GCD+: a new chemodynamical approach to modelling supernovae and chemical enrichment in elliptical galaxies

By Daisuke Kawata, B. Gibson. 2002

191 citations recorded by the source corpus.

We have developed a new galactic chemo-dynamical evolution code, called GCD+, for studies of galaxy formation and evolution. This code is based on our original threedimensional tree N-body/smoothed particle hydrodynamics code which includes selfgravity, hydrodynamics, radiative cooling, star formation, supernova feedback, and metal enrichment. GCD+ includes a new Type II (SNe II) and Ia (SNe Ia) supernovae model taking into account the lifetime of progenitor stars, and chemical enrichment from intermediate mass stars. We apply GCD+ to simulations of elliptical galaxy formation, and examine the colour-magnitude relation (CMR), the Kormendy relation, and the [Mg/Fe]–magnitude relation of simulation end-products. GCD+ is a useful and unique tool which enables us to compare simulation results with the observational data directly and quantitatively. Our simulation confirm the results of Kawata (2001) who uses a simpler chemo-dynamical evolution code. We newly find that radiative cooling becomes more efficient and thus the gas infall rate increases,with decreasing mass of galaxies, which contributes to the slope of the CMR. In addition, the sophisticated treatments of both SNe II and SNe Ia in GCD+ show that feedback from SNe Ia plays a crucial role in the evolution of elliptical galaxies. We conclude that the feedback effect of SNe Ia should not be ignored in studying the evolution of elliptical galaxies.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/9161b7a42e96e1358b9080654f37b0ff5820bf14

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Citations in the corpus

Star formation and feedback in smoothed particle hydrodynamic simulations – I. Isolated galaxies (2006, methodology): “…GASOLINE (Wadsley et al. 2004), c© 0000 RAS we choose to follow a different method that is outlined in Katz (1992), one that uses a stochastic formulation for star formation (see also Kawata & Gibson (2003), the ’ordinary’ star formation in Springel & Hernquist (2003), and Okamoto et al. (2005)).”
Impacts of a flaring star-forming disc and stellar radial mixing on the vertical metallicity gradient (2016, methodology): “We use our original Tree N-body code, GCD+ (Kawata & Gibson 2003; Kawata et al. 2013) for the numerical experiments presented in this paper, and model the evolution of a barred disc galaxy similar in size to the Milky Way.”
Making Galaxies in a Cosmological Context: The Need for Early Stellar Feedback (2012, background): “The other is thermal feedback in which stars simply heat gas particles and allow the adiabatic work of the particles to push other gas out of the way (Gerritsen & Icke 1997; Thacker & Couchman 2000; Kawata & Gibson 2003; Stinson et al. 2006).”
On the relation between the Schmidt and Kennicutt-Schmidt star formation laws and its implications for numerical simulations (2007, background): “…Katz, Weinberg, & Hernquist 1996; Gnedin 1996; Gerritsen & Icke 1997; Yepes et al. 1997; Springel 2000; Thacker & Couchman 2000; Kay et al. 2002; Kawata & Gibson 2003; Kravtsov 2003; Springel & Hernquist 2003; Sommer-Larsen, Götz, & Portinari 2003; Marri & White 2003; Okamoto et al. 2003;…”
Chemodynamical evolution of the Milky Way disk - I. The solar vicinity (2012, background): “…including some treatment of chemical evolution have been performed by a number groups (Raiteri et al., 1996; Mosconi et al., 2001; Lia et al., 2002; Kawata and Gibson, 2003; Kobayashi, 2004; Scannapieco et al., 2005; Martı́nez-Serrano et al., 2008; Oppenheimer and Davé, 2008; Wiersma et al.,…”
Feedback and metal enrichment in cosmological smoothed particle hydrodynamics simulations ¿ I. A model for chemical enrichment (2005, background): “…in galaxy formation it is necessary to consider the full cosmological growth of structure in which mergers and interactions have important effects on the star formation process and the dynamical evolution of galaxies (see also Kawata & Gibson 2003; Tornatore et al. 2004; Okamoto et al. 2005).”
The Dynamical and Chemical Evolution of Dwarf Spheroidal Galaxies with GEAR (2009, background): “Kawata et al. (2006), following Kawata & Gibson (2003), combined kinetic and thermal feedbacks, which could generate galactic winds in elliptical galaxies.”
The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time (2016, methodology): “The energy injected from SN may be either thermal (e.g. Kawata & Gibson 2003; Stinson et al. 2006; Scannapieco et al. 2008; Keller C© 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society Downloaded from…”
THE METALLICITY EVOLUTION OF INTERACTING GALAXIES (2011, background): “…of mass and metals is transferred from a single stellar particle to a set of nearest SPH neighbors (e.g. Steinmetz & Mueller 1994; Kawata 2001; Kawata & Gibson 2003; Okamoto et al. 2005; Scannapieco et al. 2005; Stinson et al. 2006; Tornatore et al. 2007; Wiersma et al. 2009; Montuori et…”
Stellar populations of early-type galaxies in different environments - II. Ages and metallicities (2006, background): “However, other processes such as supernova feedback may play a role in regulating the rate at which stars form in these systems (e.g. Kawata & Gibson 2003).”
The transition from population III to population II-I star formation (2010, methodology): “This is consistent with any simulation including metal enrichment (Raiteri et al. 1996; Gnedin 1998; Mosconiet al. 2001; Lia et al. 2002a,b; Kawata & Gibson 2003; Kobayashi 2004; Ricotti & Ostriker 2004; Scannapieco et al. 2005; Tornatoreet al. 2007; Oppenheimer et al. 2009).”
Chemical signatures of formation processes in the stellar populations of simulated galaxies (2011, unknown): “…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).”
A model for cosmological simulations of galaxy formation physics: multi-epoch validation (2013, background): “…feedback (e.g., Dekel & Silk 1986; Navarro & White 1993; Mihos & Hernquist 1994; Gerritsen & Icke 1997; Thacker & Couchman 2000; Kay et al. 2002; Kawata & Gibson 2003; Sommer-Larsen et al. 2003; Springel & Hernquist 2003a; Brook et al. 2004; Oppenheimer & Davé 2006; Stinson et al. 2006; Dubois…”
Astrophysical smooth particle hydrodynamics (2009, background): “A large variety of chemical evolution approaches has been implemented into SPH, for a starting point one may want to consult (Steinmetz and Müeller, 1994, 1995; Raiteri et al., 1996; Carraro et al., 1998; Berczik, 1999; Kawata and Gibson, 2003; Kobayashi, 2004; Tornatore et al., 2004; Scannapieco et”
Simulations of Cosmic Chemical Enrichment (2006, background): “There are only a few studies that simulate the detailed chemical enrichment by both Type II and Ia supernovae (SNe II and SNe Ia) (Raiteri, Villata & Navarro 1996; Carraro, Lia & Chiosi 1998; Mosconi et al. 2001; Kawata & Gibson 2003; Nakasato & Nomoto 2003; Tornatore et al. 2004; K04).”
The Emergence of the Thick Disk in a Cold Dark Matter Universe (2004, background): “Details of GCD+ can be found in Kawata & Gibson (2003).”
Effects of feedback on the morphology of galaxy discs (2005, unknown): “In particular, Kawata & Gibson (2003) have argued that the non-instantaneous nature of SNe II and SNe Ia is important for the dynamical evolution of galaxies.”