Magnetic Energy Powers the Corona: How We Can Understand its 3D Storage & Release

Authors:
  • ACAmir Caspi
    Amir Caspi
  • DSDaniel B. Seaton
    Daniel B. Seaton
  • RCRoberto Casini
    Roberto Casini
  • CDCooper Downs
    Cooper Downs
  • SGSarah E. Gibson
    Sarah E. Gibson
  • HGHolly Gilbert
    Holly Gilbert
  • LGLindsay Glesener
    Lindsay Glesener
  • SGSilvina E. Guidoni
    Silvina E. Guidoni
  • JHJ. Marcus Hughes
    J. Marcus Hughes
  • DMDavid McKenzie
    David McKenzie
  • JPJoseph Plowman
    Joseph Plowman
  • KRKatharine K. Reeves
    Katharine K. Reeves
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Abstract
The coronal magnetic field is the prime driver behind many as-yet unsolved mysteries: solar eruptions, coronal heating, and the solar wind, to name a few. It is, however, still poorly observed and understood. We highlight key questions related to magnetic energy storage, release, and transport in the solar corona, and their relationship to these important problems. We advocate for new and multi-point co-optimized measurements, sensitive to magnetic field and other plasma parameters, spanning from optical to $γ$-ray wavelengths, to bring closure to these long-standing and fundamental questions. We discuss how our approach can fully describe the 3D magnetic field, embedded plasma, particle energization, and their joint evolution to achieve these objectives.
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