Magnetopause encounters in the magnetotail at distances of approximately 80 R(sub e)

Details Magnetopause encounters in the magnetotail at distances of approximately 80 R(sub e) Magnetopause encounters in the magnetotail at distances of approximately 80 R(sub e)

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994georl..21.3007w&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 21, no. 25, p. 3007-3010

Physics

10

Flow Velocity, Geomagnetic Tail, Ion Emission, Magnetohydrodynamic Flow, Magnetopause, Magnetosheath, Satellite Observation, Solar Wind, Space Plasmas, Anisotropy, Geophysical Satellites, Magnetic Signatures, Mass Distribution, Particle Acceleration, Particle Mass, Plasma Density, Velocity Distribution

Scientific paper

The GEOTAIL satellite experienced several encounters with the magnetopause during the interval 0300 to 0600 hours on 27 October 1992 at a gsm location of (X,Y,Z) approximately (-81, -8, 7.5) R(sub e). Energetic ions of both solar wind and ionospheric origin (H(+), He(++), and O(+)) were observed streaming in the anti-solar direction on both the lobe and magnetosheath side of the plasma mantle-magnetosheath boundary, with maximum fluxes occuring at the boundary. Even though the mantle plasma had penetrated well into the lobe through convective drift, the energetic ions were observed only at the magnetopause and provided a clear signature of the boundary region. Using a measured convective drift velocity and observed ergetic particle anisotropies, we estimated that the maximum distance from GEOTAIL that the energetic ions could have been accelerated or made contact with the boundary field lines was less than 8 - 39 R(sub e), implying that both solar wind and ionospheric ions are accelerated and contact the magnetopause many tens of earth radii behind the earth. We further found that the unusual magnetopause positions encountered at this time could be explained in part by solar wind aberration effects. However additional processes (e. g., magnetospheric breathing modes, convoluted tail topologies) are required to fully explain these observations.

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