Magnetosonic polarization in synthetic turbulence produces field-line diffusion scaling as (δB/B)^4 with subdiffusion matching MHD simulations, unlike the (δB/B)^2 scaling for random polarization.
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Solar Orbiter data reveals SEP flux deflections associated with magnetic flux tubes, positioning SEPs as a diagnostic for solar wind structures.
Simulations demonstrate non-monotonic guide-field regulation of reconnection efficiency via balance between drift-kink suppression and tearing-mode hindrance in 3D relativistic current sheets.
Magnetic reconnection at the heliospheric current sheet produces power-law ion distributions whose spectral index and Emax scaling with charge-to-mass ratio are consistent with Parker Solar Probe data.
citing papers explorer
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Polarized 3D Synthetic Turbulence I: Magnetic Field Line Random Walk
Magnetosonic polarization in synthetic turbulence produces field-line diffusion scaling as (δB/B)^4 with subdiffusion matching MHD simulations, unlike the (δB/B)^2 scaling for random polarization.
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Probing Solar Wind Structures with Solar Energetic Particle Observations from Solar Orbiter
Solar Orbiter data reveals SEP flux deflections associated with magnetic flux tubes, positioning SEPs as a diagnostic for solar wind structures.
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Guide-Field-mediated Multiscale Instabilities in Relativistic Reconnection
Simulations demonstrate non-monotonic guide-field regulation of reconnection efficiency via balance between drift-kink suppression and tearing-mode hindrance in 3D relativistic current sheets.
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The Role of Magnetic Reconnection in Energizing Protons and Heavier Ions at the Heliospheric Current Sheet
Magnetic reconnection at the heliospheric current sheet produces power-law ion distributions whose spectral index and Emax scaling with charge-to-mass ratio are consistent with Parker Solar Probe data.