Physics
Scientific paper
Dec 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsm43c1240w&link_type=abstract
American Geophysical Union, Fall Meeting 2005, abstract #SM43C-1240
Physics
2154 Planetary Bow Shocks, 2706 Cusp, 2716 Energetic Particles: Precipitating, 2753 Numerical Modeling, 2784 Solar Wind/Magnetosphere Interactions
Scientific paper
It has been suggested by satellite observations that energetic (101 - 102 KeV) ions in the magnetospheric cusp are originated from the quasi-parallel bow shock. In this study, a 3-D global-scale hybrid simulation is carried out to investigate the ion signature and ion energization in the cusp regions of the magnetosphere. The simulation is shown for cases in which the IMF geometry leads to the inter-connection between the field lines in the northern cusp and those in the quasi-parallel bow shock through a high-latitude reconnection. The IMF and solar wind conditions are kept constant in each case. First, ion velocity distributions are examined for the foreshock region. Accelerated, backstreaming ions are found in the foreshock of the quasi-parallel shock. The foreshock ions possess a diffuse ion distribution with a non-thermal spectral break at energy ~ 15-30KeV for cases with Mach number M_A =5-9, and the differential ion flux evolves with the field-aligned distance to the bow shock by an e-folding distance of 3-9 RE at various energy channels, consistent the satellite observation. Second, the coupling between the particle signatures in the foreshock and the cusp is investigated. The energetic ions (up to ~ 102 KeV) are also present downstream of the shock, through the magnetosheath to the cusp vicinity, with a spectral break similar to that in the foreshock. The distributions in the cusp boundary show the presence of two ion populations: a population of the local cusp proper and an ion beam from the magnetosheath. Our simulation indicates a strong coupling between the energetic ions at the quasi-parallel shock and the cusp energetic ions. Third, Alfvén waves are found to be generated in the magnetosphere due to the foreshock pressure pulses, and due to magnetic reconnection at the magnetopause. The influence of the waves on the cusp magnetosphere is discussed. The results will also be compared with the cases in which the IMF is also northward but the bow shock is dominated by a quasi-perpendicular shock.
Chang Sandy
Lin Yangtin
Wang Xinhua
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