On the onset of galactic winds in quiescent star forming galaxies

By Y. Dubois, Romain Teyssier. 2007

218 citations recorded by the source corpus.

Context. The hierarchical model of galaxy formation, despite its many successes, still overpredicts the baryons fraction locked in galaxies as a condensed phase. The efficiency of supernovae feedback, proposed a long time ago as a possible solution for this so-called “overcooling” problem, is still under debate, mainly because modelling supernovae explosions within a turbulent interstellar medium, while capturing realistic large scale flows around the galaxy is a very demanding task. Aims. Our goal is to study the effect of supernovae feedback on a disc galaxy, taking into account the impact of infalling gas on both the star formation history and the corresponding outflow structure, the apparition of a supernovae-driven wind being highly sensitive to the halo mass, the galaxy spin and the star formation efficiency. Methods. We model our galaxies as cooling and collapsing NFW spheres. The dark matter component is modelled as a static external potential, while the baryon component is described by the Euler equations using the AMR code RAMSES. Metal-dependent cooling and supernovae-heating are also implemented using state-of-the-art recipes coming from cosmological simulations. We allow for three parameters to vary: the halo circular velocity, the spin parameter and the star formation efficiency. Results. We found that the ram pressure of infalling material is the key factor limiting the apparition of galactic winds. We obtain a very low feedback efficiency, with supernovae to wind energy conversion factor around one percent, so that only low circular velocity galaxies give rise to strong winds. For massive galaxies, we obtain a galactic fountain, for which we discuss the observational properties. Conclusions. We conclude that for quiescent isolated galaxies, galactic winds appear only in very low mass systems. Although this can quite efficiently enrich the IGM with metals, they do not carry away enough cold material to solve the overcooling problem.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ead96a509d6e7f8d2eef1f8aaea370fb7bf99976

