Nonradial and nonpolytropic astrophysical outflows. V. Acceleration and collimation of self-similar winds

Details Nonradial and nonpolytropic astrophysical outflows. V. Acceleration and collimation of self-similar winds Nonradial and nonpolytropic astrophysical outflows. V. Acceleration and collimation of self-similar winds

2002-05-14

arxiv.org/abs/astro-ph/0205203v1

Astronomy and Astrophysics

Astrophysics

18 pages, 13 figures, accepted for publication in Astronomy and Astrophysics

Scientific paper

10.1051/0004-6361:20020684

An exact model for magnetized and rotating outflows, underpressured at their axis, is analysed by means of a nonlinear separation of the variables in the two-dimensional governing magnetohydrodynamic (MHD) equations for axisymmetric plasmas. The outflow starts subsonically and subAlfv\'enically from the central gravitating source and its surrounding accretion disk and after crossing the MHD critical points, high values of the Alfv\'en Mach number may be reached. Three broad types of solutions are found: (a) collimated jet-type outflows from efficient magnetic rotators where the outflow is confined by the magnetic hoop stress; (b) collimated outflows from inefficient magnetic rotators where the outflow is cylindrically confined by thermal pressure gradients; and (c) radially expanding wind-type outflows analogous to the solar wind. In most of the cases examined cylindrically collimated (jet-type) outflows are naturally emerging with thermal and magnetic effects competing in the acceleration and the confinement of the jet. The interplay of all MHD volumetric forces in accelerating and confining the jet is displayed along all its length and for several parameters. The solutions may be used for a physical understanding of astrophysical outflows, such as those associated with young stellar objects, planetary nebulae, extragalactic jets, etc.

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