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Strong magnetic fields in bipolar outflows

Published online by Cambridge University Press:  03 August 2017

M. D. Smith ,
P. W. J. L. Brand  and
A. Moorhouse
M. D. Smith
Affiliation:
Dept. of Physics, University of Durham
P. W. J. L. Brand
Affiliation:
Dept. of Astronomy, University of Edinburgh
A. Moorhouse
Affiliation:
Dept. of Mathematics, UMIST

Abstract

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A supersonic wind from a young star will produce regions of strong magnetic field in the stellar environment. The associated shocks compress the molecular gas, increasing the density n, pressure p, and field B. Crucially, the Alfvén speed, v A ∝ B/n1/2, is also increased since the total shock compression is approximately of the form B ∝ n. But is there any evidence for such high v A - or ‘active cloud’ - regions within bipolar outflows? We indicate below one implication which has important observable consequences: fast shocks of low Alfvén number (v/v A ) now arise. With a low ionization level, the C-shock structure is qualitatively different from the high Alfvén number flows which are common to ‘quiescent cloud’ conditions. The magnetic-field cushioning now allows molecular hydrogen to survive very fast shocks and broad H2 lines are feasible. We display results which show that the resolved broad lines and line ratio properties in the OMC-1 outflow can be explained with fast bow shocks moving through such active regions.

Type
Early Stages of Stellar Evolution
Information
Symposium - International Astronomical Union , Volume 147: Fragmentation of Molecular Clouds and Star Formation , 1991 , pp. 373 - 376
Copyright
Copyright © Kluwer 1991 

References

Brand, P.W.J.L., Moorhouse, A., Burton, M.G., Geballe, T.R., Bird, M., & Wade, R., 1988. Astrophys. J. Letters 334, L103.Google Scholar
Brand, P., Toner, M.P. et al. 1989. M.N.R.A.S. 236, 929.Google Scholar
Brand, P., Toner, M.P. et al. 1989. M.N.R.A.S. 237, 1009.Google Scholar
Draine, B.T., Roberge, W.G. & Dalgarno, A., 1983. Ap. J., 264, 485.Google Scholar
Smith, M.D. & Brand, P.W.J.L., 1990a. M.N.R.A.S. 242, 495.Google Scholar
Smith, M.D. & Brand, P.W.J.L., 1990b. M.N.R.A.S. 245, 108.CrossRefGoogle Scholar
Smith, M.D., Brand, P.W.J.L. & Moorhouse, A., 1990a & 1990b. M.N.R.A.S. submitted Google Scholar