%0 Generic %1 gatto2014modelling %A Gatto, A. %A Walch, S. %A Mac Low, M. M. %A Naab, T. %A Girichidis, P. %A Glover, S. C. O. %A Wünsch, R. %A Klessen, R. S. %A Clark, P. C. %A Baczynski, C. %A Peters, T. %A Ostriker, J. P. %A Ibáñez-Mejía, J. C. %A Haid, S. %D 2014 %K ism outflows sn turbulence %T Modelling the supernova-driven ISM in different environments %U http://arxiv.org/abs/1411.0009 %X We use hydrodynamical simulations in a $(256\;pc)^3$ periodic box to model the impact of supernova (SN) explosions on the multi-phase interstellar medium (ISM) for initial densities $n =$ 0.5-30 cm$^-3$ and SN rates 1-720 Myr$^-1$. We include radiative cooling, diffuse heating, and the formation of molecular gas using a chemical network. The SNe explode either at random positions, at density peaks, or both. We further present a model combining thermal energy for resolved and momentum input for unresolved SN remnants. Random driving at high SN rates results in hot gas ($T10^6$ K) filling $> 90$% of the volume. This gas reaches high pressures ($10^4 < P/k_B < 10^7$ K cm$^-3$) due to the combination of SN explosions in the hot, low density medium and confinement in the periodic box. These pressures move the gas from a two-phase equilibrium to the single-phase, cold branch of the cooling curve. The molecular hydrogen dominates the mass ($>50$%), residing in small, dense clumps. Such a model might resemble the dense ISM in high-redshift galaxies. Peak driving results in huge radiative losses, but disrupts the densest regions by construction, producing a filamentary ISM with virtually no hot gas, and a small molecular hydrogen mass fraction ($1$%). Varying the ratio of peak to random SNe yields ISM properties in between the two extremes, with a sharp transition for equal contributions (at $n = 3$ cm$^-3$). Modern galaxies have few SNe in density peak locations due to preceding stellar winds and ionisation. The velocity dispersion in HI remains $10$ km s$^-1$ in all cases. For peak driving the velocity dispersion in H$_\alpha$ can be as high as $70$ km s$^-1$ due to the contribution from young, embedded SN remnants.

@misc{gatto2014modelling, abstract = {We use hydrodynamical simulations in a $(256\;{\rm pc})^3$ periodic box to model the impact of supernova (SN) explosions on the multi-phase interstellar medium (ISM) for initial densities $n =$ 0.5-30 cm$^{-3}$ and SN rates 1-720 Myr$^{-1}$. We include radiative cooling, diffuse heating, and the formation of molecular gas using a chemical network. The SNe explode either at random positions, at density peaks, or both. We further present a model combining thermal energy for resolved and momentum input for unresolved SN remnants. Random driving at high SN rates results in hot gas ($T\gtrsim 10^6$ K) filling $> 90$% of the volume. This gas reaches high pressures ($10^4 < P/k_\mathrm{B} < 10^7$ K cm$^{-3}$) due to the combination of SN explosions in the hot, low density medium and confinement in the periodic box. These pressures move the gas from a two-phase equilibrium to the single-phase, cold branch of the cooling curve. The molecular hydrogen dominates the mass ($>50$%), residing in small, dense clumps. Such a model might resemble the dense ISM in high-redshift galaxies. Peak driving results in huge radiative losses, but disrupts the densest regions by construction, producing a filamentary ISM with virtually no hot gas, and a small molecular hydrogen mass fraction ($\ll 1$%). Varying the ratio of peak to random SNe yields ISM properties in between the two extremes, with a sharp transition for equal contributions (at $n = 3$ cm$^{-3}$). Modern galaxies have few SNe in density peak locations due to preceding stellar winds and ionisation. The velocity dispersion in HI remains $\lesssim 10$ km s$^{-1}$ in all cases. For peak driving the velocity dispersion in H$_\alpha$ can be as high as $70$ km s$^{-1}$ due to the contribution from young, embedded SN remnants.}, added-at = {2014-11-04T09:56:12.000+0100}, author = {Gatto, A. and Walch, S. and Mac Low, M. M. and Naab, T. and Girichidis, P. and Glover, S. C. O. and Wünsch, R. and Klessen, R. S. and Clark, P. C. and Baczynski, C. and Peters, T. and Ostriker, J. P. and Ibáñez-Mejía, J. C. and Haid, S.}, biburl = {https://www.bibsonomy.org/bibtex/2c7025820ccc1f974c78eea8f370b04c3/miki}, description = {[1411.0009] Modelling the supernova-driven ISM in different environments}, interhash = {e2f8693445d1081dcc0232cd6dd27974}, intrahash = {c7025820ccc1f974c78eea8f370b04c3}, keywords = {ism outflows sn turbulence}, note = {cite arxiv:1411.0009Comment: 18 pages, 12 figures, 2 tables. Submitted to MNRAS}, timestamp = {2014-11-04T09:56:12.000+0100}, title = {Modelling the supernova-driven ISM in different environments}, url = {http://arxiv.org/abs/1411.0009}, year = 2014 }