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Model of a magnetised star-disk system
Interaction between the magnetic field and the accretion disk
produces a gap between the disk and the stellar surface.
The dipolar structure becomes detached due to the accretion pressure.
Matter flows from the inner disk radius to the polar region
of the star. Two different model assumptions could be
considered: A high resistivity disk (left, "AMP"), where the
field does not penetrate the disk, and a low resistivity
disk (right, "ARP"), respectively. These assumptions
also determine the asymptotic behaviour of the jet solution.
(Figure adapted from Fendt, Ch., 1994, PhD thesis, Univ. of Heidelberg)
Historical note
The model of protostellar star-disk coupling and the connection
to jet formation has been first mentioned and published by
Max Camenzind (1990, Reviews in Modern Astronomy 3, 234-265, see
figure below) and later by Koenigl (1991, ApJ 370, L39),
Collier Cameron & Campbell (1993, A&A 274, 309) or
Shu and collaborators (1994, ApJ 429, 781).
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