Solar wind, foreshock, bow shock, and magnetosheath transient phenomena and their effects
Transient solar wind phenomena and processes in the foreshock, at the bow shock, and in the magnetosheath are all drivers of significant downstream effects at the magnetopause, inside the magnetosphere, in the ionosphere, and on ground. These phenomena encompass, but are not restricted to, interplanetary magnetic field discontinuities and related hot flow anomalies or foreshock bubbles, foreshock cavities, cavitons and related spontaneous hot flow anomalies, as well as SLAMS and magnetosheath jets. The local effects of these phenomena may include severe changes in local plasma parameters, e.g., heating, compression or expansion, and deflection of plasma. Further downstream, they may be associated with significant magnetopause dynamics including magnetic reconnection, inner-magnetospheric waves and changes in the radiation belt electron populations, geomagnetic variations, ionospheric flow enhancements, particle precipitation, and auroral forms.
We invite contributions focusing on these upstream phenomena, their (downstream) effects, and the coupling between them, i.e., the transport of mass, momentum, and energy, across and between the bow shock and magnetopause boundaries, not only at Earth but also at other planets and solar system bodies. We encourage the presentation of latest results based on in-situ measurements (including the Geotail, Cluster, THEMIS/ARTEMIS, MMS, and Van Allen Probes), on ground-based observations (e.g., magnetometers, radars, riometers, and all-sky imagers), as well as on numerical simulations and theoretical modelling. Presentations of studies using any combination of the above approaches are particularly welcome.