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Age-resolved chemistry of red giants in the solar neighbourhood

Feuillet, Diane LU ; Bovy, Jo ; Holtzman, Jon ; Weinberg, David H. ; Garcia-Hernandez, D A ; Hearty, Fred R. ; Majewski, Steven R ; Roman-Lopes, Alexandre ; Rybizki, Jan and Zamora, Olga (2018) In Monthly Notices of the Royal Astronomical Society 477(2). p.2326-2348
Abstract
In the age of high-resolution spectroscopic stellar surveys of the Milky Way, the number of stars with detailed abundances of multiple elements is rapidly increasing. These elemental abundances are directly influenced by the evolutionary history of the Galaxy, but this can be difficult to interpret without an absolute timeline of the abundance enrichment. We present age-abundance trends for [M/H], [α/M], and 17 individual elements using a sample of 721 solar neighbourhood Hipparcos red giant stars observed by Apache Point Observatory Galactic Evolution Experiment. These age trends are determined through a Bayesian hierarchical modelling method presented by Feuillet et al. We confirm that the [α/M]-age relation in the solar neighbourhood is... (More)
In the age of high-resolution spectroscopic stellar surveys of the Milky Way, the number of stars with detailed abundances of multiple elements is rapidly increasing. These elemental abundances are directly influenced by the evolutionary history of the Galaxy, but this can be difficult to interpret without an absolute timeline of the abundance enrichment. We present age-abundance trends for [M/H], [α/M], and 17 individual elements using a sample of 721 solar neighbourhood Hipparcos red giant stars observed by Apache Point Observatory Galactic Evolution Experiment. These age trends are determined through a Bayesian hierarchical modelling method presented by Feuillet et al. We confirm that the [α/M]-age relation in the solar neighbourhood is steep and relatively narrow (0.20 dex age dispersion), as are the [O/M]-age and [Mg/M]-age relations. The age trend of [C/N] is steep and smooth, consistent with stellar evolution. The [M/H]-age relation has a mean age dispersion of 0.28 dex and a complex overall structure. The oldest stars in our sample are those with the lowest and highest metallicities, while the youngest stars are those with solar metallicity. These results provide strong constraints on theoretical models of Galactic chemical evolution (GCE). We compare them to the predictions of one-zone GCE models and multizone mixtures, both analytic and numerical. These comparisons support the hypothesis that the solar neighbourhood is composed of stars born at a range of Galactocentric radii, and that the most metal-rich stars likely migrated from a region with earlier and more rapid star formation such as the inner Galaxy. (Less)
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author
publishing date
type
Contribution to journal
publication status
published
in
Monthly Notices of the Royal Astronomical Society
volume
477
issue
2
article number
10.1093/mnras/sty779
pages
26 pages
publisher
Oxford University Press
external identifiers
  • scopus:85047169252
ISSN
1365-2966
DOI
10.1093/mnras/sty779
language
English
LU publication?
no
id
dec7d069-deb7-490f-a719-be156986ef15
date added to LUP
2019-11-27 10:45:34
date last changed
2020-08-05 05:37:18
@article{dec7d069-deb7-490f-a719-be156986ef15,
  abstract     = {In the age of high-resolution spectroscopic stellar surveys of the Milky Way, the number of stars with detailed abundances of multiple elements is rapidly increasing. These elemental abundances are directly influenced by the evolutionary history of the Galaxy, but this can be difficult to interpret without an absolute timeline of the abundance enrichment. We present age-abundance trends for [M/H], [α/M], and 17 individual elements using a sample of 721 solar neighbourhood Hipparcos red giant stars observed by Apache Point Observatory Galactic Evolution Experiment. These age trends are determined through a Bayesian hierarchical modelling method presented by Feuillet et al. We confirm that the [α/M]-age relation in the solar neighbourhood is steep and relatively narrow (0.20 dex age dispersion), as are the [O/M]-age and [Mg/M]-age relations. The age trend of [C/N] is steep and smooth, consistent with stellar evolution. The [M/H]-age relation has a mean age dispersion of 0.28 dex and a complex overall structure. The oldest stars in our sample are those with the lowest and highest metallicities, while the youngest stars are those with solar metallicity. These results provide strong constraints on theoretical models of Galactic chemical evolution (GCE). We compare them to the predictions of one-zone GCE models and multizone mixtures, both analytic and numerical. These comparisons support the hypothesis that the solar neighbourhood is composed of stars born at a range of Galactocentric radii, and that the most metal-rich stars likely migrated from a region with earlier and more rapid star formation such as the inner Galaxy.},
  author       = {Feuillet, Diane and Bovy, Jo and Holtzman, Jon and Weinberg, David H. and Garcia-Hernandez, D A and Hearty, Fred R. and Majewski, Steven R and Roman-Lopes, Alexandre and Rybizki, Jan and Zamora, Olga},
  issn         = {1365-2966},
  language     = {eng},
  number       = {2},
  pages        = {2326--2348},
  publisher    = {Oxford University Press},
  series       = {Monthly Notices of the Royal Astronomical Society},
  title        = {Age-resolved chemistry of red giants in the solar neighbourhood},
  url          = {http://dx.doi.org/10.1093/mnras/sty779},
  doi          = {10.1093/mnras/sty779},
  volume       = {477},
  year         = {2018},
}