Three MURaM simulations of a coronal loop at 60, 24, and 12 km grid spacing show that bulk properties and synthetic EUV emission largely saturate at 24 km, while small-scale currents and velocities continue to change.
EUV line emission from a multi-threaded coronal loop
3 Pith papers cite this work, alongside 9 external citations. Polarity classification is still indexing.
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3D rMHD simulations show coronal nanojets originate in cool dense plasma during reconnection, explaining their collimation and visibility across wavelengths.
Pre-flare IRIS observations of an X9 flare reveal 7-21 minute oscillations and rising Si IV velocities consistent with slow coronal magnetic destabilization before rapid reconnection.
citing papers explorer
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Effect of Numerical Resolution on Synthetic Observables of Simulated Coronal Loops
Three MURaM simulations of a coronal loop at 60, 24, and 12 km grid spacing show that bulk properties and synthetic EUV emission largely saturate at 24 km, while small-scale currents and velocities continue to change.
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On the cool nature of coronal nanojets
3D rMHD simulations show coronal nanojets originate in cool dense plasma during reconnection, explaining their collimation and visibility across wavelengths.
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Investigating Pre-flare Signatures in Spectroscopic Observations of an X9-class Solar Flare
Pre-flare IRIS observations of an X9 flare reveal 7-21 minute oscillations and rising Si IV velocities consistent with slow coronal magnetic destabilization before rapid reconnection.