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We present three-dimensional magneto-hydrodynamical simulations of theself-gravitating interstellar medium (ISM) in a periodic (256 pc)$^3$ box witha mean number density of 0.5 cm$^{-3}$. At a fixed supernova rate weinvestigate the multi-phase ISM structure, H$_{2}$ molecule formation anddensity-magnetic field scaling for varying initial magnetic field strengths (0,$6\times 10^{-3}$, 0.3, 3 $\mu$G). All magnetic runs saturate at mass weightedfield strengths of $\sim$ 1 $-$ 3 $\mu$G but the ISM structure is notablydifferent. With increasing initial field strengths (from $6\times 10^{-3}$ to 3$\mu$G) the simulations develop an ISM with a more homogeneous density andtemperature structure, with increasing mass (from 5% to 85%) and volume fillingfractions (from 4% to 85%) of warm (300 K $<$ T $<$ 8000 K) gas, withdecreasing volume filling fractions (VFF) from $\sim$ 35% to $\sim$ 12% of hotgas (T $> 10^5$ K) and with a decreasing H$_{2}$ mass fraction (from 70% to $<$1%). Meanwhile the mass fraction of gas in which the magnetic pressuredominates over the thermal pressure increases by a factor of 10, from 0.07 foran initial field of $6\times 10^{-3}$ $\mu$G to 0.7 for a 3 $\mu$G initialfield. In all but the simulations with the highest initial field strengthself-gravity promotes the formation of dense gas and H$_{2}$, but does notchange any other trends. We conclude that magnetic fields have a significantimpact on the multi-phase, chemical and thermal structure of the ISM anddiscuss potential implications and limitations of the model.

The impact of magnetic fields on the chemical evolution of the supernova-driven ISM