Observations of protons with energies exceeding 100 keV in the earth's magnetosheath

Details Observations of protons with energies exceeding 100 keV in the earth's magnetosheath Observations of protons with energies exceeding 100 keV in the earth's magnetosheath

Feb 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976jgr....81..569w&link_type=abstract

Journal of Geophysical Research, vol. 81, Feb. 1, 1976, p. 569-584. ERDA-sponsored research.

Physics

10

Magnetosheath, Magnetospheric Proton Density, Proton Energy, Solar Activity Effects, Bow Waves, Geomagnetism, Lines Of Force, Ogo-5, Proton Flux Density, Satellite Observation, Shock Waves

Scientific paper

A comprehensive study of energetic protons (100 to 1300 keV) in the magnetosheath is presented, based on OGO 5 observations of bursts of such protons in the sheath and in the upstream wave region beyond the earth's bow shock during periods of generally enhanced solar and geomagnetic activity in 1968. A summary of the described observations shows that: (1) the major bursts tend to appear near the magnetopause in the afternoon magnetosheath, (2) the proton bursts often correlate with depressions in the sheath magnetic field and usually correlate with enhanced magnetic-field turbulence, (3) the directional distributions generally coincide with the plasma flow direction, (4) the flux intensities show a fairly good correlation with Kp index, (5) the peak unidirectional spectra and fluxes in the sheath near the magnetopause are often quite similar to those in the nearby magnetosphere, (6) the main fluxes of upstream protons usually come from the solar-wind direction, and (7) magnetopause boundary-layer effects are often associated with the fluxes. It is shown that many features of the directional distributions can be explained through a combination of the Compton-Getting effect, proton-flux spatial gradients, and free streaming of protons along field lines away from the source region. Possible sources of the sheath protons considered include escape from the magnetosphere, acceleration in the magnetosheath, acceleration in the bow shock, and acceleration in the upstream wave region with leakage into the magnetosheath.

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