Summary
Interstellar magnetic fields play certainly a distinct role in star formation and in galactic molecular disks. These magnetic fields are, however, also a key ingredient for accretion disks around young stellar objects and in the nuclei of galaxies. In these objects we find a strong observational link between accretion disks and bipolar outflows in the form of winds and jets.
In turbulent disks, the magnetic fields evolve according to the induction equation of mean field electrodynamics. In case of axisymmetric configurations, this leads to a coupled system of partial differential equations for the poloidal magnetic flux and the toroidal magnetic field including the effects of advection, spatial diffusion, differential rotation and helicity of the turbulence. In geometrically thin accretion disks, the lowest axisymmetric dynamo mode which can grow exponentially imtil equipartition with turbidence, is the quadrupolar field. Dipolar fields are found to decay exponentially.
The magnetic fields exterior to the disk have the structure of a rotating force-free magnetosphere. The shape of the poloidal field lines follows here from the solution of the relativistic Grad-Schlüter-Shafranov equation. The velocity and density in open magnetospheres is then essentially determined by the structure of the magnetic flux tubes. The luminosity of the wind is given by the magnetic luminosity of the disk surface. Magnetized winds ejected from the surface of the disk will be collimated by magnetic effects on scales typically larger than the light cylinder radius for these objects. The VLBI-jets of Quasars have therefore a radius of a fraction of a light year and reach a highly relativistic motion due to the extremely strong magnetization in the corona of the accretion disk. Protostellar jets have moderate velocities and jet radii of a few hundred AU.
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Camenzind, M. (1990). Magnetized Disk-Winds and the Origin of Bipolar Outflows. In: Klare, G. (eds) Accretion and Winds. Reviews in Modern Astronomy, vol 3. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-76238-3_17
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