Collimation of astrophysical MHD Outflows

K. Tsinganos, N. Vlahakis, S. Bogovalov, C. Sauty, E. Trussoni, J. J. G. Lima

Resumo
We explain in simple terms why a rotating and magnetized outflow forms a core with a jet and show numerical simulations which substantiate this argument. The outflow from a solar-type inefficient magnetic rotator is found to be very weakly collimated while the outflow from a ten times faster rotating YSO is shown to produce a tightly collimated jet. This gives rise to an evolutionary scenario for stellar outflows. We also propose a two-component model consisting of a wind outflow from a central object and a faster rotating outflow launched from a surrounding accretion disk which plays the role of the flow collimator.

Astrophysics and Space Science
Volume 287, Página 103
outubro 2003

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