![]() A part of the energy is stored in the magnetotail and another part drives the convection of plasma particles in the magnetosphere. During a strong solar wind-magnetosphere coupling, a large amount of solar wind energy enters the geospace. Magnetosphere-ionosphere interaction and the subsequent energy transfer is a significant phenomenon in magnetospheric dynamics. K A represents the remaining percentage of the released energy from the previous magnetosphere-ionosphere energy transfer, stored in the ionosphere. The parameter K A plays a significant role in the entire process. The entire 23 rd solar cycle had been studied using the model. The spectral response of the simulated output follows a 1/f β power law, demonstrates a breakpoint at f 0 = 0.050 mHz (5.5 hours) having slopes β A = 2.2–2.4 for f > f 0 and β B = 0.9–1.0 for f < f 0, the typical characteristics of the natural AE index. The model produces an output series which can be regarded as a mathematical representation of the AE index. Both the direction and intensity of the real-time values of the B Z component of the interplanetary magnetic field (IMF) are the factors controlling the energy injection into the system. ![]() The input parameter to this model is derived from the real-time values of solar wind ion density and flow speed data. ![]() The model is a SOC-driven dissipative dynamical system with both spatial and temporal degrees of freedom. Magnetosphere-ionosphere energy transfer and AE fluctuations are studied using a cellular automata model of terrestrial magnetosphere based on the concept of self-organised criticality (SOC). ![]()
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