This session is intended as a discussion forum on our recent understanding of particle acceleration mechanisms in solar system plasmas from both experimental and theoretical view points, with special emphasis on current and future synergies between in situ and remote observations and models/simulations supporting them. Synergism is crucial to establish how fundamental acceleration mechanisms operate in different solar system plasma environments (e.g. solar corona/wind, planetary magnetospheres) and to what extent the knowledge obtained from those can be realistically exported to distant astrophysical environments (e.g. stellar coronae, supernovae and astrophysical jets), where similar acceleration mechanisms are thought to operate. Such collaborative approach is strongly motivated by major observational advances, obtained with new generation of spacecraft like Cluster, Themis, Rhessi, Hinode, Stereo, SDO, etc, and future missions such as Solar Orbiter and Solar Probe Plus that will allow the first simultaneous in situ and remote observations in the solar corona/wind. The ultimate goal is to establish a network of scientists from different fields aiming to study particle acceleration from a comparative point of view. We solicit contributions on a wide range of acceleration mechanisms such as those operating in reconnection regions during solar flares and planetary substorms, in slow/fast solar wind and co-rotating interaction regions, at interplanetary and planetary shocks/foreshocks, in radiation belts and in auroral regions. We are also addressing the role of magnetic topology for the acceleration, e.g. parallel and perpendicular shock geometries, formation of resonant magnetic field lines and expanding flux ropes and generation of boundaries between fast reconnection jets and ambient magnetic field/plasma.