Simulating galactic outflows with kinetic supernova feedback

By Claudio Dalla Vecchia, Joop Schaye. 2008

344 citations recorded by the source corpus.

Feedback from star formation is thought to play a key role in the formation and evolution of galaxies, but its implementation in cosmological simulations is currently hampered by a lack of numerical resolution. We present and test a subgrid recipe to model feedback from massive stars in cosmological smoothed particle hydrodynamics simulations. The energy is distributed in kinetic form among the gas particles surrounding recently formed stars. The impact of the feedback is studied using a suite of high-resolution simulations of isolated disc galaxies embedded in dark haloes with total mass 10 10 and 10 12 h -1 M ⊙ . We focus, in particular, on the effect of pressure forces on wind particles within the disc, which we turn off temporarily in some of our runs to mimic a recipe that has been widely used in the literature. We find that this popular recipe gives dramatically different results because (ram) pressure forces on expanding superbubbles determine both the structure of the disc and the development of large-scale outflows. Pressure forces exerted by expanding superbubbles puff up the disc, giving the dwarf galaxy an irregular morphology and creating a galactic fountain in the massive galaxy. Hydrodynamic drag within the disc results in a strong increase in the effective mass loading of the wind for the dwarf galaxy, but quenches much of the outflow in the case of the high-mass galaxy.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ae3da011ea295ce2e268367ce018c7ddc04a44a3

