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Centro de Astrofísica da Universidade do Porto

Collimation of astrophysical MHD Outflows

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

Abstract
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, Page 103
October 2003

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