A publicly available simulation of an enhanced network region of the Sun

TL;DR

This paper presents a realistic simulation of the Sun's chromosphere using the Bifrost code, providing valuable data for understanding magnetic and plasma interactions in the solar outer atmosphere.

Contribution

It offers publicly available, detailed MHD simulations of the solar chromosphere, aiding comparison with observations and advancing solar physics research.

Findings

Simulation data available online for community use

Properties and limitations of the simulation discussed

Facilitates comparison between models and observations

Abstract

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.