Integral field spectroscopy of Na I D1/D2 lines reveals standing ~5.5 mHz oscillations at a sunspot umbral center indicating resonance-cavity dynamics, with propagating modes and damping at the boundary.
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31 Pith papers cite this work. Polarity classification is still indexing.
31
Pith papers citing it
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A multi-height extrapolation framework using chromospheric vector data recovers a pre-eruptive flux-rope configuration in an observed solar filament, outperforming photosphere-only models in simulation tests.
Comet Lovejoy deposits 10^14-10^16 W via SPMI, below the 10^17 W brightening intensity but potentially able to trigger solar flares as a magnetic perturbation.
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}.
Multi-wavelength timing analysis of an X-class flare reveals temperature-dependent phase drifting in 5-minute QPPs, interpreted as evidence for periodic magnetic reconnection triggered by lower-atmosphere oscillations.
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.
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.
Non-force-free initial magnetic fields in solar flare simulations release about twice the magnetic energy and yield EUV emission closer to observations than conventional NLFF extrapolations.
Realistic 3D MHD modeling of observed active region AR 11166 reproduces key observed properties of quasi-periodic fast propagating magnetosonic waves with improved qualitative agreement over idealized setups.
Observations of coronal rain downflows reveal preceding compressions, microflare-scale impact energy, hot rebound flows carrying under 15% of kinetic energy, and footpoint heating signatures matching TNE-TI cycles.
DEM analysis of the 6 September 2011 coronal wave finds 6-8% density and 10-18% temperature increases at the front, indicating heating mechanisms in addition to compressional adiabatic heating.
Observational report of polar polarity reversal times in solar cycle 25 from Hinode data, with northern reversal in November 2024 and southern in October 2024.
Shock waves from nonlinear steepening in the chromosphere drive spicules, transition to large-amplitude compressive MHD waves in the corona depending on field strength, produce PCDs, show period evolution from ~5 to >=10 minutes, and supply mass flux toward the solar wind.
Analysis of the September 6, 2011 coronal wave with the SOLERwave multi-sector method reveals over 40% speed variation (750-1500 km/s) between northward and northwestward segments, attributed to differences in magnetosonic speed from an MHD solution.
Composite three-channel preprocessing of SDO/AIA images yields a YOLOv5 prominence detector with mAP@50 of 0.749 and 78% recall that also generalizes to SUVI data.
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.
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.
Network regions with more compact positive-polarity magnetic features produce both visible coronal plumes and higher, faster transition-region jets.
Light bridge transverse motions appear as projections of umbral core dynamics with coupling to coronal loops.
Observational data-driven MHD simulations reproduced an X1.6 flare's onset and showed that photospheric velocity input extends prediction lead time beyond one hour.
citing papers explorer
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Standing oscillations in a resonant sunspot atmosphere captured by integral field spectroscopy
Integral field spectroscopy of Na I D1/D2 lines reveals standing ~5.5 mHz oscillations at a sunspot umbral center indicating resonance-cavity dynamics, with propagating modes and damping at the boundary.
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Chromospheric magnetic field extrapolations reveal the flux-rope configuration of a solar filament
A multi-height extrapolation framework using chromospheric vector data recovers a pre-eruptive flux-rope configuration in an observed solar filament, outperforming photosphere-only models in simulation tests.
-
Sungrazer comets as analogs of star-planet magnetic interactions
Comet Lovejoy deposits 10^14-10^16 W via SPMI, below the 10^17 W brightening intensity but potentially able to trigger solar flares as a magnetic perturbation.
-
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}.
-
Phase-drifting with emitting plasma temperature in the quasi-periodic pulsations of an X-class solar flare
Multi-wavelength timing analysis of an X-class flare reveals temperature-dependent phase drifting in 5-minute QPPs, interpreted as evidence for periodic magnetic reconnection triggered by lower-atmosphere oscillations.
-
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.
-
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.
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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.
