This splinter meeting is to allow more discussions on one aspect of the session ST1.4. The emphasis is on energetic particles arising in the slow and fast solar wind, co-rotating interactions regions, interplanetary or planetary shocks and foreshock regions, and from magnetic reconnection events such as solar flares. Remote or in-situ observations of the particle populations in the solar system are continuously ongoing owing to several dedicated spacecraft missions (from new generations of spacecraft like STEREO and THEMIS and earlier ones like ACE, SOHO, WIND, Cluster, RHESSI, etc.). Their measurements, the associated data analysis, as well as theoretical considerations provide crucial information for understanding the sources of the particle populations, their acceleration and propagation/transport processes. Magnetic topology plays an important role through parallel and perpendicular shock geometries, the trapping of the energetic particles and re-acceleration from long-lived acceleration sites. This session invites contributions on a wide range of theoretical, modeling and observational topics. The signatures of the various forms of plasma interactions, the effects of dynamically evolving magnetic field configurations such as resonant magnetic field lines or expanding flux ropes, or using the particles to probe the magnetic topology of the structures they originate from are highly relevant.