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Radial structure and formation of the Milky Way disc [PDF]
Astronomy & Astrophysics, 2021 Context. The formation of the Galactic disc is an enthusiastically debated issue. Numerous studies and models seek to identify the dominant physical process(es) that shaped its observed properties; for example, satellite accretion, starburst, quenching, gas infall, and stellar radial migration. Aims.
Katz, D. +4 more
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Constraining the formation of the Milky Way: Ages [PDF]
EPJ Web of Conferences, 2013 We present a new approach for studying the chemodynamical evolution of the Milky Way, which combines a thin disk chemical evolution model with the dynamics from N-body simulation of a galaxy with properties similar to those of our Galaxy. A cosmological re-simulation is used as a surrogate in order to extract ∼ 11 Gyrs of self-consistent dynamical ...
Cristina Chiappini +2 more
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Abundance Gradients and the Formation of the Milky Way [PDF]
The Astrophysical Journal, 2001 In this paper we adopt a chemical evolution model, which is an improved version of the Chiappini, Matteucci and Gratton (1997) model, assuming two main accretion episodes for the formation of the Galaxy. The present model takes into account in more detail than previously the halo density distribution and explores the effects of a threshold density in ...
Cristina Chiappini +3 more
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Star formation law in the Milky Way [PDF]
Publications of the Astronomical Society of Japan, 2017 Abstract The Schmidt law (SF law) in the Milky Way was investigated using 3D distribution maps of H ii regions and H i and molecular (H2) gases with spatial resolutions of ∼1 kpc in the Galactic plane and a few tens of pc in the vertical direction. H ii regions were shown to be distributed in a star-forming (SF) disk with nearly constant
Hiroyuki Nakanishi, Yoshiaki Sofue
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STAR FORMATION RELATIONS IN THE MILKY WAY [PDF]
The Astrophysical Journal, 2016 ABSTRACT The relations between star formation and properties of molecular clouds (MCs) are studied based on a sample of star-forming regions in the Galactic Plane. Sources were selected by having radio recombination lines to provide identification of associated MCs and dense clumps. Radio continuum emission and mid-infrared emission were
Nalin Vutisalchavakul +2 more
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Traces of the formation history of the Milky Way [PDF]
Proceedings of the International Astronomical Union, 2013 AbstractChemical and kinematical information is needed in order to understand and trace the formation history of our Galaxy. In the homogeneous large sample of F and G stars in the survey by Nordström et al. (2004), groups of stars with orbital parameters different from field stars were found by Helmi et al. (2006).
Nordström, Birgitta +3 more
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The Milky Way as a Star Formation Engine [PDF]
, 2014 The cycling of material from the interstellar medium (ISM) into stars and the return of stellar ejecta into the ISM is the engine that drives the "galactic ecology" in normal spirals, a cornerstone in the formation and evolution of galaxies through cosmic time.
Molinari, S. +10 more
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The formation of the Galactic bulge of the Milky Way [PDF]
EPJ Web of Conferences, 2012 We aim to determine if the bulge formed via mergers as predicted by Cold Dark Matter (CDM) theory, or from disk instabilities, as suggested by its boxy shape, or both processes. We are observing about 28,000 bulge stars in fields that span longitudes of − 31 to + 26° and latitudes of − 5° to − 10°, targeting mostly red clump giants and we are measuring
Kenneth C. Freeman, Melissa Ness
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Formation and Evolution of the Milky Way [PDF]
Symposium - International Astronomical Union, 1997 To paint with broad brush strokes, the spectrum of Galactic formation models has as extrema what may be termed the “fast and smooth” and the “slow and lumpy” scenarios. Appropriate or not, to ascribe as champions of these views the works of, respectively, Eggen et al.
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Clues to the formation of the Milky Way’s thick disk [PDF]
Astronomy & Astrophysics, 2015 7 pages, 6 figures, accepted for publication in A&A, replaced to include a correction on the color bar of figure 2 and ...
Haywood, M. +3 more
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