Understanding the geoeffective properties of rapid changes in the solar wind and interplanetary magnetic field (Invited)

Details Understanding the geoeffective properties of rapid changes in the solar wind and interplanetary magnetic field (Invited) Understanding the geoeffective properties of rapid changes in the solar wind and interplanetary magnetic field (Invited)

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm23b..06r&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM23B-06

Physics

[2712] Magnetospheric Physics / Electric Fields, [2736] Magnetospheric Physics / Magnetosphere/Ionosphere Interactions, [2784] Magnetospheric Physics / Solar Wind/Magnetosphere Interactions

Scientific paper

The magnetosphere is strongly driven by the state of the solar wind and interplanetary magnetic field (IMF). When these change, the magnetosphere reacts in different ways depending on the specific change. For example, when the IMF reorients, the reconnection site needs to move and become reestablished. After this, Alfven waves propagate to the ionosphere, communicating the change. Overall, this alteration can take many minutes to initialize and 10-20 minutes to set up a new potential pattern. Conversely, when the solar wind changes and the magnetopause position alters, a fast-mode wave propagates throughout the system communicating the new state. During this time period, the ionospheric convection can become significantly enhanced for a few to tens of minutes. This has a ramification on the geoeffectiveness of highly structured solar wind and IMF, as occurs during the sheath of a coronal mass ejection. Namely, the magnetosphere acts as a low pass filter on the highly variable IMF, but reacts strongly to the strongly varying solar wind density. We present systematic simulation results that demonstrate these properties of the magnetosphere, and discuss the effectiveness of the different frequencies of variations that may encounter the magnetosphere.

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