Mon. Not. R. Astron. Soc., 465, 4611-4633 (2017/March-2)
The impact of magnetic fields on the chemical evolution of the supernova-driven ISM.
PARDI A., GIRICHIDIS P., NAAB T., WALCH S., PETERS T., HEITSCH F., GLOVER S.C.O., KLESSEN R.S., WUNSCH R. and GATTO A.
Abstract (from CDS):
We present three-dimensional magneto-hydrodynamical simulations of the self-gravitating interstellar medium (ISM) in a periodic (256 pc)3 box with a mean number density of 0.5 cm–3. At a fixed supernova rate we investigate the multi-phase ISM structure, H2 molecule formation and density-magnetic field scaling for varying initial magnetic field strengths (0, 6 x 10–3, 0.3, 3 µG). All magnetic runs saturate at mass-weighted field strengths of ∼1-3 µG but the ISM structure is notably different. With increasing initial field strengths (from 6 x 10–3 to 3 µG) the simulations develop an ISM with a more homogeneous density and temperature structure, with increasing mass (from 5 to 85 per cent) and volume filling fractions (VFFs; from 4 to 85 per cent) of warm (300 < T < 8000 K) gas, with decreasing VFFs from ∼35 to ∼12 per cent of hot gas (T > 105 K) and with a decreasing H2 mass fraction (from 70 to < 1 per cent). Meanwhile, the mass fraction of gas in which the magnetic pressure dominates over the thermal pressure increases by a factor of 10, from 0.07 for an initial field of 6 x 10–3 µG to 0.7 for a 3 µG initial field. In all but the simulations with the highest initial field strength self-gravity promotes the formation of dense gas and H2, but does not change any other trends. We conclude that magnetic fields have a significant impact on the multi-phase, chemical and thermal structure of the ISM and discuss potential implications and limitations of the model.
MHD - turbulence - methods: numerical - ISM: clouds - ISM: magnetic fields - ISM: supernova remnants - ISM: supernova remnants
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