Energies of backstreaming protons in the foreshock

Details Energies of backstreaming protons in the foreshock Energies of backstreaming protons in the foreshock

Sep 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976georl...3..553g&link_type=abstract

Geophysical Research Letters, vol. 3, Sept. 1976, p. 553-556. Research supported by the TRW Independent Research and Development

Physics

Bow Waves, Cislunar Space, Magnetospheric Proton Density, Proton Belts, Shock Waves, Solar Wind, Atmospheric Boundary Layer, Energy Distribution, Particle Interactions, Particle Motion, Particle Production, Satellite Observation, Upstream, Wave Interaction

Scientific paper

At least some part of the cislunar solar wind region outside the earth's bow shock is continuously populated by particles and waves of shock or magnetospheric origin. The varying precursor region, or foreshock, is divided into several subregions, not all geometrically distinct, which are defined by differing particle species and wavemodes. A first-order examination is presented of the way in which the geometry of the foreshock wave boundary of Diodato et al. (1976) can be translated into a geometry of return proton energies. A predicted pattern of energy versus detector location in the cislunar region is displayed for proton guiding-centers traveling upstream away from the quasi-parallel bow shock. Only the simplest case of gyrationless particles is considered. Important contributors to the spread in energies to be expected of ions coming from each segment are discussed. The actual pattern of return particles will be somewhat different from the idealized one discussed, because foreshock boundary-protons will be neither unidirectional nor monoenergetic.

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