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1 Introduction
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2 Observations of the IRV/SRV sample
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3 The Mira sample
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4 Modelling of circumstellar line emission
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5 CO modelling of the Miras
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6 Size of the SiO envelope
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7 Results of the SiO line model fits
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8 Discussion and conclusions
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Appendix A: Observational results
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Appendix B: Spectra
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References
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