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.
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Tsinganos, K., Vlahakis, N., Bogovalov, S. et al. Collimation of astrophysical MHD outflows. Astrophysics and Space Science 287, 103–108 (2003). https://doi.org/10.1023/B:ASTR.0000006208.62633.d0
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DOI: https://doi.org/10.1023/B:ASTR.0000006208.62633.d0