  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 $\gamma$-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.
