The SILCC (SImulating the LifeCycle of molecular Clouds) project - II. Dynamical evolution of the supernova-driven ISM and the launching of outflows

By P. Girichidis, Stefanie Walch, T. Naab, A. Gatto, R. Wunsch, S. Glover, Ralf Klessen, P. C. Clark, Thomas Peters, Dominik Derigs and 1 more. 2015

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The SILCC project (SImulating the Life-Cycle of molecular Clouds) aims at a more self-consistent understanding of the interstellar medium (ISM) on small scales and its link to galaxy evolution. We present three-dimensional (magneto) hydrodynamic simulations of the ISM in a vertically stratified box including self-gravity, an external potential due to the stellar component of the galactic disc, and stellar feedback in the form of an interstellar radiation field and supernovae (SNe). The cooling of the gas is based on a chemical network that follows the abundances of H+, H, H-2, C+, and CO and takes shielding into account consistently. We vary the SN feedback by comparing different SN rates, clustering and different positioning, in particular SNe in density peaks and at random positions, which has a major impact on the dynamics. Only for random SN positions the energy is injected in sufficiently low-density environments to reduce energy losses and enhance the effective kinetic coupling of the SNe with the gas. This leads to more realistic velocity dispersions (sigma(HI) approximate to 0.8 sigma(300-8000) (K) similar to 10-20 km s(-1), sigma(H alpha) approximate to 0.6(8000-3x105 K) similar to 20-30 km s(-1)), and strong outflows with mass loading factors (ratio of outflow to star formation rate) of up to 10 even for solar neighbourhood conditions. Clustered SNe abet the onset of outflows compared to individual SNe but do not influence the net outflow rate. The outflows do not contain any molecular gas and are mainly composed of atomic hydrogen. The bulk of the outflowing mass is dense (rho similar to 10(-25)-10(-24) g cm(-3)) and slow (v similar to 20-40 km s(-1)) but there is a high-velocity tail of up to v similar to 500 km s(-1) with rho similar to 10(-28)-10(-27) g cm(-3).

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/c447b31fd1e3e2ae7bdcbc0f70190666729c3969

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Citations in the corpus

Three-phase Interstellar Medium in Galaxies Resolving Evolution with Star Formation and Supernova Feedback (TIGRESS): Algorithms, Fiducial Model, and Convergence (2016, background): “…in driving turbulence and shaping the multiphase ISM in galactic disks have been extensively investigated (e.g., Korpi et al. 1999; de Avillez 2000; de Avillez & Breitschwerdt 2004; Joung & Mac Low 2006; Hill et al. 2012; Gent et al. 2013; Walch et al. 2015; Girichidis et al. 2016; Li et al. 2017).”
Theoretical Challenges in Galaxy Formation (2016, methodology): “…vertical gas column density distribution (top panels) and mid-plane temperatures (bottom panels) for three simulations of stratified galacitc disk (Σgas = 10M pc−2 shaped by supernovae (SNe) exploding at a constant rate (taken from the SILCC simulations, Girichidis et al. 2016b, Walch et al. 2015).”
The SILCC project - III. Regulation of star formation and outflows by stellar winds and supernovae (2016, background): “…find that outflows from the galactic disc can be launched by the thermal pressure of the SN-driven, hot gas, in cases where the SFR (i.e. the SN rate) is high enough to cause a hot volume filling phase (see Girichidis et al. 2016b, for wind-launching mechanisms driven by non-thermal cosmic rays).”
First results from the TNG50 simulation: galactic outflows driven by supernovae and black hole feedback (2019, background): “At small scales there are many idealized studies aimed at understanding the details of supernova-driven wind launching mechanisms (Girichidis et al. 2016; Fielding et al. 2017; Kim & Ostriker 2017) or detailed phase-interaction physics (Richings & FaucherGiguère 2018; Schneider & Robertson 2018).”
Raining on black holes and massive galaxies: the top-down multiphase condensation model (2016, background): “The minimum simulated temperature is 20 K, below which the gas is expected to be fully molecular (Girichidis et al. 2016) and nearly isothermal (Koyama & Inutsuka 2000).”