Abstract
Outflows are evidently a common evolutionary phase for stars of all masses. The outflow phenomenon occurs within the first 105 years of a YSO’s life and is likely responsible for dispersing the dense gas surrounding it. The bulk of the high velocity molecular emission in an outflow arises from ambient cloud material swept up into an expanding shell by a faster, and more energetic stellar wind. This wind is largely neutral, atomic, and highly collimated into opposed jets. Finally, the energy and momentum carried away by the wind may have important consequences for both the star formation process and for the turbulent support of molecular clouds against gravity.
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Snell, R.L. (1989). Molecular outflows. In: Tenorio-Tagle, G., Moles, M., Melnick, J. (eds) Structure and Dynamics of the Interstellar medium. Lecture Notes in Physics, vol 350. Springer, Berlin, Heidelberg. https://doi.org/10.1007/BFb0114872
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DOI: https://doi.org/10.1007/BFb0114872
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