Outflows from magnetic rotators II. Asymptotic structure and collimation

Details Outflows from magnetic rotators II. Asymptotic structure and collimation Outflows from magnetic rotators II. Asymptotic structure and collimation

1999-02-25

arxiv.org/abs/astro-ph/9902365v2

Astronomy and Astrophysics

Astrophysics

14 pages, LATEX, 16 figures, accepted by A&A

Scientific paper

The asymptotic structure of outflows from rotating magnetized objects confined by a uniform external pressure is calculated. The flow is assumed to be perfect MHD, polytropic, axisymmetric and stationary. The well known associated first integrals together with the confining external pressure, which is taken to be independent of the distance to the source, determine the asymptotic structure. The integrals are provided by solving the flow physics for the base within the framework of the model developed in Paper I (Lery et al. 1998), which assumes conical geometry below the fast mode surface, and ensures the Alfv\'en regularity condition. Far from the source, the outflow collimate cylindrically. Slow (i.e. with small rotation parameter $\omega$) rigid rotators give rise to diffuse electric current distribution in the asymptotic region. They are dominated by gas pressure. Fast rigid rotators have a core-envelope structure in which a current carrying core is surrounded by an essentially current free region where the azimuthal magnetic field dominates. The total asymptotic poloidal current carried away decreases steadily with the external pressure. A sizeable finite current remains present for fast rotators even at exceedingly small, but still finite, pressure.

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