期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 454, 期 1, 页码 238-268出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stv1975
关键词
MHD; ISM: clouds; ISM: evolution; ISM: structure; ISM: supernova remnants; galaxies: ISM
资金
- Deutsche Forschungsgemeinschaft (DFG) [SPP 1573]
- Bonn-Cologne Graduate School
- DFG [SFB 881]
- European Research Council under European Community via ERC [339177]
- Cluster of Excellence 'Origin and structure of the Universe'
- Czech Science Foundation [209/12/1795]
- Academy of Sciences of the Czech Republic [RVO: 67985815]
- Forschungskredit of the University of Zurich [FK-13-112]
- [SFB 956]
The SILCC (SImulating the Life-Cycle of molecular Clouds) project aims to self-consistently understand the small-scale structure of the interstellar medium (ISM) and its link to galaxy evolution. We simulate the evolution of the multiphase ISM in a (500 pc)(2) x +/-5 kpc region of a galactic disc, with a gas surface density of Sigma(GAS) = 10 M-circle dot pc(-2). The FLASH 4 simulations include an external potential, self-gravity, magnetic fields, heating and radiative cooling, time-dependent chemistry of H-2 and CO considering (self-) shielding, and supernova (SN) feedback but omit shear due to galactic rotation. We explore SN explosions at different rates in high-density regions (peak), in random locations with a Gaussian distribution in the vertical direction (random), in a combination of both (mixed), or clustered in space and time (clus/clus2). Only models with self-gravity and a significant fraction of SNe that explode in low-density gas are in agreement with observations. Without self-gravity and in models with peak driving the formation of H-2 is strongly suppressed. For decreasing SN rates, the H-2 mass fraction increases significantly from <10 per cent for high SN rates, i.e. 0.5 dex above Kennicutt-Schmidt, to 70-85 per cent for low SN rates, i.e. 0.5 dex below KS. For an intermediate SN rate, clustered driving results in slightly more H-2 than random driving due to the more coherent compression of the gas in larger bubbles. Magnetic fields have little impact on the final disc structure but affect the dense gas (n greater than or similar to 10 cm(-3)) and delay H-2 formation. Most of the volume is filled with hot gas (similar to 80 per cent within +/-150 pc). For all but peak driving a vertically expanding warm component of atomic hydrogen indicates a fountain flow. We highlight that individual chemical species populate different ISM phases and cannot be accurately modelled with temperature-/density-based phase cut-offs.
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