An overview of energetic particles (from 55 keV to > 30 MeV) recorded in the close Martian environment, and their energization in local and external processes

Abstract

Observations made by the SLED particle detector on Phobos-2 in the close Martian environment from 29 January to 27 March, 1989 during the early rising phase of Solar Cycle 22, show the frequent presence close to the planet, under reasonably “quiet” interplanetary conditions, of particles with energies ( E) in the range from several tens of, to several hundred, keV. Under disturbed interplanetary circumstances, particles reaching energies of several tens of MeV were recorded close to Mars. Those particles in the keV range were observed at well-defined locations, i.e. at the Terminator Shocks ( E up to ≈600 keV); just inside the subsolar Planetopause ( E up to ≈225 keV), and travelling down the Tail, E≥55 keV. These three populations are herein suggested, instancing various candidate mechanisms, to have been energized by processes local to the planet. Since the seed particles for ions accelerated at the Terminator Shocks may comprise ambient, pre-accelerated, solar particles, the energies of ions detected by SLED during Bow Shock transits was observed (during two months) to vary between ≈50 keV and ≈600 keV. Particles with energies up to several tens of MeV which were found to suffuse the close planetary environment over extended periods, are interpreted to have been produced in association with solar processes external to Mars (Co-rotating Interaction Regions; Gradual and Impulsive Solar Events). Particle enhancements in the keV range recorded by SLED (under favourable magnetic conditions) during Bow Shock traversals, provide topographical information concerning the location of the Martian subsolar and distant shock surfaces. These observations constitute a new data set, complementary to those determinations of key boundaries derived from plasma and magnetic field measurements made aboard various American and Russian spacecraft at Mars which, for more than thirty years now, have been generally used in modelling the Solar Wind interaction with the planet. Three-dimensional measurements made at low altitudes over long dwell times are presently required to provide further insights into those local processes whereby populations of keV particles discovered in SLED data, close to the inbound Planetopause and travelling down the Tail, are individually energized.