HR: 16:25h
AN: SH22C-02    [PDF]
TI: Energetic Particles Upstream From the Earth's Bow Shock: Multipoint Observations by Cluster and Polar
AU: * Roeder, J L
EM: james.roeder@aero.org
AF: The Aerospace Corporation, P O Box 92957, Los Angeles, CA 90009 United States
AU: Fennell, J F
AF: The Aerospace Corporation, P O Box 92957, Los Angeles, CA 90009 United States
AU: Blake, J B
AF: The Aerospace Corporation, P O Box 92957, Los Angeles, CA 90009 United States
AU: Daly, P W
AF: Max Planck Institute for Aeronomy, Max-Planck-Str. 2, Lindau-Katlenburg, 37191 Germany
AU: Grande, M
AF: Rutherford Appleton Laboratory, Chilton, Didcot, OX11 0QX United Kingdom
AU: Perry, C
AF: Rutherford Appleton Laboratory, Chilton, Didcot, OX11 0QX United Kingdom
AU: Carter, M
AF: Rutherford Appleton Laboratory, Chilton, Didcot, OX11 0QX United Kingdom
AB: One of the primary goals of the Cluster mission is to use multipoint observations to separate temporal and spatial variations in the measured fields and particle fluxes. An example is found in observations by the Cluster RAPID instruments of 30-1500 keV particle populations upstream of the Earth's bow shock. When the Cluster constellation is closely spaced ($\sim$600 km), the energetic particle fluxes observed by the four spacecraft are nearly identical because the locations differ by less than one gyroradius of the lowest energy particles. The measured magnetic field vectors at the four spacecraft are also virtually identical, and connect to a single region on the bow shock surface. We contrast this with recent cases in which the Cluster separation is much greater ($\sim$6000 km) and the magnetic field connects the four spacecraft to different points on the shock. In this way, the particle acceleration processes at several points on the shock may be monitored simultaneously. Similar energetic particle measurements in the dayside outer magnetosphere by the Polar spacecraft are compared with the Cluster observations with a special focus on the differences in relative ion composition between the upstream populations and the magnetospheric particles.
DE: 2154 Planetary bow shocks
DE: 2720 Energetic particles, trapped
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting