Turbulence from mixed-polarity magnetic carpet fields supplies enough dissipated energy to heat the solar chromosphere and lower corona, with gradual heating of spicules by entrained turbulence.
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3 Pith papers cite this work. Polarity classification is still indexing.
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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.
Galactic wind advection with a peak velocity of ~700 km/s reproduces cosmic ray spectral hardening from hundreds of GV and softening from a few TV without diffusion breaks, predicts a hard spectrum (index ~2) at 3-5 kpc altitudes consistent with Fermi bubbles, and shows the wind maintains disk metal
citing papers explorer
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Turbulence and its Potential Impact on Solar Chromospheric and Coronal Heating
Turbulence from mixed-polarity magnetic carpet fields supplies enough dissipated energy to heat the solar chromosphere and lower corona, with gradual heating of spicules by entrained turbulence.
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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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Cosmic-Ray Spectra and Metal Budget Regulated by the Galactic Wind
Galactic wind advection with a peak velocity of ~700 km/s reproduces cosmic ray spectral hardening from hundreds of GV and softening from a few TV without diffusion breaks, predicts a hard spectrum (index ~2) at 3-5 kpc altitudes consistent with Fermi bubbles, and shows the wind maintains disk metal