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The Chemical Evolution of the Milky Way Disk
Space Science Reviews, 1997Abstract The chemical evolution of the disk of our Galaxy is studied with numerical models assuming infall and a radially varying star formation rate (SFR). We propose a model with a minimal set of physically plausible assumptions which satisfies the main observational constraints of the disk, including those of the solar neighborhood.
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The Milky Way disk non‐axisymmetries and galactoseismology
Astronomische Nachrichten, 2016AbstractCurrent Galactic dynamical models still most often rely on the assumptions of a smooth time‐independent and axisymmetric gravitational potential. On the other hand, ab initio simulations in a cosmological context are not very flexible to precisely produce a model of our own Galaxy, or to disentangle the internal and the external/environmental ...
Famaey, Benoit +2 more
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EVOLUTION OF THE MILKY WAY DISK
2006The Solar neighbourhood is where the physical basis for models of the evolu- tion of spiral galaxy disks can be tested most stringently. A new survey has provided full space motions, metallicities, ages, and duplicity information for over 14,000 nearby F and G dwarfs.
Nordström, Birgitta, Andersen, Johannes
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The Evolution of the Milky Way Disk
2000The Milky Way is a heterogeneous system, with at least three components (halo, bulge, disk) having very different chemical, photometric and kinematical properties. A reliable model for the evolution of the Milky Way accounting for those properties does not exist at present.
N. Prantzos, S. Boissier
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Chemical evolution in the Milky Way Disk
AIP Conference Proceedings, 2006Classical models of galactic evolution predict a smooth rise in heavy‐element abundance (metallicity) with time. We test this prediction with a new, large and unbiased sample of long‐lived stars in the solar neighbourhood and find that several of the key tests fail to support the classical predictions.
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Chemo-Spectral Evolution of the Milky way and of Spiral Disks
Astrophysics and Space Science, 1999Our model and its application to the Milky Way are discussed in detail in Boissier & Prantzos (1998). The stellar yields of Woosley & Weaver (1995) are used to compute the chemical evolution, while the spectral one is coherently followed with the stellar evolution tracks of the Geneva group (Schaller et al. (1992), Charbonnel et al.
Samuel Boissier, Nikos Prantzos
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Identification of an [α/Fe]—Enhanced Thick Disk Component in an Edge-on Milky Way Analog
Astrophysical Journal Letters, 2021Nicholas Scott +2 more
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Modeling of Spiral Structure in a Multi-Component Milky Way-Like Galaxy
Galaxies, 2021Sergey S Khrapov +2 more
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Elemental abundances in the Milky Way stellar disk(s), bulge, and halo
New Astronomy Reviews, 2013Sofia Feltzing, Masashi Chiba
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