Free Access

Fig. 4


The rotation angle and fractional linear polarisation as a function of the magnetic field in the presence of preferential acceleration. The higher the solar outflow, the more the plane of linear polarisation rotates. The upper curves (full lines) are reference cases for the normal solar outflows given by the model of Wang et al. (1993), the ones below (dotted curves) have their outflow velocity multiplied by two, the broken lines have their outflow velocities multiplied by three, the dot-line-dot curves have their outflow multiplied by four, and the lowest curves (three dots and one line) have the nominal value of the solar outflow multiplied by a factor of five.

This figure is made of several images, please see below:

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.