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Compression of the Earth's magnetotail by interplanetary shocks directly drives transient magnetic flux closure

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Academic year: 2021

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Figure

Figure  1.  Solar  wind  velocity  (top  panel),  dynamic  pressure  (middle  panel)  and  IMF  B z
Figure 2. Polar view of the proton aurora captured with IMAGE-FUV SI12 (expressed in  image counts) prior to and after that an interplanetary shock did hit the Earth at 0339 UT
Figure 3. Open magnetic flux of the magnetosphere (a), flux opening rate at the dayside (b)  and flux closure rate in the magnetotail (c), 8 November 2000, deduced from combined  ground-based and global remote sensing observations
Figure 4. Solar wind dynamic pressure used as input of the MHD simulation (a). Computed  magnetic field B x  component in the tail lobe at 10 R E  (b) and computed reconnection power  (c)
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