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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41 Pith papers cite this work, alongside 4,155 external citations. Polarity classification is still indexing.
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Frequent EUV microflashes at solar plume bases, each releasing ~10^24 erg, are identified as a new unipolar network event and suggested as a candidate mechanism to power the open corona and solar wind.
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.
A forward-modeling correction using real-time lens imaging reduces dust stray-light noise by 67% and restores expected coronal intensity profiles in ground-based data.
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.
New EIS effective area curves confirm factor-of-two long-wavelength degradation without fine structure and reveal inverse FIP bias with Fe/H at 0.57 of photospheric value at 10 MK, confirmed by Chandrayaan-2 SXM spectra.
NuSTAR observations of 113 faint solar X-ray transients show they are cooler and dimmer than RHESSI microflares, with quiet-Sun events having lower energies and no cases above 3x10^27 erg.
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.
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.
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.
Data-constrained 3D modeling of the 2011 August 4 flare reveals strong polarity asymmetry in electron precipitation driven by magnetic mirror ratios, with turbulent scattering and Coulomb collisions modulating the energy-dependent flux.
New observations of ~160 s VLPs in metric type-I bursts show spatiotemporal correlation with ~170 s oscillations in sunspot umbrae, supporting modulation by slow magnetoacoustic waves via plasma emission.
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.
-
Extreme Ultraviolet Microflashes at Plume Bases: A Candidate for Powering the Corona and Solar Wind?
Frequent EUV microflashes at solar plume bases, each releasing ~10^24 erg, are identified as a new unipolar network event and suggested as a candidate mechanism to power the open corona and solar wind.
-
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.
-
Forward Modeling of Dust-Induced Stray Light in Ground-Based Coronagraphs: A Dual-Path Monitoring Approach for High-Precision Inner Corona Observations
A forward-modeling correction using real-time lens imaging reduces dust stray-light noise by 67% and restores expected coronal intensity profiles in ground-based data.
-
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.
-
Modeling Flare Continuum Emission Observed by Hinode/EIS: Instrument Calibration and Element Composition Results
New EIS effective area curves confirm factor-of-two long-wavelength degradation without fine structure and reveal inverse FIP bias with Fe/H at 0.57 of photospheric value at 10 MK, confirmed by Chandrayaan-2 SXM spectra.
-
A Statistical Survey of Faint Solar X-ray Transients Observed by NuSTAR
NuSTAR observations of 113 faint solar X-ray transients show they are cooler and dimmer than RHESSI microflares, with quiet-Sun events having lower energies and no cases above 3x10^27 erg.
-
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.
-
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.
-
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.
-
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.
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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.
-
Data-Constrained Modeling of Electron Transport and Asymmetric Precipitation in the 2011 August 4 Solar Flare
Data-constrained 3D modeling of the 2011 August 4 flare reveals strong polarity asymmetry in electron precipitation driven by magnetic mirror ratios, with turbulent scattering and Coulomb collisions modulating the energy-dependent flux.
-
Spatio-temporal Characteristics of Very Long-periodic Pulsations in Solar Metrewave Bursts: Implications for their Origins
New observations of ~160 s VLPs in metric type-I bursts show spatiotemporal correlation with ~170 s oscillations in sunspot umbrae, supporting modulation by slow magnetoacoustic waves via plasma emission.
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Solar Extreme Ultraviolet Spectrograph and High-energy Imager (SEUSHI): Design, Development, and Pre-Flight Calibration
SEUSHI is a compact dual-mode instrument that delivers 1-arcmin temperature maps every 5 seconds plus 0.2-nm EUV spectra and photon-counting SXR spectroscopy to study flare initiation and elemental abundances.
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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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Full-Disk Spectroscopy of the Solar Corona Across a Solar Cycle with Hinode/EIS
Hinode/EIS full-disk mosaics show coronal intensity tracks solar cycle via active region coverage while velocity properties in log T~6.2 plasma remain stable across cycles 24-25.
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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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Bidirectional Plasma Jets Driven by Magnetic Reconnection: Observations by GST and SDO
New GST and SDO observations of bidirectional plasma jets in a sunspot link them to magnetic reconnection triggered by rising filamentary material interacting with horizontal magnetic loops.
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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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Microwave Polar Brightening and Its Connection to Polar Coronal Holes
Long-term 17 GHz microwave polar brightening shows strong correlations with polar coronal hole area and polar magnetic field strength.
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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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Analysis of Eruptive Prominence Plasma Parameters' Effects on the \ion{He}{2} 304~\AA\ Line with Solar Orbiter EUI Observations
Column mass and temperature profile steepness dominate He II 304 Å line formation in the February 15 2022 eruptive prominence, with radiative processes outweighing collisional excitation.
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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.
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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.
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Solar Radio Burst Fine Structures
Recent sub-second imaging spectroscopy of solar radio burst fine structures challenges existing theoretical models, with the SKA positioned to enable new frameworks for electron acceleration and coronal turbulence.
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Magnetic loops in the solar transition region
A review summarizing observational properties, dynamics, and heating implications of transition region loops observed primarily with IRIS, distinct from coronal loops.
- On the Nature of Candle-Flame-Shaped Solar Flares and Sub-Alfv\'enic Supra-Arcade Plasma Downflows