The solar wind is a magnetized plasma and as such exhibits collective plasma behavior
associated with its characteristic spatial and temporal scales. The characteristic length …

In this review we will focus on a topic of fundamental importance for both astrophysics and
plasma physics, namely the occurrence of large-amplitude low-frequency fluctuations of the …

Magnetic reconnection, topological changes in magnetic fields, is a fundamental process in
magnetized plasmas. It is associated with energy release in regions of magnetic field …

Four different applications of spectral proper orthogonal decomposition (SPOD) are
demonstrated on large-eddy simulation data of a turbulent jet. These are: low-rank …

This paper summarises some of the recent progress that has been made in understanding
astrophysical plasma turbulence in the solar wind, from in situ spacecraft observations. At …

This paper presents a theoretical framework for understanding plasma turbulence in
astrophysical plasmas. It is motivated by observations of electromagnetic and density …

We show the first three dimensional (3D) dispersion relations and k spectra of magnetic
turbulence in the solar wind at subproton scales. We used the Cluster data with short …

We report the first direct determination of the dissipation range of magnetofluid turbulence in
the solar wind at the electron scales. Combining high resolution magnetic and electric field …

Solar wind is probably the best laboratory to study turbulence in astrophysical plasmas. In
addition to the presence of magnetic field, the differences with neutral fluid isotropic …

The proton temperature anisotropy in the solar wind is known to be constrained by the
theoretical thresholds for pressure-anisotropy-driven instabilities. Here, we use …