The chemical evolution of the galaxy

By F. Matteucci. 2003

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View Paper: https://www.semanticscholar.org/paper/f655a24367fc46e6cc6df5e4e1ff817b2266efc3

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In Astronomy and Astrophysics

Citations in the corpus

Oxygen abundances in nearby stars - Clues to the formation and evolution of the Galactic disk (2007, unknown): “Simple homogeneous Galactic Chemical Evolution (GCE) models have been described in detail by, e.g., Tinsley (1980), Clayton (1984), Rana (1991), Pagel (1997), and Matteucci (2001).”
Observational Clues to the Progenitors of Type Ia Supernovae (2013, background): “As a consequence, the distribution of [α/Fe] (typically [O/Fe] vs. [Fe/H]) is sensitive to the DTD (De Donder & Vanbeveren 2004, Matteucci 2001, Matteucci & Greggio 1986, Tinsley 1979).”
First results from the IllustrisTNG simulations: a tale of two elements - chemical evolution of magnesium and europium (2017, background): “…and chromium are created over longer timescales in Type Ia supernovae (SNIa), whereas s-process neutron capture elements (e.g. strontium and barium) probe their proposed injection sites – intermediate and low-mass asymptotic giant branch stars (AGB; e.g. Tinsley 1980; Pagel 1997; Matteucci 2001).”
Galactic Chemical Evolution: Carbon through Zinc (2006, background): “Elemental abundance ratios are the treasure house of information on star formation and galaxy formation because different types of supernovae produce different heavy elements with different timescales (e.g., Tinsley 1980; Pagel 1997; Matteucci 2001).”
Chemodynamics of the Milky Way - I. The first year of APOGEE data (2013, unknown): “Another possibility is to use planetary nebulae as tracers of chemical evolution (Maciel & Chiappini 1994; Maciel & Köppen 1994), although their ages and even their abundances are still subject to considerable uncertainties (Stasińska 2010).”
Nucleosynthesis yields of core-collapse supernovae and hypernovae, and galactic chemical evolution (2006, background): “These parameter can be determined uniquely from the metallicity distribution function and the [O/Fe]-[Fe/H] evolutionary trend at [Fe/H] ∼ > −1 (87; 63).”
Evolution of interstellar dust and stardust in the solar neighbourhood (2007, methodology): “Several scenarios for gas accretion have been proposed by different authors, suggesting di fferent rates and sequences of formation of the galactic components, see Matteucci (2003) for details. Models assuming an exponentially decreasing infall of the gas are most successful in reproducing the G-dwa”
The Apache Point Observatory Galactic Evolution Experiment (APOGEE) (2007, unknown): “…of H-band-accessible elements offers a number of potentially interesting insights into various aspects of Galactic chemical evolution (see, e.g., Matteucci 2001 and the recent review of nucleosynthesis and chemical evolution by Nomoto et al. 2013): • C, N: Important elements produced in…”
The evolution of the Milky Way from its earliest phases: Constraints on stellar nucleosynthesis (2004, background): “Moreover, from the study of the [el/Fe] versus [Fe/H] relations one can infer very important constraints on stellar nucleosynthesis calculations, stellar lifetimes and the star formation history in galaxies (see Matteucci, 2001).”
The evolution of isotope ratios in the Milky Way Galaxy (2011, background): “Kobayashi et al. (2006) presented the nucleosynthesis yields of SNe II and HNe as a function of the progenitor mass (M = 13, 15, 18, 20, 25, 30, and 40M⊙) and metallicity (Z = 0, 0.”