Energetic particles (greater than 34 KeV - 3.2 MeV) in the deep Martian magnetotail (X = 15.5 RM), modeling of the Martian bow shock and the influence of low solar wind pressure on Mars as an obstacle

Details Energetic particles (greater than 34 KeV - 3.2 MeV) in the deep Martian magnetotail (X = 15.5 RM), modeling of the Martian bow shock and the influence of low solar wind pressure on Mars as an obstacle Energetic particles (greater than 34 KeV - 3.2 MeV) in the deep Martian magnetotail (X = 15.5 RM), modeling of the Martian bow shock and the influence of low solar wind pressure on Mars as an obstacle

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992esasp.346..107m&link_type=abstract

In ESA, Study of the Solar-Terrestrial System p 107-111 (SEE N93-31674 12-90)

Physics

Bow Waves, Energetic Particles, Magnetosheath, Mars (Planet), Planetary Magnetotails, Solar Wind, Wind Pressure, Boundary Layer Transition, Planetary Boundary Layer, Satellite Observation, Shock Waves

Scientific paper

The first observations of energetic particles (range greater than 34 KeV to less than 3.2 MeV) in the tailward part of the Martian magnetosheath, as well as during crossings of the Martian bow shock within the deep magnetotail (X = 15.5 RM), are reported. This was done by using data from the SLED (Solar Low Energy Detector) instrument on Phobos 2. The energies observed cannot be attained by the pickup process acting alone. Sporadic field line merging at the dayside of the planet would conceivably accelerate the particles to the observed energies. The presence of an unusually weak dynamic solar wind pressure during orbits 3 and 4 suggests that a weak intrinsic field could have expanded outwards under these conditions to provide a dayside obstacle radius for Mars of up to about 2000 km.

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