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Open research questions in Solar and Space Plasma Dynamics

42 unresolved questions extracted from the limitations and future-work sections of 443 Solar and Space Plasma Dynamics papers in our library. Each links back to the study that raised it.

What the literature leaves open

  • The origin of magnetic switchbacks-large-amplitude, spherically polarized magnetic-field fluctuations with local polarity inversions shown to be nearly ubiquitous in the inner heliosphere by Parker Solar Probe-is presently one of the most outstanding open questions in solar and heliospheric science.

    Potential Solar Precursors to Magnetic Switchbacks · 2026

  • Observations commonly show asymmetric HXR photon fluxes between paired footpoints, whose physical origin remains debated, as the conventional magnetic mirroring mechanism often fails to explain the observed asymmetry.

    What Causes the Asymmetry of Conjugate Hard X-Ray Footpoints in Solar Flares? · 2026

  • This similarity suggests that a CBO-like process may also operate in these fully convective, low-mass objects, though the plasma source and acceleration mechanisms remain uncertain.

    Coherent and Incoherent Emission from the Ordered Magnetospheres of Low-Mass Stars, UCDs, and Massive Stars · 2026

  • Future work will explore a broader parameter space, including more realistic mass ratios, to further assess the robustness of these results. This hypothesis remains to be tested in future work, which will investigate the coupled evolution of turbulence, expansion, and kinetic instabilities starting from nearly Maxwellian initial conditions at the onset of expansion. A key limitation of this study lies in the formation of non- Maxwellian electron VDFs (only in the perpendicular direction) prior to the onset of expansion.

    Formation of Suprathermal Electron Populations in the Expanding, Turbulent Solar Wind · 2026 · DOI

  • 
ERs occur most frequently near solar minima, consistent with earlier studies and likely reflecting AutoTAB's greater sensitivity to weaker regions when strong BMRs are scarce.

    Large ephemeral regions and their tilt angles · 2026 · DOI

  • Ultraviolet (UV) and HXR ribbon emission can show quasiperiodic pulsations (QPPs), but the link between HXR QPP sources and slipping reconnection remains poorly understood.

    Quasiperiodic Pulsations and Three-dimensional Magnetic Reconnection during 2022 March 31 Flare Observed by IRIS and STIX · 2026 · DOI

  • Comparison with in situ shock detections highlights the role of CME–solar wind interactions in shaping heliospheric signatures, though shock arrival times remain uncertain at the 11 hr level.

    Understanding the Complex Morphology of a Coronal Mass Ejection. II. How Pre-eruptive Conditions Shape Coronal Mass Ejection Evolution · 2026 · DOI

  • ・Applying stellar observations, Investigating consistency with other scaling laws. → Stellar cases in Posters of P1161 (Umezawa et al.) and P2008 (Ichihara et al.). ・Clarifying the condition for postflare loops becoming dominant in Hα emission. ＜5.

    Appearance Timing of Hα PostflareLoops: Simple Scaling Law Based on Radiative Cooling · 2026 · DOI

  • While the present study is limited to a relatively small set of events, expanding on this work with a larger sample size and performing a robust statistical analysis would allow us to investigate important questions such as: • Whether the volumetric expansion of slow CMEs differs systematically from that of fast CME • How the ambient interplanetary medium and solar cycle conditions influence CME expansion rates.

    A Study of the Kinematic and Volumetric Coevolution of Earth-directed Coronal Mass Ejections · 2026 · DOI

  • 78 Compact Research Statement The solar closure research program may therefore be summarized as follows: The Sun should be investigated as a radially stratified closure hierarchy by constructing operational proxies for shell legibility, interaction density, transition amplification, and closure Reynolds intensity, and then testing whether these observables exhibit the predicted five-band ordering from the deep interior to the corona.

    CLOSURE STELLAR PHYSICS Shell Law, Coherence Core and Partial Closure Turbulence · 2026 · DOI

  • The model achieves 0.857 precision but only 0.561 recall for Type III/Group Type III bursts, with ground truth containing 107 events but 47 false negatives. No analysis was provided on whether these missed detections correlate with specific instrumental characteristics (frequency ranges, antenna types, observing conditions) across the distributed e-CALLISTO network stations.

    Automated Detection and Classification of Solar Radio Bursts in CALLISTO Spectrograms Using Deep-Learning YOLOv5 Model and Ensemble Methods · 2026 · DOI

  • Weighted Box Fusion achieved the best performance (F1=0.738) using weight exponent 0.5 applied to model ranks, but the sensitivity to alternative weighting schemes (power laws, entropy-based weights, performance-scaled weights) was not explored. Future work should systematically optimize the weighting function for ensemble solar radio burst detection across heterogeneous YOLOv5 model architectures.

    Automated Detection and Classification of Solar Radio Bursts in CALLISTO Spectrograms Using Deep-Learning YOLOv5 Model and Ensemble Methods · 2026 · DOI

  • Model performance shows high variability across different training-validation splits due to limited dataset size, but no specific dataset size threshold or saturation analysis was performed. Quantitative experiments are needed to determine the minimum number of labeled CALLISTO spectrograms required for stable YOLOv5 performance and when additional data augmentation yields diminishing returns.

