Simulations of Cosmic Chemical Enrichment

By C. Kobayashi, Volker Springel, Simon D. M. White. Proceedings of the International Astronomical Union, 2006

162 citations recorded by the source corpus.

Abstract We simulate cosmic chemical enrichment with a hydrodynamical model including supernova and hypernova feedback. We find that the majority of stars in present-day massive galaxies formed in much smaller galaxies at high redshifts, despite their late assembly times. The hypernova feedback drives galactic outflows efficiently in low mass galaxies, and these winds eject heavy elements into the intergalactic medium. The ejected baryon fraction is larger for less massive galaxies, correlates well with stellar metallicity. The observed mass-metallicity relation is well reproduced as a result of the mass-dependent galactic winds.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/1bdd1c7194758e8e676dff52599b1f5fe5014058

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Citations in the corpus

Metallicity evolution, metallicity gradients, and gas fractions at z ~ 3.4 (2013, background): “…although effects associated with the IMF, downsizing and gas infalls have also been invoked and several thorough theoretical models have been proposed (Köppen et al. 2007; Kobayashi et al. 2007; Brooks et al. 2007; De Rossi et al. 2007; Cescutti et Article number, page 1 of 32 ar X iv :1 31 1.”
A fundamental relation between mass, SFR and metallicity in local and high redshift galaxies (2010, background): “C O ] 2 man 1996; Garnett 2002; Tremonti et al. 2004; Kobayashi et al. 2007; Scannapieco et al. 2008; Spitoni et al. 2010), “downsizing”, i.e., a systematic dependence of the efficiency of star formation with galaxy mass (e.g., Brooks et al. 2007; Mouchine et al. 2008; Calura et al. 2009),…”
Mass, metal, and energy feedback in cosmological simulations (2007, background): “…into a number of surrounding gas particles in a Smoothed Particle Hydrodynamic (SPH) simulation, and find that hypernovae with 10× the typical supernova energy are needed to enrich the IGM to observed levels while matching the stellar baryonic content of the local Universe (Kobayashi et al. 2007).”
Galaxy formation theory (2010, background): “Numerous hydrodynamical simulation codes now contain implementations of chemical enrichment (Scannapiecoet al. 2005; Kobayashi et al. 2007; Pontzen et al. 2008; Gnedin et al. 2009).”
The physics of the intergalactic medium (2007, background): “Exam- 57 ples of recent wind simulations include Theuns et al. (2002b), Aguirre et al. (2005), Cen et al. (2005), Cen and Ostriker (2006), Oppenheimer and Davé (2006), Kobayashi et al. (2007), and Kawata and Rauch (2007).”
The Aquila comparison project: the effects of feedback and numerical methods on simulations of galaxy formation (2011, methodology): “The large scatter leads us to conclude that caution must be exercised when analysing the instantaneous 6 http://www.mpa-garching.mpg.de/SDSS/DR7/ SFRs of simulated galaxies, since these depend sensitively on the details of accretion and of the implemented subgrid physics.”
CHEMODYNAMICAL SIMULATIONS OF THE MILKY WAY GALAXY (2008, background): ““Feedback” is also important for solving the angular momentum problem and the missing satellite problem, and for explaining the existence of heavy elements in the intracluster and intergalactic medium, and possibly the mass-metallicity relation of galaxies (Kobayashi et al. 2007).”
The origin of the galaxy mass-metallicity relation and implications for galactic outflows (2007, background): “In fact, the tendency of gas-phase metallicities to track an equilibrium value combined with a tendency for η̃MLF to decline and Zg,eq to grow as galaxies grow requires that the fraction of metals retained and the mean stellar metallicity must grow together, as found by Kobayashi et al. (2007).”
Chemical signatures of formation processes in the stellar populations of simulated galaxies (2011, background): “…of treatments of chemical evolution have been implemented in the cosmological hydrodynamics codes used to simulate galaxy formation (e.g. Raiteri et al. 1996; Mosconi et al. 2001; Lia et al. 2002; Kawata & Gibson 2003; Kobayashi et al. 2007; Wiersma et al. 2009; Mart́ınez-Serrano et al. 2008).”
THEORETICAL EVOLUTION OF OPTICAL STRONG LINES ACROSS COSMIC TIME (2013, background): “…the mean metallicity of galaxies rises with cosmic time as galaxies undergo successive generations of star formation (e.g., Nagamine et al. 2001; De Lucia et al. 2004; Kobulnicky & Kewley 2004; Kobayashi et al. 2007; Maiolino et al. 2008; Davé et al. 2011a; Yuan et al. 2012; Zahid et al. 2012).”
Chemical enrichment in cosmological, smoothed particle hydrodynamics simulations (2009, methodology): “2008 for a review), but in recent years chemodynamical cosmological simulations have also become more common (e.g. Mosconi et al. 2001; Scannapieco et al. 2005; Kobayashi et al. 2007; Oppenheimer & Davé 2008).”
NEW STRONG-LINE ABUNDANCE DIAGNOSTICS FOR H ii REGIONS: EFFECTS OF κ-DISTRIBUTED ELECTRON ENERGIES AND NEW ATOMIC DATA (2013, background): “These emission lines enable us to investigate the metallicity evolution of the universe as a whole (Nagamine et al. 2001; De Lucia et al. 2004; Kobayashi et al. 2007; Yuan et al. 2013).”
Chemodynamical evolution of the Milky Way disk - I. The solar vicinity (2012, background): “However, although the results are encouraging and globally observed trends seem to be reproduced, such as the mass-metallicity relation (e.g., Kobayashi et al., 2007) or the metallicity trends between the different Galactic components (e.g., Tissera et al., 2012), it is still a challenge for these…”
Characterizing Supernova Progenitors via the Metallicities of their Host Galaxies, from Poor Dwarfs to Rich Spirals (2007, background): “This would have implications for modeling and understanding of galactic chemical evolution, which include the effects of white dwarf winds to shut down SNe Ia at low metallicities (e.g., Kobayashi et al. 2007).”