Thoughts on New Three Dimensional Asymmetric Model of the Magnetopause

Details Thoughts on New Three Dimensional Asymmetric Model of the Magnetopause Thoughts on New Three Dimensional Asymmetric Model of the Magnetopause

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsm13d1622z&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SM13D-1622

Physics

[2722] Magnetospheric Physics / Forecasting, [2724] Magnetospheric Physics / Magnetopause And Boundary Layers, [2740] Magnetospheric Physics / Magnetospheric Configuration And Dynamics, [2784] Magnetospheric Physics / Solar Wind/Magnetosphere Interactions

Scientific paper

Considering the asymmetries of the global structure of the magnetopause and indentations nearby the cusps, a new three asymmetric global model of the magnetopause is presented in this talk. Based on the magnetopause crossings from Geotail, IMP8, Interball, TC1, THEMIS, Wind, Cluster, 14 Polar, LANL, GOES and Hawkeye, and the corresponding upstream solar wind parameters from ACE, Wind or OMNI, this new model is parameterized by solar wind dynamic pressure and magnetic pressure (Dp+Bp), interplanetary magnetic field (IMF) Bz, and dipole tilt, and is constructed by the Levenberg-Marquardt method for nonlinear multi-parameter fitting step by step over the divided regions from the global system point of view. It is demonstrated that this model can be used to quantitatively study how Dp+Bp compresses the magnetopause, how IMF Bz erodes the magnetopause, how large the asymmetries of the magnetopause are, and how the dipole tilt influences the indentations and the asymmetries of the global magnetopause. In addition, the extrapolation for the distant tail magnetopause and for the extreme solar wind conditions is also considered for modeling magnetopause size and shape. Comparison with previous models implies that the standard deviation and the absolute deviation of the new model are obviously decreased. It is shown that this new model is not only appropriate to predict the magnetopause size and shape for the various solar wind conditions, but also can provide a reasonable estimation of the distant tail magnetopause shape. It is implied that this new model can be used to predict the magnetopause size and shape not only for theoretical research and numerical simulation, but also for space weather applications.

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