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Outstanding Issues

Delve into the intricate world of solar flares, from morphology to particle acceleration mechanisms. Explore flare intensity distribution, morphology, energetic particles, and the energetics of flares. Investigate CMEs, shock development, and seed population for large SEP events. Unravel the mysteries of flare acceleration mechanisms, ultra-heavy ion enhancements, and spectral shapes of 3He in impulsive events. Examine energy-dependent charge states and the implications for flare acceleration and particle transport.

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Outstanding Issues

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  1. Outstanding Issues Gordon Holman&The SPD Summer SchoolFaculty and Students

  2. Origin of Flares • What active region evolution precedes flares and coronal mass ejections? • What is the relationship between flares and filament eruptions? • What is the relationship between flares and coronal mass ejections?

  3. Flare Intensity Distribution • Does the distribution continue to lower intensities with the -1.8 power-law index? • What is and what determines the highest “intensity” flare? • Is coronal heating dominated by “nanoflares”?

  4. Flare Morphology • Do single-loop flares exist? • Do all flare loops or arcades have the cusp structure? • Do the basic features of the “standard model” apply to all flares? • Is the “magnetic breakout” model valid? • Is multipolar magnetic structure necessary for flares?

  5. Energetic Particles I • Exactly where are energetic particles injected into the flaring region? • What is the highest particle energy in each flare? • What are the lowest particle energies in each flare? • What is the angular distribution of the particles?

  6. Energetic Particles II • How are the energetic particles “seen” in microwaves related to those “seen” in hard X-rays? • How can electron and ion produced sources be in different locations? • What is the exciter of white light flares?

  7. Energetic Particles III – Gamma Ray Results • Relationship of impulsive SEPs and particles producing flare X-ray and gamma-ray emission. • Energy content of the low-energy (<1 MeV) ions • Composition (heavy element and 3He enhancements) of the accelerated particles producing flare gamma-ray emission. • Understanding the high-density(>1013 cm–3)-high-temperature(>105 K) environment implied by the positron annihilation line observations. • Explanation for how the coronal-like high-FIP enhancements implied by gamma-ray line observations can already be present at chromospheric densities.

  8. Particle Acceleration • Is there one dominant particle acceleration mechanism? If so, what is it? • Is particle acceleration confined to a region high in the corona, or is it more distributed? • What is the efficiency of particle acceleration?

  9. Flare Energetics • What is the relative amount of energy injected directly into plasma heating vs. particle acceleration? • What is the relative amount of energy injected into electrons vs. ions? • What is the relative amount of energy injected directly into cooler plasma vs. “hot” plasma? • What is the relative amount of energy contained in the flare vs. the CME • What is the total magnetic energy released in each flare?

  10. Coronal Mass Ejections • Are there reliable precursors? Can we predict CMEs? • How are CMEs initiated and why? • How do CMEs affect the large-scale corona? • What is the relationship between CMEs, flares, and filaments? • What is the 3-D structure of CMEs? • Where do shocks develop?

  11. What is the seed population for large SEP events? does the composition depend on energy? what are the relative contributions of solar wind, coronal, and flare material? Do flare particles escape large flaring regions when associated with large/fast CMEs and if so, how? Do perpendicular shocks have a higher injection threshold energy than parallel shocks? How low in the corona can CME-driven shocks form and accelerate particles? to what energies? over what time scales? What does the energy dependent charge states in impulsive events mean? in terms of seed population for flare acceleration in terms of stripping in the corona in terms of where the acceleration is taking place Outstanding SEP issues

  12. Why do so many interplanetary shocks not accelerate particles? What is the flare acceleration mechanism and can it explain the high enhancements of ultra-heavy ions in impulsive events? What does the different spectral shapes of 3He in impulsive events tell us? about the acceleration process about the transport process Outstanding SEP Issues

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