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We present new 3D magnetohydrodynamic (MHD) simulations of asupernova-driven, stratified interstellar medium. These simulations were runusing the Waagan (2009) positivity preserving scheme for ideal MHD implementedin the Flash code. The scheme is stable even for the Mach numbers approaching100 found in this problem. We have previously shown that the densitydistribution arising from hydrodynamical versions of these simulations createslow-density pathways through which Lyman continuum photons can travel toheights |z| > 1 kpc. This naturally produces the warm ionized medium throughphotoionization due primarily to O stars near the plane. However, our earliermodels reproduce the peak but not the width of the observed emission measuredistribution. Here, we examine whether inclusion of magnetic fields and agreater vertical extent to the simulation domain produce a gas distributionthat better matches the observations. We further study the change of magneticenergy over time in our models, showing that it appears to reach a steady stateafter a few hundred megayears, presumably supported by a turbulent dynamodriven by the supernova explosions.

MHD simulations of a supernova-driven ISM and the warm ionized medium using a positivity preserving ideal MHD scheme