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Energetics and Emission in a Simulated Solar Flare Initialised by a Non-Force Free Magnetic Field
Non-force-free initial magnetic fields in solar flare simulations release about twice the magnetic energy and yield EUV emission closer to observations than conventional NLFF extrapolations.
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Modeling the Excitation, Propagation and Damping of Quasi-Periodic Fast Magnetosonic Waves in Realistic Coronal Active Region Magnetic Field Structures
Realistic 3D MHD modeling of observed active region AR 11166 reproduces key observed properties of quasi-periodic fast propagating magnetosonic waves with improved qualitative agreement over idealized setups.
-
Compression, Impact and Hot Rebound Flows from Coronal Rain Downflows
Observations of coronal rain downflows reveal preceding compressions, microflare-scale impact energy, hot rebound flows carrying under 15% of kinetic energy, and footpoint heating signatures matching TNE-TI cycles.
-
DEM analysis of the 6 September 2011 large-scale coronal wave
DEM analysis of the 6 September 2011 coronal wave finds 6-8% density and 10-18% temperature increases at the front, indicating heating mechanisms in addition to compressional adiabatic heating.
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Polarity Reversal of the Polar Magnetic Fields in Solar Cycle 25
Observational report of polar polarity reversal times in solar cycle 25 from Hinode data, with northern reversal in November 2024 and southern in October 2024.
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On the Relationship between Solar Spicules and Propagating Coronal Disturbances: The Role of Shocks
Shock waves from nonlinear steepening in the chromosphere drive spicules, transition to large-amplitude compressive MHD waves in the corona depending on field strength, produce PCDs, show period evolution from ~5 to >=10 minutes, and supply mass flux toward the solar wind.
-
Investigation of the Two-Dimensional Velocity Field of the Large-Scale Coronal Wave from September 6, 2011 using the SOLERwave Tool
Analysis of the September 6, 2011 coronal wave with the SOLERwave multi-sector method reveals over 40% speed variation (750-1500 km/s) between northward and northwestward segments, attributed to differences in magnetosonic speed from an MHD solution.
-
A Robust Deep Learning Framework for Prominence Detection through Composite Feature Representations
Composite three-channel preprocessing of SDO/AIA images yields a YOLOv5 prominence detector with mAP@50 of 0.749 and 78% recall that also generalizes to SUVI data.
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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.
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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.
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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.
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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.
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On the relation between transition region network jets and coronal plumes
Network regions with more compact positive-polarity magnetic features produce both visible coronal plumes and higher, faster transition-region jets.
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Apparent Transverse Motion of Light Bridges Coupled to Coronal Loop Dynamics
Light bridge transverse motions appear as projections of umbral core dynamics with coupling to coronal loops.
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Predictability of a solar flare in May 2024 using observational data-driven MHD simulations
Observational data-driven MHD simulations reproduced an X1.6 flare's onset and showed that photospheric velocity input extends prediction lead time beyond one hour.
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Oscillatory Phase and Acoustic Travel-Time Inconsistencies Measured between SDO/HMI and GONG Dopplergrams
Contemporaneous Dopplergram analysis reveals time-varying northwestern phase anomalies and east-west travel-time inconsistencies in both SDO/HMI and GONG data, indicating systematic artifacts.
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Recurrent Coronal Jets and QPPs: Periodic Reconnection and Localized Heating Across Quiet-Sun to Active Regions
Recurrent coronal jets show QPPs of 6-13 min periods driven by periodic reconnection, with flux periodicities and sub-cooling timescales implying persistent localized heating in fan-spine structures.
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An Improved HDBSCAN-based Detection and Tracking Method for Solar Active Regions in Magnetograms
HARDAT applies HDBSCAN clustering with differential-rotation tracking and SVM-based polarity inversion line extraction to magnetograms, claiming superior sensitivity, accuracy and identity continuity over DBSCAN-based DSARD and NOAA catalogs.
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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.
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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.
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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.
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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.