    Automated Detection and Classification of Solar Radio Bursts in CALLISTO Spectrograms Using Deep-Learning YOLOv5 Model and Ensemble Methods · 2026 · DOI

  • The optimal image resolution of 640×640 pixels for YOLOv5 models was empirically determined, but the relationship between burst feature distinguishability and resolution remains unexplored. Systematic analysis is needed to quantify how specific burst morphologies (Type II, Type III, Type IV) respond to resolution variations and to develop resolution-adaptive detection strategies for heterogeneous e-CALLISTO network instruments.

    Automated Detection and Classification of Solar Radio Bursts in CALLISTO Spectrograms Using Deep-Learning YOLOv5 Model and Ensemble Methods · 2026 · DOI

  • Annotation ambiguities between individual Type III bursts and Groups of Type III bursts limit model evaluation; the authors note that merging these categories reduces false positives but increases false negatives. A concrete annotation protocol for distinguishing spatially or temporally proximate Type III bursts in CALLISTO spectrograms needs to be established and validated across multiple human annotators.

    Automated Detection and Classification of Solar Radio Bursts in CALLISTO Spectrograms Using Deep-Learning YOLOv5 Model and Ensemble Methods · 2026 · DOI

  • Type III and Group of Type III burst classification shows substantially lower recall (0.561) compared to Type II (0.735) and Type IV (0.775) bursts in the deep learning model, with low-contrast faint bursts being missed due to high background noise variability across different e-CALLISTO instruments. Systematic investigation is needed into background noise characterization and adaptive contrast normalization strategies specific to individual radio telescope stations.

    Automated Detection and Classification of Solar Radio Bursts in CALLISTO Spectrograms Using Deep-Learning YOLOv5 Model and Ensemble Methods · 2026 · DOI

  • Soft voting ensemble method for solar radio burst detection consistently underperformed compared to individual YOLOv5 models and hard voting, but the underlying reasons for this degradation have not been investigated. Future work should analyze why soft voting with CALLISTO spectrograms produces lower F1 scores despite theoretical advantages of probability averaging.

    Automated Detection and Classification of Solar Radio Bursts in CALLISTO Spectrograms Using Deep-Learning YOLOv5 Model and Ensemble Methods · 2026 · DOI

  • Recent numerical results indicate that very high resolution and robust seeding are needed to properly resolve plasmoid-mediated fast reconnection in undriven two-dimensional MHD, suggesting limitations of current simulation capabilities.

    Conservation of magnetic-helicity fluctuations due to spatial decorrelation of fluxes in decaying MHD turbulence · 2026 · DOI

  • For the newly identified class of gauges (3.17) where magnetic-helicity may not be conserved, it is conjectured that helicity density is redistributed along wandering field lines, but this aspect requires exploration in future work.

    Conservation of magnetic-helicity fluctuations due to spatial decorrelation of fluxes in decaying MHD turbulence · 2026 · DOI

  • With these reconstructed positions, the issues we are able to analyze include but are not limited to the compression of magnetopause and widening of the cusp after an enhancement of solar wind flux, as well as the erosion of the magnetopause and equatorward motion of cusp after the southward turning of the interplanetary magnetic field.

    Soft X‐ray Imaging of the Magnetosheath and Cusps Under Different Solar Wind Conditions: MHD Simulations · 2019 · DOI

  • , the tearing or Kelvin–Helmholtz instabilities) can in theory lead to boundary perturbations with similar projected complexity, and morph- ology alone is insufficient to discriminate between candidate trigger mechanisms without additional diagnostics.

    Automatic Detection of Flare Ribbon Fine Structures as Proxies for Plasmoid Dynamics in Flare Reconnection · 2026 · DOI

  • However, the flow of CRs down pressure gradients in the hot gas does substantial additional work on the CR fluid within |z| ≲ 2 kpc.

    Cosmic-Ray Feedback in Galactic Disks: Star Formation, Cosmic-Ray Transport, and Multiphase Outflows in T <scp>igress++</scp> Simulations · 2026 · DOI

  • Using both polarized and total brightness observations yields the most accurate recon- structions, whereas two viewpoints with total brightness alone are insufficient for reliable results.

    SuNeRF-CME: Physics-informed Neural Radiance Fields for Tomographic Reconstruction of Coronal Mass Ejections · 2026 · DOI

  • This boundary has not been previously reported in the solar physics literature, where helicity thresholds have been studied exclusively in the context of eruption onset prediction.

    A Helicity-Dependent Phase Boundary for Chirality Determinacy in Solar Active Regions: Evidence from SDO/HMI SHARP Near-Real-Time Telemetry · 2026 · DOI

  • Most observational studies to date have relied on near-ecliptic measurements dominated by slow wind, and the full range of wind speed, including fast wind, is insufficiently explored.

    Investigation of Solar Wind Speed Characteristics Using IPS Observations and the PFSS+SCS Model · 2026

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42 open questions have been extracted from the limitations and future-work passages of 443 Solar and Space Plasma Dynamics papers in our library. Each one below links back to the study that raised it, so you can read the original claim in context.

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