Simulation of Solar-Wind Ion Entry into the Magnetosphere with the Plasma Transport Numerical Magnetosphere Model (PlATNUMM)

Details Simulation of Solar-Wind Ion Entry into the Magnetosphere with the Plasma Transport Numerical Magnetosphere Model (PlATNUMM) Simulation of Solar-Wind Ion Entry into the Magnetosphere with the Plasma Transport Numerical Magnetosphere Model (PlATNUMM)

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsm23d..02l&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SM23D-02

Statistics

Computation

2728 Magnetosheath, 2753 Numerical Modeling, 2760 Plasma Convection (2463), 2764 Plasma Sheet, 7807 Charged Particle Motion And Acceleration

Scientific paper

We present a new global simulation model of plasma transport from the solar wind through the magnetosheath and into the magnetosphere that will be used to investigate the entry and transport of particles in the magnetosphere. On interplanetary magnetic field (IMF) lines and on open magnetospheric magnetic field lines, the model computes the full particle drift of ions and electrons using a Lorentz force solver. The particle tracing model will be coupled with the Rice Convection Model in order to compute the bounce-averaged gradient/curvature drift transport in the closed field line region of the inner and middle magnetosphere. The 3D magnetic field model includes an analytic magnetosheath magnetic field combined with a Tsyganenko magnetospheric magnetic field, while the electric field model is specified on a 3D grid by tracing magnetic field lines to the ionosphere or the unshocked solar wind where the electric field is known. The Lorentz force solver uses an adaptive Runge-Kutta time-stepper that calculates the drift path of large numbers of particles in parallel. The equivalent phase space density of particles is computed along the RCM outer boundary in order to provide the plasma boundary condition for the RCM. The magnetic and electric fields inside the magnetosphere are computed to evolve self-consistently with the plasma distribution given by the RCM and the particle tracing code. Specifying simple configurations of the IMF, we demonstrate the computation of drift path trajectories for a large number of particles launched upstream of the bow shock.

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