@article {39379,
	title = {Collimation of astrophysical MHD outflows},
	volume = {287},
	year = {2003},
	month = {2003/10/1},
	pages = {103 - 108},
	publisher = {Springer},
	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.},
	isbn = {0004-640X},
	url = {https://ui.adsabs.harvard.edu/abs/2003Ap\&SS.287..103T},
	author = {Tsinganos, K. and Vlahakis, N. and Bogovalov, S. and Sauty, C. and Trussoni, E. and Lima, J. J. G.}
}
