Time-dependent MHD models of the corona-heliosphere system produce magnetic connectivities consistent with observed strahl occurrence rates, unlike steady-state models.
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Skewness parameter δ in Skew-Kappa electron distributions for solar wind scales as δ ∼ K_N, the effective Knudsen number, via a collision-modified Boltzmann equation.
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Magnetic Connectivity in the Time-Dependent Corona and Heliosphere
Time-dependent MHD models of the corona-heliosphere system produce magnetic connectivities consistent with observed strahl occurrence rates, unlike steady-state models.
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Knudsen number as a non-thermal parameter: possible origin of skewness in space plasma distributions
Skewness parameter δ in Skew-Kappa electron distributions for solar wind scales as δ ∼ K_N, the effective Knudsen number, via a collision-modified Boltzmann equation.