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 …

How turbulent energy is dissipated in weakly collisional space and astrophysical plasmas is
a major open question. Here, we present the application of a field-particle correlation …

This review of scaling theories of magnetohydrodynamic (MHD) turbulence aims to put the
developments of the last few years in the context of the canonical time line (from Kolmogorov …

The current understanding of magnetohydrodynamic (MHD) turbulence envisions turbulent
eddies which are anisotropic in all three directions. In the plane perpendicular to the local …

Magnetohydrodynamic Turbulence Mediated by Reconnection - IOPscience This site uses
cookies. By continuing to use this site you agree to our use of cookies. To find out more, see …

The presence of magnetic fields in many astrophysical objects is due to dynamo action,
whereby a part of the kinetic energy is converted into magnetic energy. A turbulent dynamo …

We present analysis of 17,043 proton kinetic-scale current sheets (CSs) collected over 124
days of Wind spacecraft measurements in the solar wind at 11 samples s− 1 magnetic field …

Many high-energy astrophysical systems contain magnetized collisionless plasmas with
relativistic particles, in which turbulence can be driven by an arbitrary mixture of solenoidal …

We present statistical analysis of 11,200 proton kinetic-scale current sheets (CS) observed
by the Parker Solar Probe during 10 days around the first perihelion. The CS thickness λ is …

Relativistic magnetically dominated turbulence is an efficient engine for particle acceleration
in a collisionless plasma. Ultrarelativistic particles accelerated by interactions with turbulent …