  Enshrouded in several well-known controversies, dwarf galaxies have been
extensively studied to learn about the underlying cosmology, notwithstanding
that physical processes regulating their properties are poorly understood. To
shed light on these processes, we introduce the Pandora suite of 17
high-resolution (3.5 parsec half-cell side) dwarf galaxy formation cosmological
simulations. Commencing with thermo-turbulent star formation and mechanical
supernova feedback, we gradually increase the complexity of physics
incorporated leading to full-physics models combining magnetism, on-the-fly
radiative transfer and the corresponding stellar photoheating, and
SN-accelerated cosmic rays. We investigate combinations of these processes,
comparing them with observations to constrain what are the main mechanisms
determining dwarf galaxy properties. We find hydrodynamical `SN feedback-only'
simulations struggle to produce realistic dwarf galaxies, leading either to
overquenched or too centrally concentrated, dispersion dominated systems when
compared to observed field dwarfs. Accounting for radiation with cosmic rays
results in extended and rotationally-supported systems. Spatially `distributed'
feedback leads to realistic stellar and HI masses as well as kinematics.
Furthermore, resolved kinematic maps of our full-physics models predict
kinematically distinct clumps and kinematic misalignments of stars, HI and HII
after star formation events. Episodic star formation combined with its
associated feedback induces more core-like dark matter central profiles, which
our `SN feedback-only' models struggle to achieve. Our results demonstrate the
complexity of physical processes required to capture realistic dwarf galaxy
properties, making tangible predictions for integral field unit surveys, radio
synchrotron emission, and for galaxy and multi-phase interstellar medium
properties that JWST will probe.
