Abstract
Mass loss from M-Miras makes a major contribution to the injection of heavy elements into the interstellar medium and is a key stage in stellar evolution in which a late-type star embarks on its route towards the formation of a white dwarf. Recent VLBI images of SiO maser emission find that SiO masers lie in an incomplete ring around the host M-Mira (Diamond et al. 1994), stellar radius from the photosphere in the case of TX Cam, i.e. in the zone where mass loss is initiated. SiO masers show complicated and time-varying structure. With the new VLBI data and new hydrodynamic pulsation models and maser models, it is now possible to use SiO maser emission to examine critically our understanding of the mass loss mechanism in late-type stars.
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References
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© 1997 Springer Science+Business Media Dordrecht
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Humphreys, E.M.L., Gray, M.D., Field, D., Yates, J.A., Bowen, G. (1997). A Model for the Variability of SiO Masers in Mira Variables. In: Cherchneff, I., Millar, T.J. (eds) Dust and Molecules in Evolved Stars. Springer, Dordrecht. https://doi.org/10.1007/978-94-017-1307-8_31
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DOI: https://doi.org/10.1007/978-94-017-1307-8_31
Publisher Name: Springer, Dordrecht
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