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 …

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 nature of small-scale turbulent fluctuations in the solar wind is investigated using a
comparison of Cluster magnetic and electric field measurements to predictions arising from …

The dissipation of magnetized turbulence is an important paradigm for describing heating
and energy transfer in astrophysical environments such as the solar corona and wind; …

We present a combined observational and theoretical analysis to investigate the nature of
plasma turbulence at kinetic scales in the Earth's magnetosheath. In the first decade of the …

We present three-dimensional, hybrid-kinetic numerical simulations of driven Alfvén-wave
turbulence of relevance to the collisionless near-Earth solar wind. Special attention is paid to …

The nature of subproton scale fluctuations in the solar wind is an open question, partly
because two similar types of electromagnetic turbulence can occur: kinetic Alfvén turbulence …

We investigate the radial dependence of the spectral break separating the inertial from the
dissipation range in power density spectra of interplanetary magnetic field fluctuations …

We use magnetic field and ion moment data from the MFI and SWE instruments on board the
Wind spacecraft to study the nature of solar wind turbulence at ion-kinetic scales. We …

We present a study of magnetic field fluctuations in a slow solar wind stream, close to ion
scales, where an increase of the level of magnetic compressibility is observed. Here, the …