Testing the ‘clump’ model of SiO maser emission

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, com...

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Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society 1998-04, Vol.295 (4), p.970-976
Main Authors: Gray, M. D., Ivison, R. J., Humphreys, E. M. L., Yates, J. A.
Format: Article
Language:English
Subjects:
binaries: symbiotic
masers
radio lines: stars
stars: individual: R Aqr
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Summary: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.
ISSN:0035-8711
1365-2966
DOI:10.1046/j.1365-8711.1998.01366.x