Physics
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsm51b1641d&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #SM51B-1641
Physics
2753 Numerical Modeling, 2784 Solar Wind/Magnetosphere Interactions, 7859 Transport Processes
Scientific paper
Multi-fluid MHD modelling is a useful tool in the study of solar wind entry into the magnetosphere. We have shown in an earlier paper that this simulation technique allows solar wind and magnetospheric plasmas to be clearly distinguished, so that the self-consistent entry of the solar wind into the magnetosphere can be traced. Preliminary studies of this process for steady southward IMF were conducted with the multi-fluid version of the Lyon-Fedder-Mobarry global MHD model which currently includes two ion species and a neutralizing massless electron fluid. For this study, the solar wind plasma was specified to be 99.99% ion species A and 0.01% ion species B, with identical mass and temperature of both species at the upstream boundary in the solar wind. The system is then permitted to evolve until a quasi-steady magnetosphere develops. At this point, the fractions of the species are reversed at the upstream simulation boundary and the entry of species B traced. Plasma entry is clearly seen via the cusps, with some indications of entry in the vicinity of the flanks. Here, we examine changes in the dynamics of the previously quasi-steady magnetosphere resulting from entry of the now dominant upstream species B. We also investigate the effect of varying key parameters such as the length of time the system evolves (prior to the reversal of the species fractions) and the fractional concentrations of each species in the solar wind. The global characteristics of these results are contrasted with the evolution of the single-fluid MHD system. Additionally, results from a similar analysis of a steady northward IMF configuration are reported.
Damiano Peter A.
Lotko William
Lyon John G.
Wiltberger Michael J.
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