A simple model for the evolution of disc galaxies: the Milky Way

By T. Naab, Jeremiah P. Ostriker. 2005

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A simple model for the evolution of disc galaxies is presented. We adopt three numbers from observations of the Milky Way disc, � d the local surface mass density, r d the stellar scalelength (of the assumed exponential disc), v c, the amplitude of the (assumed flat) rotation curve, and physically, the (local) dynamical Kennicutt star formation prescription, standard chemical evolution equations assuming a Salpeter initial mass function and a model for spectral evolution of stellar populations. We can determine the detailed evolution of the model with only the addition of standard cosmological scalings with the time of the dimensional parameters. A surprising wealth of detailed specifications follows from this prescription including the gaseous infall rate as a function of radius and time, the distribution of stellar ages and metallicities with time and radius, surface brightness profiles at different wavelengths, colours, etc. Some of the detailed properties are as follows: the global gas infall rate and the global star formation rate ,

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/9301d3805d803cfe4804374831fa95cd8ba93f42

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Citations in the corpus

The influence of gas on the structure of merger remnants (2006, unknown): “Analytical models of disc formation (e.g. Naab & Ostriker 2006) which contain all the information about stellar ages and metallicitites of the progenitor discs and semi-analytical modeling (Khochfar & Burkert 2005; Khochfar & Silk 2006) in combination with detailed merger simulations (Naab et al.…”
Neutral hydrogen in nearby elliptical and lenticular galaxies: the continuing formation of early-type galaxies (2006, background): “Also in spiral galaxies, ga accretion events are found to be very common over their lifetim (Naab & Ostriker 2006, van der Hulst & Sancisi 2004).”
Physical Processes in the Interstellar Medium (2014, methodology): “Our Galaxy forms new stars at a rate of ṀSF ∼ 2−4M yr−1 (e.g. Naab & Ostriker, 2006; Adams et al., 2013).”
The Cold Gaseous Halo of NGC 891 (2007, background): “Such accretion may be necessary to explain the evolution of disk galaxies (Naab & Ostriker 2006).”
Kinematics and history of the solar neighbourhood revisited (2009, background): “The study of Galactic evolution in a cosmological context by Hernandez, Avila-Reese & Firmani (2001) yields τmax = 11 Gyr, while that of Naab & Ostriker (2006) yields τmax ∼ 10 Gyr, our lower limit.”
Thin, thick and dark discs in ΛCDM (2008, methodology): “Models for the Milky Way suggest that stars have continued to form at a constant rate since z = 1, yet the surface density of gas likely remained constant with time due to fresh gas inflow (Rocha-Pinto et al. 2000; Naab & Ostriker 2006; Just & Jahreiss 2007).”
How do minor mergers promote inside-out growth of ellipticals, transforming the size, density profile and dark matter fraction? (2012, background): “This growth process is distinctively different from the star formation driven inside-out growth of disk galaxies (Prantzos & Aubert 1995; Matteucci & Francois 1989; Mo et al. 1998; Naab & Ostriker 2006; Governato et al. 2007; Wang et al. 2011; Kauffmann et al. 2012).”
The Gaia-ESO Survey : radial metallicity gradients and age-metallicity relation of stars in the Milky Way disk (2014, background): “…of the formation and evolution of the Milky Way (e.g. Burkert et al. 1992; Pagel & Tautvaisiene 1995; Velazquez & White 1999; Hou et al. 2000; Chiappini et al. 2001; Brook et al. 2004, 2005; Naab & Ostriker 2006; Schönrich & Binney 2009b; Kubryk et al. 2013; Minchev et al. 2013; Rix & Bovy 2013).”
Chemical evolution with radial mixing (2008, background): “…assumed that a galaxy such as the Milky Way can be divided into concentric cylindrical annuli, each of which evolves independently of the others (e.g. Pagel 1997; Chiappini, Matteucci & Gratton 1997; Chiappini, Matteucci & Romano 2001; Naab & Ostriker 2006; Colavitti, Matteucci & Murante 2008).”
Reconstructing the star formation history of the Milky Way disc(s) from chemical abundances (2014, methodology): “For instance, there is no explicit thick disc phase in the models of Fenner & Gibson (2003) or Naab & Ostriker (2006).”
Galactic star formation and accretion histories from matching galaxies to dark matter haloes (2012, result): “This in accord with standard formation and enrichment scenarios for disk galaxies (Matteucci & Francois 1989; Mo et al. 1998; Prantzos & Silk 1998; Naab & Ostriker 2006; Kauffmann et al. 2012).”
Determination of the Local Dark Matter Density in our Galaxy (2009, methodology): “The rotation curve can be flattened, e.g. by decreasing the distance between the Sun and the GC, but then r⊙ ≈ 7 kpc is needed (Honma and Sofue 1997), which is clearly outside the present errors given in Eq.”
The evolution of the Galactic metallicity gradient from high-resolution spectroscopy of open clusters (2008, methodology): “…over 22 kpc radii, consistent with the recent estimate ∼5 M yr−1 by de Boer (2004), and favoured by recent models of disk galaxy evolution (e.g., Naab & Ostriker 2006); (ii) the predicted current star formation rate is ∼3 M yr−1 integrated over 22 kpc radii, to be compared with the…”
Accretion-driven turbulence as universal process: galaxies, molecular clouds, and protostellar disks (2009, background): “Its gas mass out to 25 kpc is ∼9×109 M (Naab & Ostriker 2006; Xue et al. 2008).”