Abstract
Mira (o Ceti), the prototypical Mira variable, due to its proximity (D = 128 +19−14 pc, van Leeuwen et al. 1997) is one of the best-studied red giant stars. Mira has an extended molecular envelope created by mass-loss, whose properties can be determined from studies of rotational emission lines from various molecules at millimeter and submillimeter wavelengths. The CO molecule is a particularly important probe because its has a relatively high abundance relative to hydrogen, [CO/H2] > 10−4, which is constant throughout large parts of the envelope, from the stellar photosphere, R star = 2.5 × 1013 cm, out to a radius R ~ 5 × 1016 cm. The bulk of the emission observed in a given rotational line arises from a limited certain part of the envelope, so that multi-transition studies allows us to determine temperature, density, and velocity profiles throughout the envelope, as well as an estimate of the mass-loss rate.
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© 1997 Springer Science+Business Media Dordrecht
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Crosas, M., Menten, K.M., Young, K., Phillips, T.G. (1997). Radiative Transfer in a Turbulent Expanding Molecular Envelope: Application to Mira. 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_25
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DOI: https://doi.org/10.1007/978-94-017-1307-8_25
Publisher Name: Springer, Dordrecht
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