Testing the 'clump' model of SiO maser emission

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

    Research output: Contribution to journalArticlepeer-review


    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.
    Original languageEnglish
    Pages (from-to)970-976
    Number of pages6
    JournalMonthly Notices of the Royal Astronomical Society
    Issue number4
    Publication statusPublished - 21 Apr 1998


    • Binaries: symbiotic
    • Masers
    • Radio lines: stars
    • Stars: individual: R Aqr


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