Identifying Interplanetary Shock Parameters in Heliospheric MHD Simulation Results

Details Identifying Interplanetary Shock Parameters in Heliospheric MHD Simulation Results Identifying Interplanetary Shock Parameters in Heliospheric MHD Simulation Results

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh43a..03l&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SH43A-03

Physics

2114 Energetic Particles, Heliospheric (7514), 2118 Energetic Particles, Solar, 7811 Discontinuities

Scientific paper

One of the challenges of integrating SEP models into heliospheric space weather event simulations is the identification and characterization of the shock in the underlying MHD simulation results. We investigate the numerical method by which the jumps can be identified, the shock surface orientation characterized, and the upstream and downstream conditions defined. Our approach uses snapshots of observer-connected interplanetary magnetic field lines. First we determine whether a shock is on the connected field line, and record its position and the change in the MHD variables (field, density, velocity). We also examine several adjacent field lines and similarly determine the shock positions. The identification of the jumps takes into account the lack of spatial resolution at the shock front. The shock surface orientation is determined by a cross-product method. Then the shock normal angle is determined from the upstream and downstream vector fields and the normal. These calculations are relatively fast and can be embedded in a simulation run for use in overlaid SEP shock source descriptions or for analyzing the evolution of the connected shock parameters with time.

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