  Context. The solar chromosphere is the interface between the solar surface
and the solar corona. Modelling of this region is difficult because it
represents the transition from optically thick to thin radiation escape, from
gas-pressure domination to magnetic-pressure domination, from a neutral to an
ionised state, from MHD to plasma physics, and from near-equilibrium (LTE) to
non-equilibrium conditions.
  Aims. Our aim is to provide the community with realistic simulations of the
magnetic solar outer atmosphere. This will enable detailed comparison of
existing and upcoming observations with synthetic observables from the
simulations, thereby elucidating the complex interactions of magnetic fields
and plasma that are crucial for our understanding of the dynamic outer
atmosphere.
  Methods. We used the radiation magnetohydrodynamics code Bifrost to perform
simulations of a computational volume with a magnetic field topology similar to
an enhanced network area on the Sun.
  Results. The full simulation cubes are made available online. The general
properties of the simulation are discussed, and limitations are discussed.
