CHEMODYNAMICAL SIMULATIONS OF THE MILKY WAY GALAXY

By C. Kobayashi, N. Nakasato. Proceedings of the International Astronomical Union, 2008

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We present chemodynamical simulations of a Milky-Way-type galaxy using a self-consistent hydrodynamical code that includes supernova feedback and chemical enrichment, and predict the spatial distribution of elements from oxygen to zinc. In the simulated galaxy, the kinematical and chemical properties of the bulge, disk, and halo are consistent with the observations. The bulge formed from the assembly of subgalaxies at z ≳ 3, and has higher [α/Fe] ratios because of the small contribution from Type Ia supernovae. The disk formed with a constant star formation over 13 Gyr, and shows a decreasing trend of [α/Fe] and increasing trends of [(Na,Al,Cu,Mn)/Fe] against [Fe/H]. However, the thick disk stars tend to have higher [α/Fe] and lower [Mn/Fe] than thin disk stars. We also predict the frequency distribution of elemental abundance ratios as functions of time and location, which can be directly compared with galactic archeology projects such as HERMES.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/e5743807de15a026eacf85916bd8c73693f6b0b3

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STELLAR ABUNDANCES IN THE SOLAR NEIGHBORHOOD: THE HYPATIA CATALOG (2014, background): “…shown by the blue and black trend lines, is classic α-element, starting from core-collapse supernovae depositing large amounts of oxygen but no iron and later on SN Ia injecting significant amounts of iron but no oxygen (Gratton & Ortolani 1986; Marcolini et al. 2009; Kobayashi & Nakasato 2011).”
The Aquila comparison project: the effects of feedback and numerical methods on simulations of galaxy formation (2011, background): “The lifetimes span a range of 0.1–20 Gyr as a function of progenitor metallicity, which is consistent with the observed SN rates and with the observed [α/Fe] relations in the Milky Way Galaxy.”
Using chemical tagging to redefine the interface of the Galactic disc and halo (2015, background): “Thus, given the results of Kobayashi & Nakasato (2011), one would expect the thin disk to have a higher [Mn/Fe] ratio than the thick disk.”
Nucleosynthesis in Stars and the Chemical Enrichment of Galaxies (2013, methodology): “As noted above, however, AGB stars can also contribute to N production even at [Fe/H] −2.5 in chemodynamical simulations (Kobayashi & Nakasato 2011).”
OXYGEN ABUNDANCES IN NEARBY FGK STARS AND THE GALACTIC CHEMICAL EVOLUTION OF THE LOCAL DISK AND HALO (2013, background): “Admittedly, some cosmological simulations (e.g., Kobayashi & Nakasato 2011) can probably reproduce the observational properties of the solar neighborhood equally well.”
The Horizon-AGN simulation: evolution of galaxy properties over cosmic time (2016, background): “Thus, stellar feedback should be modelled more realistically by taking into account stellar winds and both Type II and Type Ia supernovae (SNe; e.g. Kobayashi & Nakasato 2011; Hopkins et al. 2012).”
CHEMICAL CARTOGRAPHY WITH APOGEE: METALLICITY DISTRIBUTION FUNCTIONS AND THE CHEMICAL STRUCTURE OF THE MILKY WAY DISK (2015, methodology): “Several simulations and models find that “inside-out” (e.g., Larson 1976; Kobayashi & Nakasato 2011) and “upside-down” (e.g., Bournaud et al. 2009; Bird et al. 2013) formation of the Galactic disk reproduces observed trends in the Galaxy, such as the radial gradient and the lower vertical scale…”
Thin disc, thick disc and halo in a simulated galaxy (2012, methodology): “…simulations that have analysed the origins of stellar components have had overly massive spheroids (e.g. Abadi et al. 2003; Zolotov et al. 2009; Kobayashi & Nakasato 2011; Tissera et al. 2011) (from the accretion of an excess of stars) and suffered from an inability to match the empirical…”
ARGOS - III. Stellar populations in the Galactic bulge of the Milky Way (2012, methodology): “In Cold Dark Matter (ΛCDM) simulations of Galaxy formation (e.g. Abadi et al. 2003; Kobayashi & Nakasato 2011), bulges are built up primarily through hierarchical mergers.”
Impacts of a flaring star-forming disc and stellar radial mixing on the vertical metallicity gradient (2016, background): “…vertical metallicity gradient for the thin disc population is not well studied (for studies for the combined populations of thin and thick discs, see e.g. Kobayashi & Nakasato 2011; Loebman et al. 2011; Pilkington et al. 2012; Roškar et al. 2013; Miranda et al. 2016; Schönrich & McMillan 2016).”
Gaseous Galaxy Halos (2012, unknown): “The current chemical evolution models of our Galaxy are largely semi-analytic (although see Few et al., 2012; Kobayashi & Nakasato, 2011).”
Metallicity gradients in disks - Do galaxies form inside-out? (2012, methodology): “KN11 corresponds to the so-called ‘Wider Region’ model described by Kobayashi & Nakasato (2011), realized used a hybrid grape-SPH code.”
CARBON-ENHANCED METAL-POOR STAR FREQUENCIES IN THE GALAXY: CORRECTIONS FOR THE EFFECT OF EVOLUTIONARY STATUS ON CARBON ABUNDANCES (2014, background): “These frequencies, in turn, provide important constraints on Galactic chemical evolution (e.g., Kobayashi & Nakasato 2011) and population synthesis models (e.g., Pols et al. 2012), on the initial mass function (IMF; e.g., Lee et al. 2014), and on the chemical compositions of progenitor stellar…”
The SINS/zC-SINF Survey of z ∼ 2 Galaxy Kinematics: SINFONI Adaptive Optics–assisted Data and Kiloparsec-scale Emission-line Properties (2018, result): “…2006, 2010; Rupke et al. 2010; Rich et al. 2012), and in line with predictions from theoretical models and simulations (e.g., Rahimi et al. 2011; Kobayashi & Nakasato 2011; Few et al. 2012; Pilkington et al. 2012; Torrey et al. 2012; Gibson et al. 2013; Mott et al. 2013), these findings have…”