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Fig. 5

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Results of using the Newtonian approximation to obtain the pressure normal to the magnetopause associated with the solar wind static and dynamic pressures (p i and p sw) and assuming the boundary is in pressure equilibrium with the internal pressure we compute the energy density ω at all locations in the magnetospheric tail between X GSE = 0 and X GSE = −50 R E. The top panel shows the average value of ω at a given X GSM for various combinations of the model inputs IMF B z and dipole tilt ϕ. The red and blue lines are for ϕ = 0 and B z = −6 nT and 0, respectively. The pink and dashed red and cyan and dashed blue are the corresponding variations for ϕ = −33° and ϕ = +33°. The middle panel shows the difference in mean energy density for the B z = −6 nT and B z = 0 cases, δω〉, the black, green and dashed lines being for ϕ = 0, ϕ = +33° and ϕ = −33°, respectively. The bottom panel shows the rise δω〉 as a ratio of its value for B z = 0, δω〉/〈ω Bz=0.

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