Galactic chemical evolution: abundance gradients of individual elements

By F. Matteucci, P. François. 1989

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Citations in the corpus

Yule-Simpson’s paradox in Galactic Archaeology (2019, background): “The negative metallicity gradient observed today suggests that the disk has formed inside out (Matteucci & Francois 1989).”
Measuring Radial Orbit Migration in the Galactic Disk (2018, methodology): “This is expected both from models of chemical evolution (Matteucci & Francois 1989) and from observations of the interstellar gas and young stars in galaxies (e.g., Przybilla et al. 2008).”
Mass-metallicity relation explored with CALIFA I. Is there a dependence on the star-formation rate? (2013, background): “…relation is explained as a simple effect of the inside-outmass/metallicity growth that dominates the secular evolution of late-type galaxies (e.g. Matteucci & Francois1989; Boissier & Prantzos 1999), combined with the fact that more massive regions form stars faster (i.e. at higher SFRs), thus…”
Specific Star Formation Rate Profiles in Nearby Spiral Galaxies: Quantifying the Inside-Out Formation of Disks (2006, unknown): “Moreover, the inside-out scenario of disk formation has been also proposed to explain the radial variation of the abundances of elements and colors in the disk of our own Milky Way (Matteucci & Francois 1989; Boissier & Prantzos 1999).”
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).”
Chemical abundance analysis of the open clusters Cr 110, NGC 2099 (M 37), NGC 2420, NGC 7789, and M 67 (NGC 2682) (2009, background): “Such a slope comes naturally in most Galactic chemical evolution mdels (Tosi, 1982, 1988; Matteucci & Francois, 1989; Tosi, 1996; Chiappini et al., 2001; Andrievsky et al., 2004; Colavitti eal., 2009; Magrini et al., 2009), when different star formation and infall rates are assumed for the inner…”
The Milky Way’s stellar disk (2013, methodology): “The chemical evolution of the Milky Way has been studied with a variety of approaches (e.g., Matteucci & Francois 1989; Gilmore et al. 1989; Chiappini et al. 2001) mostly with physically motivated but geometrically simplified models (not cosmological ab initio simulations): these studies have aimed…”
Λ Cold Dark Matter, Stellar Feedback, and the Galactic Halo Abundance Pattern (2005, background): “…1972; Talbot & Arnett 1973; Pagel & Patchett 1975; Hartwick 1976; Tinsley 1980; Twarog 1980; Matteucci & Greggio 1986; Matteucci & Tornambe 1987; Matteucci & Francois 1989; Wheeler et al. 1989; Ferrini et al. 1992; Timmes et al. 1995; Tsujimoto et al. 1995; Devriendt et al. 1999; Ferreras &…”
The HIPASS catalogue: ΩH i and environmental effects on the H i mass function of galaxies (2005, background): “…this is a simplified view of galaxy evolution because it is well established that gas accretionplays an important role in the total neutral gas budget of galaxies(e.g., Matteucci & Francois 1989), but it can go a long way in explaining our observed correlation between HIMF slope and density.”
Aperture Effects on Star Formation Rate, Metallicity, and Reddening (2005, background): “…between the spiral arms and the interarm regions (e.g. Guesten & Mezger 1982); (2) a star formation rate dependence on radius (Phillipps & Edmunds 1991); (3) radial infall of primordial gas during disk formation (Matteucci & François 1989; Pagel 1989; 7 z A ng ul ar s iz e [ ar cs ec ] Fig.”
Riding the Spiral Waves: Implications of Stellar Migration for the Properties of Galactic Disks (2008, background): “Models of galactic chemical evolution have been enormously successful in explaining the properties of stars in our solar neighborhood (Matteucci & Francois 1989; Carigi 1996; Chiappini et al. 1997; Boissier & Prantzos 1999).”
Metallicity and Nuclear Star Formation in Nearby Galaxy Pairs: Evidence for Tidally Induced Gas Flows (2005, background): “…by IMF differences between the spiral arms and the interarm regions (e.g. Guesten & Mezger 1982); (2) a star formation rate dependence on radius (Phillipps & Edmunds 1991); (3) radial infall of primordial gas during disk formation (Matteucci & Francois 1989; Pagel 1989; Edmunds & Greenhow 1995).”
Reconstructing the star formation history of the Milky Way disc(s) from chemical abundances (2014, background): “…form for the SFR at this stage because it is a simple function and closely mimics the most commonly occurring forms in the literature e.g. Matteucci & Francois (1989), Chiosi (1980), Chiappini et al. (1997), and Fenner et al. (2002) for a SFR based on the surface density of infalling gas…”
Confirming chemical clocks: asteroseismic age dissection of the Milky Way disc(s) (2017, methodology): “Viable formation scenarios for the Milky Way disc include inside–out and upside–down formation (e.g. Matteucci & Francois 1989; Brook et al. 2006; Bird et al. 2013; Ness et al. 2016; Schönrich & McMillan 2017), although there are suggestions that the old component of the disc formed outside–in…”
New constraints on the chemical evolution of the solar neighbourhood and galactic disc(s) - improved astrophysical parameters for the Geneva-Copenhagen Survey (2011, methodology): “While the MDF has been historically used to constrain the gas infall rate (e.g. Lynden-Bell 1975; Tinsley 1980; Matteucci & Francois 1989; Chiappini et al. 1997), the increasing broadening with age suggests that old stars are also a relevant ingredient in describing the wings of the MDF.”
Quantifying the uncertainties of chemical evolution studies II. Stellar yields (2010, background): “…Milky Way are assumed to form on a relatively short time-scale (about 1 Gyr) out of a first infall episode, whereas the thin disc forms insideout (Matteucci & François 1989) on longer time-scales (7 Gyr in the solar vicinity and more than a Hubble time at the outermost radii; see also Romano et…”
Estimating stellar birth radii and the time evolution of Milky Way’s ISM metallicity gradient (2018, background): “In a pioneering paper, Matteucci & Francois (1989) established that the observed negative Milky Way disk metallicity gradient results from an inside-out disk formation.”
The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars (2014, background): “…stars, that explode as Type II supernovae, and Type Ia supernovae dominate the chemical evolution of many elements and for this reason AGB stars were until recently largely ignored in models of chemical enrichment (Matteucci & Francois 1989; Timmes et al. 1995; Gibson 1997; Kobayashi et al. 2006).”