Abstract
ABSTRACT A fundamental problem in space plasma physics and astrophysics is to understand the behaviour of magnetic field lines in turbulence. In the past it was controversial what aspects of turbulence are most important in field line random walk theory. In the current paper we employ numerical tools, commonly referred to as simulations, to gain more insight. In particular, we explore the importance of the energy range of the turbulence spectrum, spectral anisotropy, as well the existence of a component of the turbulent magnetic field parallel with respect to the mean magnetic field. The latter point is directly related to the question whether field line random walk in compressible turbulence behaves differently compared to random walk in incompressible turbulence.
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