Mathematics – Probability
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsm12b..05e&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #SM12B-05
Mathematics
Probability
2740 Magnetospheric Configuration And Dynamics, 2744 Magnetotail, 2753 Numerical Modeling, 2764 Plasma Sheet
Scientific paper
In this study we use our global magnetohydrodynamic (MHD) simulation code driven by an idealized time series of solar wind parameters to investigate the global aspects of turbulence in the plasma sheet. As a first step we will consider the effects of turbulence during southward Interplanetary Magnetic Field (IMF) conditions. During southward IMF, localized and large scale reconnection drives flows and vorticity in the tail at different scales. We impose a steady southward IMF at the upstream simulation boundary. This eliminates the solar wind as a source of turbulence in the model and to investigate the relationship between reconnection-driven convection, waves on the magnetopause boundary and turbulence in the magnetotail. For this study we used an enhanced resolution code with a minimum grid spacing of the order of 0.12 RE. We also saved the results every second at an array of points near the equatorial plane to obtain high resolution time series of the simulation results and to calculate power spectra. The simulation shows that there is considerable wave activity along the magnetopause in addition to the vorticity in the plasma sheet. We will quantify the turbulence in the plasma sheet by calculating the power spectral density and probability distributions.
Ashour-Abdalla Maha
El-Alaoui Mostafa
Goldstein Michel L.
Richard Robert L.
Walker Ray J.
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