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Fig. 5


The rotation angle and fractional linear polarisation as a function of the magnetic field in the presence of anisotropic velocity-distribution functions with and without preferential acceleration. The full lines are the reference cases (solar outflow as given by the model by Wang et al. (1993), and an isotropic velocity-distribution function). The dotted curves have w/w = 2, while the broken lines have w/w = 1/2 with the usual outflow velocities. The curves with dots and lines have w/w = 2, while the ones with three dots and one line have w/w = 1/2 in the presence of slight preferential acceleration, i.e., twice as high a solar-outflow velocity of  ~43 km s-1.

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