Journal Article

Testing the ‘clump’ model of SiO maser emission

M. D. Gray, R. J. Ivison, E. M. L. Humphreys and J. A. Yates

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 295, issue 4, pages 970-976
Published in print April 1998 | ISSN: 0035-8711
Published online April 1998 | e-ISSN: 1365-2966 | DOI: https://dx.doi.org/10.1046/j.1365-8711.1998.01366.x
Testing the ‘clump’ model of SiO maser emission

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Abstract

Building on the detection of the J=7−6 SiO maser emission in both the v=1 and v=2 vibrational states towards the symbiotic Mira R Aquarii, we have used the James Clerk Maxwell Telescope to study the changes in the SiO maser features from R Aqr over a stellar pulsational period. The observations, complemented by contemporaneous data taken at 86 GHz, represent a test of the popular thermal-instability clump models of SiO masers. The ‘clump’ model of SiO maser emission considers the SiO masers to be discrete emitting regions which differ from their surroundings in the values of one or more physical variables (SiO abundance, for example). We find that our observational data are consistent with a clump model in which the appearance of maser emission in the J=7−6 transitions coincides with an outward-moving shock impinging on the inner edge of the maser zone.

Keywords: masers; binaries: symbiotic; stars: individual: R Aqr; radio lines: stars

Journal Article.  0 words. 

Subjects: Astronomy and Astrophysics

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