Dynamics of low-energy electrons /greater than or equal to 17 keV/ and ions /greater than or equal to 80 keV/ in the vicinity of the low-latitude, duskside magnetopause - Helios 1 and 2 observations

Details Dynamics of low-energy electrons /greater than or equal to 17 keV/ and ions /greater than or equal to 80 keV/ in the vicinity of the low-latitude, duskside magnetopause - Helios 1 and 2 observations Dynamics of low-energy electrons /greater than or equal to 17 keV/ and ions /greater than or equal to 80 keV/ in the vicinity of the low-latitude, duskside magnetopause - Helios 1 and 2 observations

Apr 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979jgr....84.1453r&link_type=abstract

Journal of Geophysical Research, vol. 84, Apr. 1, 1979, p. 1453-1463. Bundesministerium für Forschung und Technologie

Physics

1

Energetic Particles, Energy Spectra, Geomagnetic Latitude, Magnetopause, Magnetospheric Electron Density, Magnetospheric Ion Density, Particle Motion, Electron Distribution, Electron Energy, Geomagnetic Tail, Helios 1, Helios 2, Ion Temperature, Magnetosheath, Solar Radio Bursts

Scientific paper

The Helios 1 and 2 magnetic field and energetic particle observations of the magnetopause layer reported earlier (Keppler et al., 1978) are discussed in some detail. These observations were made shortly after launch and while the two heliocentric space probes were traveling toward the sun. Helios 1 and 2 left the earth's magnetosphere through the duskside, at nearly zero latitude and in the dusk-noon quadrant. The Helios measurements extended to much lower energies (greater than 17 keV for electrons and 80 keV for ions) together with much higher time, directional and energy resolutions than similar observations performed earlier. The observations are briefly described, while the energy spectra and the associated energy flows are examined. Attention is given to the fine-scale structure directly at and adjacent to the magnetopause, to an analysis of the bursts of energetic particles observed directly inside the magnetopause and in the magnetosheath region close to the magnetopause, and to an examination of implications of the Helios 1 and 2 observations for magnetospheric models.

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