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Citations in the corpus

Keeping the Universe ionized: photoheating and the clumping factor of the high-redshift intergalactic medium (2008, methodology): “We employ the prescription of Dalla Vecchia & Schaye (2008), which is a variation of the Springel & Hernquist (2003) recipe for kinetic feedback.”
Kiloparsec-scale outflows are prevalent among luminous AGN: outflows and feedback in the context of the overall AGN population (2014, background): “…models, driven by both star formation and AGN activity, to reproduceth observable properties of galaxies and the intergalactic medium (e.g., Silk & Rees 1998; Di Matteo et al. 2005; Hopkins et al. 2008; Dalla Vecchia & Schaye 2008 Booth & Schaye 2010; Debuhr et al. 2012; Hopkins et al. 2013a).”
Galaxy evolution in cosmological simulations with outflows ― I. Stellar masses and star formation rates (2011, background): “We note that decoupling has a significant impact on wind propagation; simulations without such decoupling explored e.g. by Dalla Vecchia & Schaye (2008) show that decoupling greatly enhances the ability of material to escape a galaxy’s ISM.”
Implementation of feedback in smoothed particle hydrodynamics: towards concordance of methods (2012, background): “As mentioned by Dalla Vecchia & Schaye (2008), if the gas is heated to a temperature where the cooling time becomes longer than the local dynamical time, radiative overcooling may be prevented.”
Neutral hydrogen in galaxy haloes at the peak of the cosmic star formation history (2014, background): “At the same time, powerful outflows are ubiquitous around star-forming galaxies at all redshifts (e.g., Shapley et al. 2003; Martin 2005; Weiner et al. 2009; Steidel et al. 2010; Newman et al. 2012; Jones et al. 2012; Rubin et al. 2014b) and are believed to play a major role in slowing down the grow”
Cosmological simulations of the growth of supermassive black holes and feedback from active galactic nuclei: method and tests (2009, methodology): “SF is tracked in the simulations following the prescription of Schaye & Dalla Vecchia (2008).”
The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations (2015, background): “Dalla Vecchia & Schaye (2012, see also Dalla Vecchia & Schaye 2008; Creasey et al. 2011; Keller et al. 2014; Creasey, Theuns & Bower 2015) argue that the feedback energy (canonically ∼1051 erg per 100 M for a standard IMF if considering SNe as the sole energy source) is initially distributed over…”
Cosmological simulations of the formation of the stellar haloes around disc galaxies (2011, methodology): “Feedback from supernovae is incorporated using the kinetic wind model of Dalla Vecchia & Schaye (2008) with the initial wind velocity, vw, set to 600 km/s and the massloading parameter (i.e., the ratio of the mass of gas given a velocity kick to that turned into newly formed star parti- 2 Gas…”
ESCAPE FRACTION OF IONIZING PHOTONS DURING REIONIZATION: EFFECTS DUE TO SUPERNOVA FEEDBACK AND RUNAWAY OB STARS (2014, background): “2006,ApJ, 650, 560 Ceverino, D., & Klypin, A. 2009,ApJ, 695, 292 Chabrier, G. 2003,PASP, 115, 763 Chevalier, R. A. 1974,ApJ, 188, 501 Ciardi, B., Ferrara, A., & White, S. D. M. 2003,MNRAS, 344, L7 Cioffi, D. F., McKee, C. F., & Bertschinger, E. 1988,ApJ, 334, 252 Clarke, C., & Oey, M. S. 2002,MNRAS,”
The Aquila comparison project: the effects of feedback and numerical methods on simulations of galaxy formation (2011, background): “R E F E R E N C E S Abadi M. G., Navarro J. F., Steinmetz M., Eke V. R., 2003a, ApJ, 591, 499 Abadi M. G., Navarro J. F., Steinmetz M., Eke V. R., 2003b, ApJ, 597, 21 Agertz O. et al., 2007, MNRAS, 380, 963 Agertz O., Teyssier R., Moore B., 2011, MNRAS, 410, 1391 Bell E. F., de Jong R. S., 2000, MNR”
Galaxy Evolution in Cosmological Simulations with Outflows II: Metallicities and Gas Fractions (2011, background): “For a further discussion of hydrodynamic decoupling, see Dalla Vecchia & Schaye (2008) and Paper I.”
The EAGLE project: Simulating the evolution and assembly of galaxies and their environments (2014, background): “While these factors may well contribute to the problem, Dalla Vecchia & Schaye (2012, see also Dalla Vecchia & Schaye 2008, Creasey et al. 2011 and Keller et al. 2014) argued that the fact that the energy is distributed over too much mass may be a more fundamental issue.”
Black hole evolution – I. Supernova-regulated black hole growth (2015, background): “SN feedback that is an important driver of gas-mass loss in dwarf galaxies (e.g. Springel & Hernquist 2003; Dubois & Teyssier 2008; Dalla Vecchia & Schaye 2008, 2012; Hopkins et al. 2014) also turns dark matter (DM) cusps into cores (Gnedin & Zhao 2002; Mashchenko et al. 2006; Pontzen & Governato 20”
Self-regulated growth of supermassive black holes by a dual jet-heating active galactic nucleus feedback mechanism: methods, tests and implications for cosmological simulations (2011, background): “…these particular numerical experiments demonstrate that the injection of energy through AGN feedback (but it is true for any type of feedback, see Dalla Vecchia & Schaye 2008 for a similar discussion about SN feedback) is a delicate process that cannot be naively decoupled from the gas dynamics…”
SHORT-LIVED STAR-FORMING GIANT CLUMPS IN COSMOLOGICAL SIMULATIONS OF z ≈ 2 DISKS (2010, methodology): “If the winds are not decoupled they cannot escape the vicinity of the galaxies and are ineffective (Dalla Vecchia & Schaye 2008).”
The physics driving the cosmic star formation history (2009, methodology): “…that the scalings of the ‘momentum-driven’ prescription, i.e. a wind velocity that increases and a mass loading that decreases with galaxy mass, agree qualitatively with the results obtained for high-resolution simulations of energy-driven SN feedback (Dalla Vecchia & Schaye 2008, 2009).”
Simulating galactic outflows with thermal supernova feedback (2012, background): “Three types of sub-grid recipes are commonly used to solve the over-cooling problem: injecting the energy in kinetic form (e.g. Navarro & White 1993; Mihos & Hernquist 1994; Kawata 2001; Kay et al. 2002; Springel & Hernquist 2003; Oppenheimer & Davé 2006; Dalla Vecchia & Schaye 2008; Dubois & Teyss”
The case for AGN feedback in galaxy groups (2009, methodology): “Star formation is tracked in the simulations following the prescription of Schaye & Dalla Vecchia (2008).”