On November 9, 2004, the WIND spacecraft detected a typical interplanetary shock. Before the shock, there is a sustaining weak southward magnetic field lasting about 50 min. Across the shock front, the magnetic field turns northward, and the solar wind dynamic pressure is abruptly enhanced, i.e., the shock is a strong Dynamic Pressure Pulse (DPP). The magnetosphere is compressed to a rather small region upon the impact of the DPP. During the impingement of the shock, the magnetospheric compression causes two-mode disturbances of the energetic particle at the geosynchronous orbit, i.e., particle flux enhancement due to the compression near dawn and dusk and dispersionless particle injection similar to substorm. The disturbances propagate from the dayside to the nightside. The energetic particle fluxes on the dayside first increase, and then after about 1 min, the particle fluxes near dawn and dusk on the nightside begin to increase. Finally, dispersionless particle injection is seen near the midnight. Furthermore, near the noon the responses of electron are prior to those of proton. Contrarily, near the midnight the responses of proton are prior to those of electron. By using GOES-10 and GOES-12 observations on two sides of the noon, it is found that the magnetic field on the dawn-noon sector is simply compressed, while for the magnetic field on the noon-dusk sector, Bx and Bz component decreases, but By component notably increases. The TC-1 spacecraft located at near-Earth low-latitude lobe region observes the shock-induced lobe SI phenomena.
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