MMS data shows perpendicular electrons dominate j·E dissipation in magnetotail magnetic structures during turbulent reconnection, with bidirectional energy transfer and quantified mechanisms including parallel E, Fermi, betatron, and polarization effects.
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Numerical MHD and test-particle simulations indicate that unsteady loop-top dynamics enhance electron acceleration efficiency compared to quasi-steady cases by mitigating betatron cooling at compressed field edges.
3D MHD modeling of candle-flame solar flares reveals Y-points do not coincide with apparent cusp tips and observed downflow speeds underestimate reconnection Alfvén speeds by 2-10x.
citing papers explorer
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Statistical study of energy dissipation in magnetic structures during turbulent reconnection in the Earth's magnetotail
MMS data shows perpendicular electrons dominate j·E dissipation in magnetotail magnetic structures during turbulent reconnection, with bidirectional energy transfer and quantified mechanisms including parallel E, Fermi, betatron, and polarization effects.
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Numerical Investigation of Efficient Electron Acceleration at an Unsteady Solar Flare Loop-Top
Numerical MHD and test-particle simulations indicate that unsteady loop-top dynamics enhance electron acceleration efficiency compared to quasi-steady cases by mitigating betatron cooling at compressed field edges.
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On the Nature of Candle-Flame-Shaped Solar Flares and Sub-Alfv\'enic Supra-Arcade Plasma Downflows
3D MHD modeling of candle-flame solar flares reveals Y-points do not coincide with apparent cusp tips and observed downflow speeds underestimate reconnection Alfvén speeds by 2-10x.