One characteristic trait of space plasmas is the multi-scale dynamics resulting from non-
linear transfers and conversions of various forms of energy. Routinely evidenced in a range …

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 …

Direct evidence for the presence of an inertial energy cascade, the most characteristic
signature of hydromagnetic turbulence (MHD), is observed in the solar wind by the Ulysses …

The physical foundations of the dissipation of energy and the associated heating in weakly
collisional plasmas are poorly understood. Here, we compare and contrast several …

The description of the local turbulent energy transfer and the high-resolution ion distributions
measured by the Magnetospheric Multiscale mission together provide a formidable tool to …

A dynamical vectorial equation for homogeneous incompressible Hall-
magnetohydrodynamic (MHD) turbulence together with the exact scaling law for third-order …

Solar wind plasma is known to cool down more slowly while it is blown away from the Sun
than expected from an adiabatic spherical expansion. Some source of heating is thus …

We present estimates of the turbulent energy-cascade rate derived from a Hall-
magnetohydrodynamic (MHD) third-order law. We compute the contribution from the Hall …

In the context of space and astrophysical plasma turbulence and particle heating, several
vocabularies emerge for estimating turbulent energy dissipation rate, including Kolmogorov …

The transfer of energy from large to small scales in solar wind turbulence is an important
ingredient of the long-standing question of the mechanism of the interplanetary plasma …