polarization depends on the magnetic direction while circular polarization is less significant. The EVPA changes through π/2 at an angle of around 50 degrees, approximately the Van Vleck angle. The EVPA rotation result from 3D maser simulation is consistent with results from 1D simulations, and may explain the 90 degree change of the EVPA within a single cloud in the observational cases of TX Cam and R Cas.

Keywords

AGB starmaser polarizationmaser simulation
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S380: Cosmic Masers: Proper Motion toward the Next-Generation Large Projects , December 2022 , pp. 435 - 439
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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