<?xml version="1.0" encoding="UTF-8"?><xml><records><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Tsinganos, K.</style></author><author><style face="normal" font="default" size="100%">Vlahakis, N.</style></author><author><style face="normal" font="default" size="100%">Bogovalov, S.</style></author><author><style face="normal" font="default" size="100%">Sauty, C.</style></author><author><style face="normal" font="default" size="100%">Trussoni, E.</style></author><author><style face="normal" font="default" size="100%">Lima, J. J. G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Collimation of astrophysical MHD outflows</style></title><short-title><style face="normal" font="default" size="100%">Astrophysics and Space Science</style></short-title></titles><dates><year><style  face="normal" font="default" size="100%">2003</style></year><pub-dates><date><style  face="normal" font="default" size="100%">2003/10/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/2003Ap&amp;SS.287..103T</style></url></web-urls></urls><publisher><style face="normal" font="default" size="100%">Springer</style></publisher><volume><style face="normal" font="default" size="100%">287</style></volume><pages><style face="normal" font="default" size="100%">103 - 108</style></pages><isbn><style face="normal" font="default" size="100%">0004-640X</style></isbn><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">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.</style></abstract></record></records></xml>