Compact C-class solar flares with U-shaped or fan-spine magnetic structures produce white-light emission at rates near 100%, while flux-emergence types do so at only 33% and no B-class compact flares showed it.
Title resolution pending
3 Pith papers cite this work. Polarity classification is still indexing.
3
Pith papers citing it
fields
astro-ph.SR 3verdicts
UNVERDICTED 3representative citing papers
Confined flares exhibit total Lorentz force change below 1.8 × 10^22 dyne along the PIL, separating them from eruptive flares in a sample of 37 major events observed 2011-2017.
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
-
Investigation of White-light Emission in Compact Flares
Compact C-class solar flares with U-shaped or fan-spine magnetic structures produce white-light emission at rates near 100%, while flux-emergence types do so at only 33% and no B-class compact flares showed it.
-
Photospheric Lorentz force changes in eruptive and confined solar flares
Confined flares exhibit total Lorentz force change below 1.8 × 10^22 dyne along the PIL, separating them from eruptive flares in a sample of 37 major events observed 2011-2017.
-
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.