Solar wind is a highly turbulent medium exhibiting fluctuations ranging from the solar
sidereal rotation period to proton and electron gyroperiods. Their amplitudes show …

We live in an age in which high-performance computing is transforming the way we do
science. Previously intractable problems are now becoming accessible by means of …

Turbulent plasmas generate a multitude of thin current structures that can be sites for
magnetic reconnection. The Magnetospheric Multiscale (MMS) mission has recently …

A Hybrid Vlasov–Maxwell (HVM) model is presented and recent results about the link
between kinetic effects and turbulence are reviewed. Using five-dimensional (2D in space …

A statistical relationship between magnetic reconnection, current sheets, and intermittent
turbulence in the solar wind is reported for the first time using in situ measurements from the …

Using 2.5 dimensional kinetic particle-in-cell simulations, we simulate reconnection
conditions appropriate for the magnetosheath and solar wind, ie, plasma beta (ratio of gas …

We report the results of a direct comparison between different kinetic models of collisionless
plasma turbulence in two spatial dimensions. The models considered include a first …

Using high-resolution Cluster satellite observations and a multi-dimensional intermittency
technique, we show that the magnetic discontinuities in the turbulent solar wind are …

We report the properties of a novel type of sub-proton scale magnetic hole found in two
dimensional particle-in-cell simulations of decaying turbulence with a guide field. The …

We perform a high-resolution, 2D, fully kinetic numerical simulation of a turbulent plasma
system with observation-driven conditions, in order to investigate the interplay between …