A model of supernova feedback in galaxy formation

By G. Efstathiou. 2000

239 citations recorded by the source corpus.

ABSTRA C T A model of supernova feedback during disc galaxy formation is developed. The model incorporates infall of cooling gas from a halo, and outflow of hot gas from a multiphase interstellar medium (ISM). The star formation rate is determined by balancing the energy dissipated in collisions between cold gas clouds with that supplied by supernovae in a disc marginally unstable to axisymmetric instabilities. Hot gas is created by thermal evaporation of cold gas clouds in supernova remnants, and criteria are derived to estimate the characteristic temperature and density of the hot component and hence the net mass outflow rate. A number of refinements of the model are investigated, including a simple model of a galactic fountain, the response of the cold component to the pressure of the hot gas, pressure-induced star formation and chemical evolution. The main conclusion of this paper is that low rates of star formation can expel a large fraction of the gas from a dwarf galaxy. For example, a galaxy with circular speed ,50 km s 21 can expel ,60‐80 per cent of its gas over a time-scale of ,1 Gyr, with a star formation rate that never exceeds ,0.1 M( yr 21 . Effective feedback can therefore take place in a quiescent mode and does not require strong bursts of star formation. Even a large galaxy, such as the Milky Way, might have lost as much as 20 per cent of its mass in a supernova-driven wind. The models developed here suggest that dwarf galaxies at high redshifts will have low average star formation rates and may contain extended gaseous discs of largely unprocessed gas. Such extended gaseous discs might explain the numbers, metallicities and metallicity dispersions of damped Lyman a systems.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/4bfd5f6b6436d89d4829c931b27c28322a49b077

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. R. Dav'e
4. A. Dekel
5. Volker Springel
6. R. Somerville
7. T. Naab
8. E. Quataert

