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The Molecular Envolope of Mira

Published online by Cambridge University Press:  12 April 2016

P. Planesas ,
R. Bachiller ,
J. Martín-Pintado  and
V. Bujarrabal
P. Planesas
Affiliation:
Centro Astronómico de Yebes, OAN-IGN, Spain
R. Bachiller
Affiliation:
Centro Astronómico de Yebes, OAN-IGN, Spain
J. Martín-Pintado
Affiliation:
Centro Astronómico de Yebes, OAN-IGN, Spain
V. Bujarrabal
Affiliation:
Centro Astronómico de Yebes, OAN-IGN, Spain

Extract

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We have mapped the CO J = 2 → 1 and J = 1 → 0 emission of the circumstellar envelope of Mira. Emission in both transitions extends to a distance of ~ 4 x 1016cm from the star. In the inner 2 x 1016cm the lines show the presence of three velocity components. The main component has the intermediate velocity and extends over the whole envelope. From this component we have estimated a mass loss rate of 3 x 107M⊙yr-1 and a total molecular mass of 1.2 x 10-3M⊙. We have shown that, from our data, the only reliable explanation for the lowest and highest velocity components is that they are due to an outflow located within the envelope.

Type
III. Discs, Outflows, Jets and HH Objects
Information
International Astronomical Union Colloquium , Volume 120: Structure and Dynamics of the Interstellar Medium , 1989 , pp. 306
Copyright
Copyright © Springer-Verlag 1989