Abstract
Recent studies suggest that flux‐tube‐like structures may exist in the solar wind. In this scenario, the solar wind plasma are confined in many individual flux tubes and plasma in these flux tubes move independently from each other. Within each flux tubes, the (MHD) turbulence is due to the local non‐linear dynamics. Across the boundaries between adjacent flux tubes, however, the (MHD) turbulence receives another contribution from the sudden change of magnetic field directions between different flux tubes. Thus the solar wind turbulence will naturally be of multiscale and intermittent. In this paper, using the procedure we developed in [1], we analyze magnetic field data obtained from Ulysses spacecraft in both fast and slow solar wind, at various radii and latitudes. Our results show flux tubes exist in both the fast and the slow solar wind.
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