Global Pc5 pulsations during strong magnetic storms: excitation mechanisms and equatorward expansion

The spatial structure of Pc5 waves during the recovery phases of strong magnetic storms is important not only for the identification of possible physical mechanisms of its excitation, but as an important parameter of the ULF driver of relativistic electrons. The dynamics of global Pc5 waves during the magnetic storms on October 29-31, 2003 and May 15, 2005 is studied, using the data from the trans-American network of magnetometers comprising SAMBA, MAGDAS, CARISMA, and MACCS arrays. We study the behavior of Pc5 wave properties and spectral characteristics with respect to latitude. One of the accepted sources of Pc5 wave activity is Kelvin-Helmholtz instability in the flanks of the magnetosphere. In our study we examine whether the KH instability is sufficient as an excitation mechanism for the observed waves? More specifically, we attempt to determine, what is the Pc5 wave generation type: self-excitation, resonant response, trigger? While the KH instability generation takes place at the outer flanks of the magnetosphere, Pc5 waves are observed at all latitudes. We determine how deep into the magnetosphere these Pc5 waves activity can extend and what is the wave energy transmission mechanism: surface mode, cavity mode, Alfven field-line resonance, magnetospheric MHD waveguide?