Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979aipc...56..179k&link_type=abstract
In: Particle acceleration mechanisms in astrophysics; Proceedings of the Workshop, La Jolla, Calif., January 3-5, 1979. (A80-532
Astronomy and Astrophysics
Astrophysics
3
Electron Energy, Geomagnetic Tail, Particle Acceleration, Proton Energy, Angular Distribution, Anisotropy, Direct Current, Electric Fields, Energetic Particles, Magnetosheath, Mathematical Models, Periodic Variations, Plasma Acceleration, Solar Wind
Scientific paper
During geomagnetic activity large numbers of particles are accelerated to energies ranging from a few keV to more than 1 MeV and propagate within the magnetotail, magnetosheath, and upstream solar wind. Time scales of acceleration range from less than 10 sec to several minutes, and intensities of 0.3 MeV protons up to 10 to the 5th per sq cm-sec-sr-MeV have been observed. In a special class of intense proton bursts inverse velocity dispersion is observed. Close association is seen between dc electric field pulses on high latitude field lines at a few earth radii, and impulsively accelerated particles. In many cases counterstreaming between energetic particles and plasma is observed. Simultaneous observations with two or more spacecraft show development of anisotropies consistent with multiple sources within the magnetotail. It is suggested that the data are not consistent with models postulating a single X-type neutral line across the magnetotail. These observations place most stringent constraints on magnetotail particle acceleration mechanisms.
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