Simulations of Solar-Wind Ion Motion in the Magnetosheath and Magnetosphere

Details Simulations of Solar-Wind Ion Motion in the Magnetosheath and Magnetosphere Simulations of Solar-Wind Ion Motion in the Magnetosheath and Magnetosphere

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsm31e..01c&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SM31E-01

Physics

2728 Magnetosheath, 2753 Numerical Modeling, 2784 Solar Wind/Magnetosphere Interactions

Scientific paper

In this work we investigate the transport of representative solar-wind ions through the Earth's magnetosheath and magnetosphere by tracing their full trajectories. For the magnetosheath we use an analytical model, based on the draping of plasma streamlines and magnetic field lines around a conducting magnetopause that consists of half a prolate ellipsoid, extending ~11 RE upstream and ~65 RE downstream from Earth, matched there to a cylinder of radius ~28.4 RE. For a uniform but arbitrarily directed interplanetary magnetic field (IMF), the magnetosheath's magnetic field can be obtained by superposition of results for special cases in which the IMF is respectively parallel to and perpendicular to the solar-wind velocity. For the case in which the IMF is parallel to the solar-wind velocity, the magnetosheath's magnetic field is derivable from Euler potentials that can be expressed analytically as functions of ellipsoidal or cylindrical coordinates that scale inversely with the sixth root of solar- wind pressure. When the IMF is perpendicular to the solar-wind velocity, we can calculate the magnetosheath flow velocity from Bernoulli's equation and compute the time delay for the magnetosheath plasma to have traveled to any point of interest from the bow shock. Points along a magnetosheath field line are points of equal time delay from an upstream field line. For the magnetosphere we use a snapshot of the Rice Convection Equilibrium Model (RCM-E), which includes a magnetic field in force balance with the plasma. The RCM-E includes a self- consistent electrostatic field in the closed field line region and the Weimer model in the open field line region. Using the particle trajectories, we compute simulated ion density and temperature at various locations within the magnetosheath and magnetosphere for simple IMF configurations.

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