The Abundance of Fluorine in Normal G and K Stars of the Galactic Thin Disk

Pilachowski, Catherine A.; Pace, C.

doi:10.1088/0004-6256/150/3/66

Cited by 25 publications

(35 citation statements)

References 71 publications

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“…1. Observational data of Jönsson et al (2017a) are indicated with cyan circles whereas the data taken by Pilachowski & Pace (2015) are presented with gray pentagons.…”

Section: Results: Testing Different Nucleosynthesis Prescriptions Formentioning

confidence: 99%

Fluorine in the solar neighborhood: Chemical evolution models

Spitoni

Matteuccí

Jönsson

et al. 2018

A&A

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Context. In the light of the new observational data related to fluorine abundances in the solar neighborhood stars, we present here chemical evolution models testing different fluorine nucleosynthesis prescriptions with the aim to best fit those new data. Aims. We consider chemical evolution models in the solar neighborhood testing different nucleosynthesis prescriptions for fluorine production with the aim of reproducing the observed abundance ratios [F/O] [Fe/H]. We study in detail the effects of different stellar yields on the fluorine production. Methods. The adopted chemical evolution models are: i) the classical "two-infall" model which follows the chemical evolution of halo-thick disk and thin disk phases, ii) and the " one-infall" model designed only for the thin disk evolution. We tested the effects on the predicted fluorine abundance ratios of different nucleosynthesis yield sources: AGB stars, Wolf-Rayet stars, Type II and Type Ia supernovae, and novae. Results. The fluorine production is dominated by AGB stars but the Wolf-Rayet stars are required to reproduce the trend of the observed data in the solar neighborhood by Jönsson et al. (2017a) with our chemical evolution models. In particular, the best model both for the "two-infall" and "one-infall" cases requires an increase by a factor of two of the Wolf-Rayet yields given by Meynet & Arnould (2000). We also show that the novae, even if their yields are still uncertain, could help to better reproduce the secondary behavior of

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“…1. Observational data of Jönsson et al (2017a) are indicated with cyan circles whereas the data taken by Pilachowski & Pace (2015) are presented with gray pentagons.…”

Section: Results: Testing Different Nucleosynthesis Prescriptions Formentioning

confidence: 99%

Fluorine in the solar neighborhood: Chemical evolution models

Spitoni

Matteuccí

Jönsson

et al. 2018

A&A

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“…It should, however, be kept in mind that the solar F-abundance determinations are subjected to large uncertainties (of the order of ±0.25 dex; Hall & Noyes 1969;Grevesse et al 2007;Maiorca et al 2014), and that we are using the meteoric value of Lodders (2003). The choice of the value of the solar Our abundances show less scatter in the trends than many previous investigations (see, e.g, Recio-Blanco et al 2012;Pilachowski & Pace 2015;Jönsson et al 2017b). For the narrow metallicity range of the open cluster giants in Nault & Pilachowski (2013), our results agree very well, with a clear increase at super-solar values, see Figure 4.…”

Section: Fluorine Abundances and Ratios Versus Metallicitymentioning

confidence: 92%

“…The field of observationally investigating the chemical evolution of fluorine has grown in recent years due to the advent of sensitive, high resolution spectrometers recording light in the infrared; for example, Recio-Blanco et al (2012); Jönsson et al (2014b) used CRIRES at the Very Large Telescope and Pilachowski & Pace (2015); Jönsson et al (2017b); Guerço et al (2019a,b) used the Phoenix spectrometer to measure fluorine abundances in K-band spectra. Guerço et al (2019a) also used iSHELL at the NASA Infrared Telescope Facility (IRTF).…”

Section: Introductionmentioning

confidence: 99%

Fluorine in the Solar Neighborhood: The Need for Several Cosmic Sources

Ryde

Jönsson

Mace

et al. 2020

ApJ

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The cosmic origin of fluorine is still not well constrained. Several nucleosynthetic channels at different phases of stellar evolution have been suggested, but these must be constrained by observations. For this, the fluorine abundance trend with metallicity spanning a wide range is required. Our aim is to determine stellar abundances of fluorine for −1.1 < [Fe/H] < +0.4. We determine the abundances from HF lines in infrared K-band spectra (∼ 2.3 µm) of cool giants, observed with the IGRINS and Phoenix high-resolution spectrographs. We derive accurate stellar parameters for all our observed K giants, which is important since the HF lines are very temperature sensitive. We find that [F/Fe] is flat as a function of metallicity at [F/Fe]∼ 0, but increases as the metallicity increases. The fluorine slope shows a clear secondary behavior in this metallicity range. We also find that the [F/Ce] ratio is relatively flat for −0.6 < [Fe/H] < 0, and that for two metal-poor ([Fe/H] < −0.8), s-process element enhanced giants, we do not detect an elevated fluorine abundance. We interpret all these observational constraints to indicate that several major processes are at play for the cosmic budget of fluorine over time; from those in massive stars at low metallicities, through the asymptotic giant branch-star contribution at −0.6 < [Fe/H] < 0, to processes with increasing yields with metallicity at super-solar metallicities. The origins of the latter, and whether or not Wolf-Rayet stars and/or novae could contribute at super-solar metallicities, is currently not known. To quantify these observational results, theoretical modelling is required. More observations in the metal-poor region are required to clarify the processes there.

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“…Alternatively, this abundance pattern could be representative of the outer thin disk, if Monoceros is a structure of the flared thin disk. Figure 10 is similar to Figure 9, but uses two panels to compare the derived values of [F/Fe] versus [Fe/H] (including results from Jönsson et al (2014b;, Pilachowski & Pace (2015) and Li et al (2013)) to predictions from a variety of models. The top panel shows only the derived stellar values of [F/Fe], while the bottom panel overlays the various chemical evolution models over the observed abundances.…”

Section: Chemical Evolution and The Sources Of Fluorinementioning

confidence: 99%

Fluorine Abundances in the Galactic Disk

Guerço

Cunha

Smith

et al. 2019

ApJ

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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 λ2.335µm. 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 19 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 supernovae of type II (SN II). A primary behavior for [F/Fe] at low metallicity is also observed for a model including rapid 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 ∼constant value of [F/Fe], indicating a very flat gradient (with a slope of 0.02 ± 0.03 dex/kpc) of this elemental ratio over a significant portion of the Galaxy having |Z| > 300 pc away from the Galaxy mid-plane.

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The Abundance of Fluorine in Normal G and K Stars of the Galactic Thin Disk

Cited by 25 publications

References 71 publications

Fluorine in the solar neighborhood: Chemical evolution models

Fluorine in the solar neighborhood: Chemical evolution models

Fluorine in the Solar Neighborhood: The Need for Several Cosmic Sources

Fluorine Abundances in the Galactic Disk

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