An automated detection method applied to simulated flare ribbon data identifies fine structures whose motions and flux distribution are consistent with plasmoid-mediated reconnection.
Title resolution pending
6 Pith papers cite this work. Polarity classification is still indexing.
6
Pith papers citing it
fields
astro-ph.SR 6representative citing papers
High-resolution Fe I and Mg I spectral observations reveal that solar flare ribbons are modulated by stable uncombed chromospheric loops and non-flaring fine structures.
Data-driven simulation of AR 11158 produces an X-flare triggered by torus instability after MFR formation above a cPIL, with energy release and photospheric changes matching some observed trends.
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.
Statistical analysis shows solar energetic electrons rarely cross the heliospheric current sheet unless the source or spacecraft is close to it.
3D MHD simulation of successive flux-rope eruptions shows reconnection flux accumulating linearly with CME velocity, consistent with HMI/AIA observations of one event.
citing papers explorer
-
Automatic detection of Flare Ribbon Fine Structures as Proxies for Plasmoid Dynamics in Flare Reconnection
An automated detection method applied to simulated flare ribbon data identifies fine structures whose motions and flux distribution are consistent with plasmoid-mediated reconnection.
-
Solar flare ribbons structured by uncombed chromospheric loops
High-resolution Fe I and Mg I spectral observations reveal that solar flare ribbons are modulated by stable uncombed chromospheric loops and non-flaring fine structures.
-
Data-inspired simulation of AR 11158
Data-driven simulation of AR 11158 produces an X-flare triggered by torus instability after MFR formation above a cPIL, with energy release and photospheric changes matching some observed trends.
-
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.
-
Do Solar Energetic Electrons cross the Heliospheric Current Sheet? - A Statistical Study
Statistical analysis shows solar energetic electrons rarely cross the heliospheric current sheet unless the source or spacecraft is close to it.
-
Evolution of reconnection flux during eruption of magnetic flux ropes
3D MHD simulation of successive flux-rope eruptions shows reconnection flux accumulating linearly with CME velocity, consistent with HMI/AIA observations of one event.