Other
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsm23b1693c&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #SM23B-1693
Other
2134 Interplanetary Magnetic Fields, 2740 Magnetospheric Configuration And Dynamics, 2753 Numerical Modeling, 2784 Solar Wind/Magnetosphere Interactions, 2788 Magnetic Storms And Substorms (7954)
Scientific paper
Observations indicate that the magnitude of southward interplanetary magnetic field (IMF) contributes to different magnetosphere response modes. Using the University of Michigan Space Weather Modeling Framework (SWMF), including a global magnetosphere model, coupled with an inner magnetosphere model and an ionosphere electrodynamics model, we attempt to quantify the role of the IMF Bz in determining the level of activity in the magnetosphere. In separate experiments, the IMF Bz component is set to -2.5 nT, - 5 nT, -10 nT, -15 nT and -20 nT while keeping the other input solar wind parameters constant. We have found that the magnetosphere becomes more and more active as IMF Bz becomes more negative. The average vertical magnetic field at geosynchronous orbit, at all local times, decrease systematically, i.e., the inner magnetosphere becomes more stretched as the IMF Bz becomes more negative. The standard deviation also becomes larger, implying that the magnetosphere shows more variability. When the IMF is weak (-2.5 nT), the magnetic field at local midnight is quasi-steady. The magnetosphere starts to show quasi- periodic (~ 2 hours) dipolarizations when IMF is -5 nT and stronger. However, as the IMF Bz becomes more negative, increased turbulence develops around the inner magnetosphere and appears to disrupt the periodic formation of the night side reconnection.
Cai Xu
Clauer Robert C.
Ridley Aaron J.
Tóth Géza
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