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Tracing of high‐latitude magnetic field lines by solar particles
Author(s) -
Paulikas G. A.
Publication year - 1974
Publication title -
reviews of geophysics
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 8.087
H-Index - 156
eISSN - 1944-9208
pISSN - 8755-1209
DOI - 10.1029/rg012i001p00117
Subject(s) - physics , magnetosphere , earth's magnetic field , interplanetary magnetic field , solar energetic particles , ionospheric dynamo region , field line , plasma sheet , interplanetary spaceflight , electron precipitation , geophysics , energetic neutral atom , polar , latitude , interplanetary medium , ring current , solar wind , geomagnetic storm , coronal mass ejection , astronomy , electron , magnetic field , nuclear physics , quantum mechanics
Recent measurements of solar particles in the energy interval between hundreds of keV and a few MeV have shown that a direct connection exists between a portion of the high‐latitude geomagnetic field and the interplanetary magnetic field. The access window for 300‐keV solar protons that reach the center of the polar cap may be as near as 150 R E in the downstream magnetotail. Solar protons that precipitate into the atmosphere at latitudes near the geomagnetic cutoff enter through the flanks of the magnetosphere and the nearby neutral sheet, possibly within 30 R E of the earth. Comparison of the patterns of auroral particle precipitation with the zones of access of energetic solar electrons and protons indicates that a substantial fraction of the aurora originates on field lines connected to the interplanetary field.