Simultaneous Polar and Cluster Observations of the High-Latitude Dayside Boundary Layer and Cusp During a Period of Enhanced Solar Wind Pressure

Details Simultaneous Polar and Cluster Observations of the High-Latitude Dayside Boundary Layer and Cusp During a Period of Enhanced Solar Wind Pressure Simultaneous Polar and Cluster Observations of the High-Latitude Dayside Boundary Layer and Cusp During a Period of Enhanced Solar Wind Pressure

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsm31a..04c&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SM31A-04

Other

2724 Magnetopause, Cusp, And Boundary Layers, 2740 Magnetospheric Configuration And Dynamics, 2784 Solar Wind/Magnetosphere Interactions

Scientific paper

indent 12pt On April 21, 2001, a sharp increase in both the density and velocity of the solar wind was recorded by the ACE spacecraft at approximately 15:00 U.T. This high density and enhanced velocity encountered the magnetosphere at 16:00 U.T. and persisted until 02:00 U.T. on April 22, 2001. Coupled with the velocity increase (Δ v ≈ 50 km/s), the density increase (Δ n ≈ 30 /cm3) created a large increase in the solar wind pressure that compressed the magnetopause boundary to within 8 Re. During this time period, both the Cluster and Polar spacecrafts were in close proximity of each other in the dayside high-latitude region of the magnetosphere. Cluster entered the northern cusp region from the night side and recorded an increase in the flux of energetic electrons and ions until it appeared to cross the compressed magnetopause boundary and enter the magnetosheath. During the compression, Polar was near apogee on the noon side, moving toward the night side where the MICS instrument recorded an increase in the flux of solar wind particles, He++ and O>+2, while recording an absence of particles of magnetospheric origin, He+ and O<+2. Having Cluster enter the cusp region while traveling outbound while Polar is at apogee near the magnetopause boundary on the noon side created a unique situation for understanding the size and dynamics of the cusp region as well as the positions of magnetospheric boundaries during a period of high solar wind pressure. These observations are compared to the prediction of the position of the magnetopause using a model by S. Petrinic (personal communication) and that of Tsyganenko 1996. Acknowledgement is given to both the Polar/CAMMICE and Cluster/Rapid teams.

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