Throughout the solar system and beyond, the ambient space plasma populations tend to have insufficient energy to excite the intense emissions observed at their magnetic footpoints, be that in the
solar, or planetary environments or indeed astrophysical jets.
Particle acceleration can occur at locations along a magnetic field line where the necessary conditions for different processes are satisfied. These can include, but are not limited to, quasi-static
acceleration by field-aligned potential drops, acceleration by short perpendicular-scale Alfvén waves and magnetic reconnection driven processes. In all cases, electromagnetic energy is converted into particle kinetic energy. This energy is eventually converted
back into electromagnetic energy through emissions across the electromagnetic spectrum, from gamma rays through visible emissions to radio waves.
At this meeting, we will explore field-aligned plasma acceleration processes in a variety of different environments in order to fully examine the conditions under which this acceleration occurs and
attempt to link the microphysics of the acceleration processes with larger-scale events, such as substorms, solar flares, and astrophysical jets with which they are often associated. This meeting will bring together magnetospheric, solar, laboratory plasma,
astrophysics and modelling communities to compare and contrast these plasma acceleration processes in a variety of space plasma environments.
