Physics-based annual TSI reconstruction over three millennia yields a maximum difference of 1.04 W/m² in 50-year running means.
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Time-dependent MHD models of the corona-heliosphere system produce magnetic connectivities consistent with observed strahl occurrence rates, unlike steady-state models.
Statistical analysis shows solar energetic electrons rarely cross the heliospheric current sheet unless the source or spacecraft is close to it.
This review summarizes the basic principles of electron transport in inhomogeneous and tangled magnetic fields through gyro-centre trajectories, kinetic instabilities, trapping, and diffusion processes.
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