Testing the 'clump' model of SiO maser emission |
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| Authors: | M D Gray R J Ivison E M L Humphreys & J A Yates |
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| Institution: | Department of Physics, University of Bristol, Tyndall Avenue, Bristol BS8 1TL,;Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ,;School of Chemistry, University of Bristol, Cantock's Close, Bristol BS8 1TS,;Department of Physical Sciences, University of Hertfordshire, College Lane, Hatfield AL10 9AB |
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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. |
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| Keywords: | masers binaries: symbiotic stars: individual: R Aqr radio lines: stars |
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