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Radiative Transfer in a Turbulent Expanding Molecular Envelope: Application to Mira

Crosas, Mercè and Menten, Karl M. and Young, Ken and Phillips, Thomas G. (1997) Radiative Transfer in a Turbulent Expanding Molecular Envelope: Application to Mira. In: Dust and Molecules in Evolved Stars. Springer , Dordrecht, pp. 189-192. ISBN 978-90-481-5018-2.

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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.

Item Type:Book Section
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URLURL TypeDescription ReadCube access ItemJournal Article
Menten, Karl M.0000-0001-6459-0669
Additional Information:© 1997 Springer Science+Business Media Dordrecht.
Subject Keywords:Radiative Transfer; Mass Loss Rate; Turbulent Velocity; Rotational Line; Dust Shell
Record Number:CaltechAUTHORS:20200716-130908517
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:104407
Deposited By: Tony Diaz
Deposited On:16 Jul 2020 21:30
Last Modified:16 Nov 2021 18:31

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