Fluorine Abundances in the Galactic Disk
(2019) In Astrophysical Journal 885(2).- Abstract
The chemical evolution of fluorine is investigated in a sample of Milky Way red giant stars that span a significant range in metallicity from [Fe/H] ∼-1.3 to 0.0 dex. Fluorine abundances are derived from vibration-rotation lines of HF in high-resolution infrared spectra near 2.335 μm. The red giants are members of the thin and thick disk/halo, with two stars being likely members of the outer disk Monoceros overdensity. At lower metallicities, with [Fe/H] <-0.4 to-0.5, the abundance of F varies as a primary element with respect to the Fe abundance, with a constant subsolar value of [F/Fe] ∼-0.3 to-0.4 dex. At larger metallicities, however, [F/Fe] increases rapidly with [Fe/H] and displays a near-secondary behavior with respect to Fe.... (More)
The chemical evolution of fluorine is investigated in a sample of Milky Way red giant stars that span a significant range in metallicity from [Fe/H] ∼-1.3 to 0.0 dex. Fluorine abundances are derived from vibration-rotation lines of HF in high-resolution infrared spectra near 2.335 μm. The red giants are members of the thin and thick disk/halo, with two stars being likely members of the outer disk Monoceros overdensity. At lower metallicities, with [Fe/H] <-0.4 to-0.5, the abundance of F varies as a primary element with respect to the Fe abundance, with a constant subsolar value of [F/Fe] ∼-0.3 to-0.4 dex. At larger metallicities, however, [F/Fe] increases rapidly with [Fe/H] and displays a near-secondary behavior with respect to Fe. Comparisons with various models of chemical evolution suggest that in the low-metallicity regime (dominated here by thick-disk stars), a primary evolution of 19F with Fe, with a subsolar [F/Fe] value that roughly matches the observed plateau, can be reproduced by a model incorporating neutrino nucleosynthesis in the aftermath of the core collapse in Type II supernovae. A primary behavior for [F/Fe] at low metallicity is also observed for a model including rapidly rotating low-metallicity massive stars, but this overproduces [F/Fe] at low metallicity. The thick-disk red giants in our sample span a large range of galactocentric distance (R g ∼ 6-13.7 kpc) yet display a roughly constant value of [F/Fe], indicating a very flat gradient (with a slope of 0.02 ± 0.03 dex kpc-1) of this elemental ratio over a significant portion of the Galaxy having
(Less)
- author
- Guerço, Rafael ; Cunha, Katia ; Smith, Verne V. ; Hayes, Christian R. ; Abia, Carlos ; Lambert, David L. ; Jönsson, Henrik LU and Ryde, Nils LU
- organization
- publishing date
- 2019
- type
- Contribution to journal
- publication status
- published
- subject
- in
- Astrophysical Journal
- volume
- 885
- issue
- 2
- article number
- 139
- publisher
- American Astronomical Society
- external identifiers
-
- scopus:85075325439
- ISSN
- 0004-637X
- DOI
- 10.3847/1538-4357/ab45f1
- language
- English
- LU publication?
- yes
- id
- fe10ccd6-c3ce-4770-9db8-7d94fe2588c1
- date added to LUP
- 2019-12-05 09:37:21
- date last changed
- 2024-04-17 00:45:29
@article{fe10ccd6-c3ce-4770-9db8-7d94fe2588c1, abstract = {{<p>The chemical evolution of fluorine is investigated in a sample of Milky Way red giant stars that span a significant range in metallicity from [Fe/H] ∼-1.3 to 0.0 dex. Fluorine abundances are derived from vibration-rotation lines of HF in high-resolution infrared spectra near 2.335 μm. The red giants are members of the thin and thick disk/halo, with two stars being likely members of the outer disk Monoceros overdensity. At lower metallicities, with [Fe/H] <-0.4 to-0.5, the abundance of F varies as a primary element with respect to the Fe abundance, with a constant subsolar value of [F/Fe] ∼-0.3 to-0.4 dex. At larger metallicities, however, [F/Fe] increases rapidly with [Fe/H] and displays a near-secondary behavior with respect to Fe. Comparisons with various models of chemical evolution suggest that in the low-metallicity regime (dominated here by thick-disk stars), a primary evolution of <sup>19</sup>F with Fe, with a subsolar [F/Fe] value that roughly matches the observed plateau, can be reproduced by a model incorporating neutrino nucleosynthesis in the aftermath of the core collapse in Type II supernovae. A primary behavior for [F/Fe] at low metallicity is also observed for a model including rapidly rotating low-metallicity massive stars, but this overproduces [F/Fe] at low metallicity. The thick-disk red giants in our sample span a large range of galactocentric distance (R <sub>g</sub> ∼ 6-13.7 kpc) yet display a roughly constant value of [F/Fe], indicating a very flat gradient (with a slope of 0.02 ± 0.03 dex kpc<sup>-1</sup>) of this elemental ratio over a significant portion of the Galaxy having</p>}}, author = {{Guerço, Rafael and Cunha, Katia and Smith, Verne V. and Hayes, Christian R. and Abia, Carlos and Lambert, David L. and Jönsson, Henrik and Ryde, Nils}}, issn = {{0004-637X}}, language = {{eng}}, number = {{2}}, publisher = {{American Astronomical Society}}, series = {{Astrophysical Journal}}, title = {{Fluorine Abundances in the Galactic Disk}}, url = {{http://dx.doi.org/10.3847/1538-4357/ab45f1}}, doi = {{10.3847/1538-4357/ab45f1}}, volume = {{885}}, year = {{2019}}, }