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 …

The solar wind (SW) and local interstellar medium (LISM) are turbulent media. Their
interaction is governed by complex physical processes and creates heliospheric regions …

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; …

The Wind spacecraft, launched on November 1, 1994, is a critical element in NASA's
Heliophysics System Observatory (HSO)—a fleet of spacecraft created to understand the …

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 …

The zeroth law of turbulence states that, for fixed energy input into large-scale motions, the
statistical steady state of a turbulent system is independent of microphysical dissipation …

Comparative studies of fast and slow solar wind streams performed over the past decades
have illustrated several differences between the plasma regimes for these different flows …

HelioSwarm (HS) is a NASA Medium-Class Explorer mission of the Heliophysics Division
designed to explore the dynamic three-dimensional mechanisms controlling the physics of …

Alfvénic fluctuations are very common features in the solar wind and are found especially
within the main portion of fast-wind streams while the slow wind usually is less Alfvénic and …

We revisit the theory of stochastic heating of ions and investigate its phase-space signatures
in kinetic turbulence of relevance to low-β portions of the solar wind. In particular, we retain a …