Investigation of Shabansky Orbit Accessibility by Using 3D Particle Tracing in the Global MHD Simulations

Details Investigation of Shabansky Orbit Accessibility by Using 3D Particle Tracing in the Global MHD Simulations Investigation of Shabansky Orbit Accessibility by Using 3D Particle Tracing in the Global MHD Simulations

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsm22a0230s&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SM22A-0230

Physics

2720 Energetic Particles, Trapped, 2730 Magnetosphere: Inner, 2753 Numerical Modeling, 2784 Solar Wind/Magnetosphere Interactions

Scientific paper

Due to the existence of the magnetic field strength minimum in the outer cusp region, energetic particles (a few hundred keV protons and MeV electrons) approaching the dayside magnetic field lines with a minimum field off-equator will experience large scale transport toward high latitude, being trapped at high latitude, and then being scattered back through Shabansky orbit [Shabansky, 1971]. The particle trajectories inside the magnetosphere can be grouped into three classes: (a) bouncing around the Equator (trapped); (b) going through Shabansky Orbit or being elevated at dayside (pseudo-trapped); (c) lost. Characterizing these three regions of particles and understanding their dependence on the solar wind condition can help understand the energization and loss of energetic particles in the radiation belt. Recently, we developed a 3D particle tracing code to simulate particle transport in transient global MHD (LFM model) simulation output. The protons are traced with full-motion and electrons are traced with guiding-center approximation. By launching energetic electrons and protons with different pitch angle and from various location along the tail in the model magnetosphere, recording and averaging the latitude the particle experiences at the dayside, we derive the Shabansky Orbit Accessibility Map (SOAMap) to visualize the three regions (trapped, pseudo-trapped, and lost) and their dependence on the initial launching position and pitch angle. We derived the SOAMaps for both electrons and protons inside steady state magnetosphere under different solar wind conditions. We also studied the evolution of the SOAMaps during a simulated magnetospheric substorm triggered by the turning of the solar wind IMF from northward to southward. Combining 3D particle tracing and global MHD simulation provides an integrated view of 3D energetic particle transport inside the Earth's magnetosphere. Shabansky, V. P., Some processes in the magnetosphere, Space Sci. Rev., 12, 299, 1971.

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