Collimation of astrophysical MHD outflows

Authors: Tsinganos K.¹; Vlahakis N.²; Bogovalov S.³; Sauty C.⁴; Trussoni E.⁵; Lima J.J.G.⁶

Source: Astrophysics and Space Science, Volume 287, Numbers 1-4, 2003 , pp. 103-108(6)

Publisher: Springer

Buy & download fulltext article:

Price: $47.00 plus tax (Refund Policy)

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.

Keywords: MHD; solar wind; ISM; Stars: jets and outflows; galaxies: jets

Document Type: Research article

Affiliations: 1: Univ. of Athens, Dept of Physics, Panepistimiopolis, 157 84 Zografos, Greece;, Email: tsingan@phys.uoa.gr 2: Univ. of Athens, Dept of Physics, Panepistimiopolis, 157 84 Zografos, Greece;, Email: vlahakis@phys.uoa.gr 3: Astrophysics Institute of the Moscow State Engineering Physics Institute, Moscow, 11549, Russia;, Email: bogoval@axpk40.mephi.ru 4: Université Paris 7, APC, & Obs. de Paris, L.U.Th., 92190 Meudon, France;, Email: Christophe.Sauty@obspm.fr 5: INAF, Osservatorio Astron. Torino, Strada Osserv. 20, 10025 Pino Torinese, Italy;, Email: trussoni@to.astro.it 6: Centro Astrofísica, UP & DMA/FCUP, Rua das Estrelas, 4150 Porto, Portugal;, Email: jlima@astro.up.pt