Abstract
The morphology and emissivity of shell-shaped bipolar outflows, driven by a spherically-symmetric stellar wind which interacts with a non-isotropically distributed cir-cumstellar gas within a dense molecular cloud, was estimated previously (Silvestro and Robberto, 1987) in the framework of the shell model of collimated outflows suggested by Barrai and Cantò (1981). Our computation allowed to obtain a spatial map of the profiles of the molecular lines emitted in the region of interaction between the wind and the circumstellar material. The position-velocity map of the rotational CO lines from the source Mon R2 turns out to be in very good agreement with the assumed thin-shell model for the outflowing lobe.
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References
Barrai, J.F. and Cantò, J., 1981, Rev. Mexicana Astron. y Astrof., 5, 101.
Kaplan, SA., 1966, Interstellar Gas Dynamics, Pergamon Press, Oxford, p. 83.
Rodriguez, L.F., 1987, in Star Forming Regions, IAU Symposium No. 115, p. 239.
Silvestro, G., Ferrari, A., Trussoni, E., Rosnet, R., and Tsinganos, K., 1987, Nature 325, 228.
Silvestro, G., and Robberto, M., 1987, in Circumstellar Matter, IAU Symposium No. 122, in press.
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© 1988 Kluwer Academic Publishers
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Robberto, M., Silvestro, G. (1988). A Thin- Shell Model for Molecular Outflows. In: Bianchi, L., Gilmozzi, R. (eds) Mass Outflows from Stars and Galactic Nuclei. Astrophysics and Space Science Library, vol 142. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-2941-8_44
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DOI: https://doi.org/10.1007/978-94-009-2941-8_44
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-7824-5
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