Interplanetary Magnetic Field Connection to the L1 Lagrangian Orbit During Upstream Energetic Ion Events

Details Interplanetary Magnetic Field Connection to the L1 Lagrangian Orbit During Upstream Energetic Ion Events Interplanetary Magnetic Field Connection to the L1 Lagrangian Orbit During Upstream Energetic Ion Events

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh51b..06r&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH51B-06

Physics

2114 Energetic Particles, Heliospheric (7514), 2134 Interplanetary Magnetic Fields, 2154 Planetary Bow Shocks, 7807 Charged Particle Motion And Acceleration

Scientific paper

Energetic ions moving upstream from the Earth's bow shock frequently appear at the sunward Lagrangian (L1) point. The most common orientation of the interplanetary magnetic field (IMF) during these upstream events is near-radial from the sun (the nominal direction for connection to the magnetosphere). However, strong unidirectional beams of ions streaming away from Earth, consistent with good magnetic connection to the bow shock, are observed even when the IMF is transverse to the radial direction. We present observations of upstream events from as many as four upstream spacecraft. Included in this presentation are energetic ion and magnetic field measurements from: (1) ACE/EPAM, ACE/MAG; (2) WIND/3DP, WIND/MFI; (3) IMP8/EPE, IMP8/MAG; (4) GEOTAIL/EPIC, and GEOTAIL/MAG. In addition, the ACE/SWEPAM instrument identifies IMF connection between the L1 point and the Earth's bow shock by the presence of low-energy (272-372 eV) bi-directional electron flux. Instruments on the IMP8 and GEOTAIL spacecraft simultaneously measure the energetic ion intensity and IMF configuration close to the Earth's bow shock during times of particle enhancements observed at L1. Analysis of ACE, WIND, IMP8, and GEOTAIL observations show that >40% of upstream events are observed during times of non-radial IMF orientation. Observations from ACE/EPAM of over 500 upstream energetic ion events confirm this result. We find similar distributions of radial and non-radial IMF orientations both close to the bow shock and at L1. This implies that the IMF configurations during upstream events are large-scale spatial structures with radii of curvature on the order of the Earth-L1 distance, i.e. 0.01 AU. These spatial structures are being convected through the L1 point into the Earth's foreshock.

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