EDP Sciences
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Volume 387, Number 1, May III 2002
Page(s) 187 - 200
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20020369

A&A 387, 187-200 (2002)
DOI: 10.1051/0004-6361:20020369

A global jet/circulation model for young stars

T. Lery1, 2, R. N. Henriksen3, J. D. Fiege4, T. P. Ray1, A. Frank5 and F. Bacciotti6

1  Dublin Institute for Advanced Studies, 5 Merrion Square Dublin 2, Ireland
2  GRAAL, CC 72, Université de Montpellier II, 34095 Montpellier Cedex 05, France
3  Department of Physics, Queen's University, Kingston, ON K7L 3N6, Canada
4  McLennan Labs, Univ. of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, Canada
5  Department of Physics and Astronomy, Univ. of Rochester, Rochester, NY 14627-0171, USA
6  Osservatorio Astrofisico di Arcetri, L.go E. Fermi 5, 50125 Firenze, Italy

(Received 6 March 2001 / Accepted 4 March 2002)

Powerful, highly collimated jets, surrounded by bipolar molecular outflows, are commonly observed near Young Stellar Objects (YSOs). In the usual theoretical picture of star formation, a jet is ejected from a magnetized accretion disk, with a molecular outflow being driven either by the jet or by a wider wind coming from the disk. Here, we propose an alternative global model for the flows surrounding YSOs. In addition to a central accretion-ejection engine driving the jet, the molecular outflow is powered by the infalling matter and follows a circulation pattern around the central object without necessarily being entrained by a jet. It is shown that the model produces a heated pressure-driven outflow with magneto-centrifugal acceleration and collimation. We report solutions for the three different parts of this self-similar model, i.e. the jet, the infalling envelope and the circulating matter that eventually forms the molecular outflow. This new picture of the accretion/outflow phase provides a possible explanation for several observed properties of YSO outflows. The most relevant ones are the presence of high mass molecular outflows around massive protostars, and a realistic fraction (typically 0.1) of the accretion flow that goes into the jet.

Key words: stars: formation -- methods: analytical -- magnetohydrodynamics (MHD) -- ISM: jets and outflows

Offprint request: T. Lery, Thibaut.Lery@graal.univ-montp2.fr

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