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

Implementation of feedback in smoothed particle hydrodynamics: towards concordance of methods (2012, background): “…kinetic feedback approach, in which all or part of the energy is given to the surrounding medium as momentum (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 & Teyssier 2008).”
Simulating galactic outflows with thermal supernova feedback (2012, background): “…& White 1993; Mihos & Hernquist 1994; Kawata 2001; Kay et al. 2002; Springel & Hernquist 2003; Oppenheimer & Davé 2006; Dalla Vecchia & Schaye 2008; Dubois & Teyssier 2008; Hopkins, Quataert, & Murray 2012), suppressing radiative cooling by hand (e.g. Gerritsen 1997; Mori et al. 1997; Thacker &…”
On the fraction of star formation occurring in bound stellar clusters (2012, background): “…efficiency is often taken to be χ fb ∼ 0.05 (see the discussion in Appendix B and e.g. Efstathiou 2000; Abadi et al. 2003; Robertson et al. 2005; Dubois & Teyssier 2008), but unfortunately, a detailed understanding of this parameter is still lacking (Silk 1997; Mac Low & Ferrara 1999;…”
Bimodal gas accretion in the Horizon–MareNostrum galaxy formation simulation (2008, methodology): “…of state with a 5/3 index to model the complex, multi-phase and turbulent structure of the ISM (Yepes et al. 1997; Springel & Hernquist 2003) in a simplified form (see Schaye & Dalla Vecchia (2007); Dubois & Teyssier (2008)): the ISM is defined as gas with a density greater than n0 ≃ 0.1 H/cm 3.”
The effects of galaxy formation on the matter power spectrum: a challenge for precision cosmology (2011, methodology): “They used a 50h−1 Mpc box with 10243 dark matter particles and included metal-dependent gas cooling, UV heating, star formation, SN feedback (using the kinetic feedback prescription of Dubois & Teyssier 2008) and metal enrichment.”
Relativistic jet feedback – III. Feedback on gas discs (2018, background): “…formation rate has been widely used to estimate the star formation rate in computational simulations of galaxy evolution (Springel & Hernquist 2003; Dubois & Teyssier 2008) and also in recent studies of positive feedback (such as Gaibler et al. 2012; Bieri et al. 2015; Dugan et al. 2017; Bieri et…”
The formation of disc galaxies in a ΛCDM universe (2010, methodology): “Mac Low & Ferrara (1999) demonstrated that while dwarf galaxies of mass 106−109 M⊙ efficiently can expel metals in supernovae-driven winds, virtually no mass is lost for systems of mass & 107 M⊙ (see also Dubois & Teyssier 2008).”
A Superbubble Feedback Model for Galaxy Simulations (2014, methodology): “The earliest techniques were to simply deposit a fraction of the energy released in feedback events as kinetic energy (Navarro & White (1993), Mihos & Hernquist (1994), Dubois & Teyssier (2008), etc.).”
ESCAPE FRACTION OF IONIZING PHOTONS DURING REIONIZATION: EFFECTS DUE TO SUPERNOVA FEEDBACK AND RUNAWAY OB STARS (2014, methodology): “Alternatively, the explosion can be provided in kinetic form (Navarro & White 1993; Dubois & Teyssier 2008; Dalla Vecchia & Schaye 2008).”
Black hole evolution – I. Supernova-regulated black hole growth (2015, methodology): “We test two implementations of SN feedback with the kinetic modelling of Dubois & Teyssier (2008), and the prescription from Teyssier et al. (2013) in order to probe how much the strength of SN activity can alter the growth of the central BH.”
A model for cosmological simulations of galaxy formation physics: multi-epoch validation (2013, background): “…typically include a sub-resolution model for star formation (e.g., Ascasibar et al. 2002; Springel & Hernquist 2003a; Schaye & Dalla Vecchia 2008; Dubois & Teyssier 2008; Few et al. 2012), radiative cooling (e.g., Katz et al. 1996; Wiersma et al. 2009a), and chemical enrichment (e.g., Steinmetz…”
Extended Lyman-alpha emission from cold accretion streams (2011, methodology): “To prevent artificial fragmentation (Truelove et al. 1997) our simulations employ a polytropic equation of state (Dubois & Teyssier 2008) as a subgrid recipe that keeps the mostly unresolved multi-phase interstellar medium (ISM) from collapsing and fragmenting.”
The energy and momentum input of supernova explosions in structured and ionized molecular clouds (2014, background): “…rate (Ostriker et al. 2010; Shetty & Ostriker 2012; Hopkins et al. 2 2012), eventually powering large scale galactic winds (Larson 1974; Veilleux et al. 2005; Joung & Mac Low 2006; Dubois & Teyssier 2008; Creasey et al. 2013), which might drive the enrichment of the ISM with heavy elements.”
HYDRODYNAMICS OF HIGH-REDSHIFT GALAXY COLLISIONS: FROM GAS-RICH DISKS TO DISPERSION-DOMINATED MERGERS AND COMPACT SPHEROIDS (2010, methodology): “All simulations use the kinetic feedback model described in Dubois & Teyssier (2008), with 20% of the energy from each supernovae re-injected in the form of an expanding bubble of initial radius 100 pc (assuming that the rest of the supernovae energy was radiated away before propagating up to…”
AGN-driven quenching of star formation: morphological and dynamical implications for early-type galaxies (2013, methodology): “For each individual SN explosion, after 10 Myr, energy is released spherically in a kinetic mode transferring mass, momentum and energy with a mass loading parameter fw = 1 that mimic a Sedov blast wave explosion (see Dubois & Teyssier 2008, for further details).”
The evolution of massive black holes and their spins in their galactic hosts (2012, unknown): “…Dotti, Colpi, & Haardt 2006; Dotti et al. 2009, 2010a; Maio et al. 2012; O’Shea et al. 2004; Kravtsov & Gnedin 2005; Tassis et al. 2003; Tassis, Kravtsov, & Gnedin 2008; Dubois & Teyssier 2008; Blecha et al. 2011; Guedes et al. 2011; Sijacki, Springel, & Haehnelt 2011, 2009; Teyssier et al. 2011).”
Understanding the shape and diversity of dwarf galaxy rotation curves in ΛCDM (2016, background): “They both have a dark matter particle resolution of mdm = 250 M ; a finest grid cell size gas resolution of ∆x ≈ 4 pc; and a stellar sampling mass of m∗ = 300M (see e.g. Dubois & Teyssier 2008).”
ISM properties in hydrodynamic galaxy simulations: turbulence cascades, cloud formation, role of gravity and feedback (2010, methodology): “We use the kinetic feedback model described by Dubois & Teyssier (2008).”