Citations in the corpus

• Keck Absorption-Line Spectroscopy of Galactic Winds in Ultraluminous Infrared Galaxies (2002, background): “Finally, these outflows could be responsible for the damped Ly or strong Mg ii absorption systems observed in quasar spectra (e.g., Efstathiou 2000; Chen et al. 2001; Bond et al. 2001) and may contribute to reionization by opening a path for Lyman continuum photons to escape star-forming regions…”
• Cosmological smoothed particle hydrodynamics simulations: a hybrid multiphase model for star formation (2002, background): “Winds have been investigated in a number of theoretical studies (Mac Low & Ferrara, 1999; Aguirre et al., 2001a,b,c; Efstathiou, 2000; Madau et al., 2001; Scannapieco et al., 2001, among others), but the mechanism by which galactic outflows originate is not yet well understood.”
• From Rings to Bulges: Evidence for Rapid Secular Galaxy Evolution at z ~ 2 from Integral Field Spectroscopy in the SINS Survey (2008, background): “A simple check of this assertion is possible if one assumes that below a certain critical halo mass, supernova feedback prevents early star formation from converting a large fraction of the baryonic gas into stars (Dekel & Silk 1986; Efstathiou 2000).”
• The dependence of star formation history and internal structure on stellar mass for 105 low‐redshift galaxies (2002, unknown): “(e.g. McKee & Ostriker 1977; Efstathiou 2000).”
• Breathing in Low-Mass Galaxies: A Study of Episodic Star Formation (2007, unknown): “44 94 v1 [ as tr oph ] 3 1 M ay 2 00 7 Low & Ferrara 1999; Scannapieco et al. 2000, 2001; Recchi et al. 2001; Efstathiou 2000; Fragile et al. 2003; Fujita et al. 2003; Pelupessy et al. 2004; Hensler et al. 2004; Marcolini et al. 2006).”
• C II* Absorption in Damped Lyα Systems. I. Star Formation Rates in a Two-Phase Medium (2003, background): “This process has been invoked in hierarchical cosmologies in order to prevent the collapse of too many baryons into low-mass dark matter halos, and to explain the angular momentum distribution of current galaxy disks (Efstathiou 2000).”
• Cool outflows in galaxies and their implications (2020, background): “It is possible for a cold phase to form in situ via thermal instabilities and condensation from hot gas with a cooling time shorter than its dynamical time (Efstathiou 2000; Silich et al. 2003).”
• The Metal Content of Dwarf Starburst Winds: Results from Chandra Observations of NGC 1569 (2002, background): “A definitive measurement of a supersolar alpha-element to iron abundance ratio in the IGM would allow one to conclude that starburst winds, rather than winds generated during non-starburst periods (e.g., Efstathiou 2000) or tidal debris (e.g., Gnedin 1998), dominate the IGM enrichment.”
• Baryons in the Warm-Hot Intergalactic Medium (2000, methodology): “…here are capable of resolving supernovadriven galactic winds through a multi-phase interstellar medium, which are likely to be responsible for distributing energy and metals into the diffuse IGM (Mac Low 2000; Efstathiou 2000), thus we are relying on heuristic modeling of these processes.”
• The evolution of ΩHI and the epoch of formation of damped Lyman α absorbers (2001, background): “Models from Efstathiou (2000) indicate that DLA systems might predominantly be due to the outer parts of galaxies which do not even participate in star formation.”
• THE ARECIBO LEGACY FAST ALFA SURVEY. X. THE H i MASS FUNCTION AND FROM THE 40% ALFALFA SURVEY (2010, background): “Other processes related to star formation, such as supernova feedback (Efstathiou 2000) can remove gas from galaxies, preferentially removing baryons from those early galaxies residing in weak potential wells.”
• The Large-Scale and Small-Scale Clustering of Lyman Break Galaxies at 3.5 ⩽ z ⩽ 5.5 from the GOODS Survey (2005, background): “A possible physical explanation for this fact could be that in low-mass halos; gas cooling (hence star formation) is much more inefficient due to photoionization (squelching) or supernova feedback (e.g., Silk 1997, Efstathiou 2000).”
• Radiation Pressure-supported Starburst Disks and Active Galactic Nucleus Fueling (2005, background): “Models for feedback in the ISM generally invoke energy and momentum injection by supernovae and stellar winds (e.g., McKee & Ostriker 1977; Silk 1997; Efstathiou 2000).”
• Galaxy formation theory (2010, methodology): “Efstathiou (2000) does this by assuming that supernovae remnants have a porosity of unity (i.e. the total volume of remnants equals the volume of the galaxy,thereby creating an overlapping network of remnants).”
• Dwarf galaxy rotation curves and the core problem of dark matter haloes (2000, result): “Although current understanding of feedback is very limited, and we are reluctant to impose stringent lower limits on fbar, such high ejection efficiencies seem inconsistent with the high values of V200 inferred from the best-fit models (see e.g., Dekel & Silk 1986; Efstathiou 2000).”
• A simple model for the evolution of disc galaxies: the Milky Way (2005, background): “…one ring and avoided com plicated feedback and m ixing processes that m ight be m ore or less im portant in the early or late phases ofthe disc evolution (see e.g.Efstathiou 2000) Allthe above processes m ight play a role during disc galaxy evolution but were not im plicitly included in the m odel.”
• An origin for multiphase gas in galactic winds and haloes (2015, methodology): “Following Wang (1995a,b) and a number of other works including Efstathiou 2000; Silich et al. 2003, 2004; Tenorio-Tagle et al. 2003, 2005, 2007; Wünsch et al. 2011, Breitschwerdt & Schmutzler 1994, 1999, we investigate how initially hot adiabatic galactic winds cool radiatively on large scales.”
• The faint end of the galaxy luminosity function (2002, background): “There could be local feedback effects (Dekel & Silk 1986; Efstathiou 2000) or cosmological effects like the reionization of the Universe inhibiting the collapse of gas into small halos (Klypin et al. 1999; Bullock, Kravtsov & Weinberg 2000, Tully et al. 2002).”
• Mass loss from dwarf spheroidal galaxies: the origins of shallow dark matter cores and exponential surface brightness profiles (2004, background): “…the current cosmological paradigm breaks down on small scales; or it could be a result of C© 2004 RAS Downloaded from https://academic.oup.com/mnras/article-abstract/356/1/107/1049772 by guest on 28 July 2018 a complex evolutionary history for the Local Group dwarfs due to some form of feedback.”
• Virial shocks in galactic haloes (2003, background): “Other semi-analytic models (Efstathiou 2000; White & Frenk 1991) also appeal to the slow gas infall rate as a mechanism that regulates the gas input into the disc.”