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. We employ multipoint observations of the Van Allen Probes, THEMIS, GOES andCluster to present case and statistical studies of the electromagnetic field,plasma and particle response to interplanetary (IP) shocks observed by the Wind satellite. On 27 February 2014 theinitial encounter of an IP shock with the magnetopause occurred on thepostnoon magnetosphere, consistent with the observed alignment of the shockwith the spiral IMF. The dayside equatorial magnetosphere exhibited adusk–dawn oscillatory electrical field with a period of ∼330  s andpeak-to-peak amplitudes of ∼15  mV m −1 for a period of 30 min.The intensity of electrons in the energy range from 31.5 to 342 KeVresponded with periods corresponding to the shock-induced ULF (ultralow frequency) electricfield waves. We then perform a statistical study of Ey variations of theelectric field and associated plasma drift flow velocities for 60magnetospheric events during the passage of interplanetary shocks. The Ey perturbations are negative (dusk-to-dawn) in the dayside magnetosphere(followed by positive or oscillatory perturbations) and dominantly positive (dawn-to-dusk direction) in the nightside magnetosphere,particularly near the Sun–Earth line within an L-shell range from 2.5 to 5.The typical observed amplitudes range from 0.2 to 6 mV m −1 but canreach 12 mV during strong magnetic storms. We show that electric fieldperturbations increase with solar wind pressure, and the changes areespecially marked in the dayside magnetosphere. The direction of the Vx component of plasma flow is in agreement with the direction of the Ey component and is antisunward at all local times except the nightsidemagnetosphere, where it is sunward near the Sun–Earth line. The flowvelocities Vx range from 0. 2 to 40 km s −1 and are a factor of 5 to10 times stronger near noon as they correspond to greater variations of theelectric field in this region. We demonstrate that the shock-induced electricfield signatures can be classified into four different groups according tothe initial Ey electric field response and these signatures are dependenton local time. Negative and bipolar pulses predominate on the dayside whilepositive pulses occur on the nightside. The ULF electric field pulsations ofPc and Pi types produced by IP shocks are observed at all local times and inthe range of periods from several tens of seconds to several minutes. Webelieve that most electric field pulsations of the Pc5 type in the daysidemagnetosphere at L are produced by field line resonances. Weshow that the direction of the shock normal determines the direction of thepropagation of the shock-induced magnetic and plasma disturbances. Theobserved directions of velocity Vy predominately agree with those expectedfor the given spiral or orthospiral shock normal orientation.

Multisatellite observations of the magnetosphere response to changes in the solar wind and interplanetary magnetic field