ULF waves in the low-latitude boundary layer and their relationship to magnetospheric pulsations: A multisatellite observation

Details ULF waves in the low-latitude boundary layer and their relationship to magnetospheric pulsations: A multisatellite observation ULF waves in the low-latitude boundary layer and their relationship to magnetospheric pulsations: A multisatellite observation

Jan 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994uwll.rept.....t&link_type=abstract

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Mathematics

Logic

Earth Magnetosphere, Extremely Low Frequencies, Geomagnetic Pulsations, Magnetospheric Instability, Planetary Boundary Layer, Plasma Waves, Tropical Regions, Wave Generation, Ampte (Satellites), Electron Beams, Geomagnetism, Goes 5, Goes 6, Kelvin-Helmholtz Instability, Satellite Observation, Scatha Satellite, Solar Wind, Transverse Oscillation

Scientific paper

On April 30 (day 120), 1985, the magnetosphere was compressed at 0923 UT and the subsolar magnetopause remained near 7 R(sub E) geocentric for approximately 2 hours, during which the four spacecraft, Spacecraft Charging At High Altitude (SCATHA), GOES 5, GOES 6, and Active Magnetospheric Particle Tracer Explorers (AMPTE) CCE, were all in the magnetosphere on the morning side. SCATHA was in the low-latitude boundary layer (LLBL) in the second half of this period. The interplanetary magnetic field was inferred to be northward from the characteristics of precipitating particle fluxes as observed by the low-altitude satellite Defense Meteorological Satellite Program (DMSP) F7 and also from absence of substorms. We used magnetic field and particle data from this unique interval to study ULF waves in the LLBL and their relationship to magnetic pulsations in the magnetosphere. The LLBL was identified from the properties of particles, including bidirectional field-aligned electron beams at approximately 200 eV. In the boundary layer the magnetic field exhibited both a 5-10 minute irregular compressional oscillation and a broadband (Delta(f)/f approximately 1) primarily transverse oscillations with a mean period of approximately 50 s and a left-hand sense of polarization about the mean field. The former can be observed by other satellites and is likely due to pressure variations in the solar wind, while the latter is likely due to a Kelvin-Helmoltz (K.-H.) instability occurring in the LLBL or on the magnetopause.

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