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Hydrodynamical Simulation of Bipolar Flows

Published online by Cambridge University Press:  04 August 2017

F. Clausset  and
F. Combes
F. Clausset
Affiliation:
Radioastronomy, Observatoire de Meudon, France
F. Combes
Affiliation:
Radioastronomy, Observatoire de Meudon, France

Extract

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High velocity bipolar gas flows are observed very frequently towards regions of star formation, and it has been conjectured that almost every star of mass larger than 1 M⊙ could undergo a phase of mass ejection during its formation (see e.g. Lada 1985). To explain the collimation of gas flows at interstellar scale, models have been proposed based on a stellar wind or violent isotropic ejection of matter by the protostar, that is pressure collimated by the molecular cloud in which it is embedded (Canto 1980, Königl 1982). In some cases, a molecular disk is observed perpendicular to the direction of the flow, but it is not quite sufficient to collimate it, see for example the high resolution CS observations of Takano et al. (1984) and Kawabe et al. (1984). Also, collimation occurs at a distance smaller than 3x1013m, according to the optical emission line observations of Mundt and Fried (1983).

Type
I. Star Forming Processes in the Solar Neighborhood
Information
Symposium - International Astronomical Union , Volume 115: Star Forming Regions , 1987 , pp. 378 - 379
Copyright
Copyright © Reidel 1987 

References

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