Periodic beaded stripes in meter-wave solar radio bursts are modeled via DPR instability to constrain source magnetic fields to 0.2-1.7 G and densities to (1-7)×10^8 cm^{-3}.
Title resolution pending
11 Pith papers cite this work. Polarity classification is still indexing.
11
Pith papers citing it
fields
astro-ph.SR 11years
2026 11verdicts
UNVERDICTED 11representative citing papers
Gaussian separation reveals that optimization and CFIT NLFFF models reproduce some coronal current signatures from magnetogram data for AR 11429 but the CFIT model alters a flux rope signature along the lower PIL.
In the 2022 March 31 solar flare, hard X-ray QPPs correlate with UV pulsations in stationary ribbon regions tied to a specific loop system in a large-scale 3D reconnection structure, while slipping kernels experience weaker non-thermal energization.
FOXES is a Vision Transformer framework that predicts solar soft X-ray irradiance from EUV observations with 0.051 dex mean absolute error while providing spatial attribution of emission sources.
CME interaction with the HCS locally replaced the current sheet and produced a >48-hour magnetic sector transition observed near Earth in October 2024.
Leading boundary of a coronal hole has higher plasma temperature, stronger unipolar field, and lower spatial irregularity than trailing boundary due to organized loops versus dispersed bipoles.
Hybrid neural network predicts eruptive versus confined solar flares from SDO/HMI magnetogram sequences, reports good performance, and links results to magnetic flux cancellation in polarity inversion lines.
Persistent same-polarity flux emergences drove collisional shearing and cancellations at a PIL, accumulating free energy and forming MFRs that produced multiple large flares including X9.0, with a pre-flare drop in photospheric free-energy area as a possible precursor.
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.
MHD modeling of the 2024 October 26 CME demonstrates that specific pre-eruptive magnetic flux rope footpoint locations and near-real-time background fields are required to reproduce observed complex morphology from multiple viewpoints without fine-tuning.
Sympathetic filament and active-region eruptions produced two overlapping CMEs whose interaction compressed southward magnetic fields, driving a major geomagnetic storm with Dst ~ -333 nT.
citing papers explorer
-
Coronal Diagnostics Via Modelling Periodic-Beaded Stripes of Solar Radio Bursts
Periodic beaded stripes in meter-wave solar radio bursts are modeled via DPR instability to constrain source magnetic fields to 0.2-1.7 G and densities to (1-7)×10^8 cm^{-3}.
-
Validating Coronal Magnetic Field Models Using Gaussian Separation
Gaussian separation reveals that optimization and CFIT NLFFF models reproduce some coronal current signatures from magnetogram data for AR 11429 but the CFIT model alters a flux rope signature along the lower PIL.
-
Quasi-periodic pulsations and three-dimensional magnetic reconnection during 2022 March 31 flare observed by IRIS & STIX
In the 2022 March 31 solar flare, hard X-ray QPPs correlate with UV pulsations in stationary ribbon regions tied to a specific loop system in a large-scale 3D reconnection structure, while slipping kernels experience weaker non-thermal energization.
-
Improving Solar Flare Soft X-ray Classification With FOXES: A Framework For Operational X-ray Emission Synthesis
FOXES is a Vision Transformer framework that predicts solar soft X-ray irradiance from EUV observations with 0.051 dex mean absolute error while providing spatial attribution of emission sources.
-
Coronal Mass Ejection and Heliospheric Current Sheet Interaction Causing a Long-Duration Magnetic Field Sector Transition
CME interaction with the HCS locally replaced the current sheet and produced a >48-hour magnetic sector transition observed near Earth in October 2024.
-
Investigating the Relationship Between Physical Properties and Spatial Irregularities at Coronal Hole Boundaries
Leading boundary of a coronal hole has higher plasma temperature, stronger unipolar field, and lower spatial irregularity than trailing boundary due to organized loops versus dispersed bipoles.
-
Predicting Associations between Solar Flares and Coronal Mass Ejections Using SDO/HMI Magnetograms and a Hybrid Neural Network
Hybrid neural network predicts eruptive versus confined solar flares from SDO/HMI magnetogram sequences, reports good performance, and links results to magnetic flux cancellation in polarity inversion lines.
-
Magnetic Evolution of Highly-Sheared Region in Active Region 13842 Producing Large X9.0 Flare
Persistent same-polarity flux emergences drove collisional shearing and cancellations at a PIL, accumulating free energy and forming MFRs that produced multiple large flares including X9.0, with a pre-flare drop in photospheric free-energy area as a possible precursor.
-
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.
-
Understanding the complex morphology of a CME II: how pre-eruptive conditions shape CME evolution
MHD modeling of the 2024 October 26 CME demonstrates that specific pre-eruptive magnetic flux rope footpoint locations and near-real-time background fields are required to reproduce observed complex morphology from multiple viewpoints without fine-tuning.
-
A Major Geomagnetic Storm in 2024 October Linked to Sympathetic CME--Prominence Eruptions
Sympathetic filament and active-region eruptions produced two overlapping CMEs whose interaction compressed southward magnetic fields, driving a major geomagnetic storm with Dst ~ -333 nT.