Other
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsm23b1702h&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #SM23B-1702
Other
2740 Magnetospheric Configuration And Dynamics, 2744 Magnetotail, 2760 Plasma Convection (2463), 2784 Solar Wind/Magnetosphere Interactions, 2788 Magnetic Storms And Substorms (7954)
Scientific paper
Convection is the basic response of the magnetosphere to external driving by the solar wind electric field. The supply of solar wind energy into the magnetosphere may lead to different types of magnetospheric response. These include substorms, steady magnetospheric convection (SMC), poleward boundary intensifications, and sawtooth injection events. In a steady state the magnetic flux should be balanced between dayside merging process and tail returning process. However, the magnetic flux moving between the dayside and nightside is seldom in balance and eventually leads to instability in the magnetotail. The imbalance of magnetic flux is one of the main reasons why there are different types of magnetospheric activities. At the present time, the evolution from one mode of geomagnetic activity to another is still not understood. Is it dependent upon solar wind input only or is it controlled by internal magnetospheric processes only? Is it possible that both solar wind and internal magnetospheric processes can influence different dynamic regimes? A clear understanding of this issue would provide us important information concerning how the solar wind couples with the magnetosphere. In this study we have identified several interesting intervals composed of isolated substorms, substorm to SMC and SMC to substorm during THEMIS tail passages. A detailed comparison of solar wind, magnetotail, and ground observations from these events provides a good opportunity to examine the most important processes (quantities) responsible for different modes of activity. Several indices of activity will be estimated and compared such as the auroral electrojet evolution and the associated auroral disturbance. This is particularly interesting because ionospheric dissipation may be the main energy sink for the energy deposited in the magnetosphere and its understanding can reveal important information about how a transition from one mode to another occurs. The high-latitude and mid to low latitude ULF waves will be examined to see whether this is any difference in pulsation excitation. Important tail observations such as lobe magnetic field and plasma flows will be examined to see whether the loading-unloading process is significant. Solar wind observation will be used to estimate the magnetic flux transported from the dayside. The transported flux will then be compared with the tail returning flux to examine how flux imbalance can influence the dynamic mode transition. Finally, we will examine whether there is any difference in the TEC (total electron content) during SMC and substorm time.
Amm Olaf
Angelopolous Vassilis
Ge Yufei
Hsu Ted
McPherron Robert
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