The Galactic evolution of phosphorus

Caffau, E.; Bonifacio, P.; Faraggiana, R.; Steffen, M.

doi:10.1051/0004-6361/201117313

Cited by 39 publications

(88 citation statements)

References 30 publications

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“…The difference between the model and stellar abundances therefore follows the same metallicity dependence as the predicted chemical evolution model (the model slope), which constrains the potential mechanisms needed to enhance P abundances in the chemical evolution models. Possibly the neutron capture cross-section may need to be revisited or Caffau et al (2011) suggested proton capture on Si may need to be considered as a possible P production pathway.…”

Section: P Abundances Vs T Effmentioning

confidence: 99%

Phosphorus Abundances in the Hyades and Galactic Disk

Maas

Cescutti

Pilachowski

2019

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We have measured phosphorus abundances in nine disk stars between -1 < [Fe/H] < -0.5 and in 12 members of the Hyades open cluster using two P I lines at 1.06 µm. High resolution infrared spectra were obtained using Phoenix on Gemini South and abundances were determined by comparing synthetic spectra to the observations. The average abundance for the dwarf stars in our Hyades sample was < [P/Fe] > = -0.01 ± 0.06 and < [P/Fe] > = 0.03 ± 0.03 dex for the three giants. The consistency suggests abundances derived using the 1.06 µm P I lines are not subjected to temperature or luminosity dependent systematic effects at high metallicities. Our [P/Fe] ratios measured in disk stars are consistent with chemical evolution models with P yields increased by a factor of 2.75. We find [P/O], [P/Mg], [P/Si] and [P/Ti] ratios are consistent with the solar ratio over a range of -1.0 < [Fe/H] < 0.2 with the [P/Si] ratio increasing by ∼ 0.1 -0.2 dex at the lowest [Fe/H] ratios. Finally, the evolution of [P/Fe] with age is similar to other α elements, providing evidence that P is produced at the same sites.

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Section: P Abundances Vs T Effmentioning

confidence: 99%

Phosphorus Abundances in the Hyades and Galactic Disk

Maas

Cescutti

Pilachowski

2019

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“…Phosphorus (Z = 15) has never been measured in HD 84937 and indeed has been measured in very few metalpoor stars, including only five stars with a metallicity below [Fe/H] < −2.0 dex (Caffau et al 2011a(Caffau et al , 2016Roederer et al 2014). Its behaviour hints at a primary origin in massive stars .…”

Section: Introductionmentioning

confidence: 99%

Abundances of the light elements from UV (HST) and red (ESO) spectra in the very old star HD 84937

Spite

Peterson

Gallagher

et al. 2017

A&A

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Aims. In order to provide a better basis for the study of mechanisms of nucleosynthesis of the light elements beyond hydrogen and helium in the oldest stars, the abundances of C, O, Mg, Si, P, S, K, and Ca have been derived from UV-HST and visible-ESO high resolution spectra in the old, very metal-poor star HD 84937, at a metallicity that is 1/200 that of the Sun's. For this halo main-sequence turnoff star, the abundance determination of P and S are the first published determinations. Methods. The LTE profiles of the lines were computed and fitted to the observed spectra. Wherever possible, we compared the abundances derived from the UV spectrum to abundances derived from the visible or near-infrared spectra, and also corrected the derived abundances for non-LTE effects. Three-dimensional (3D) CO 5 BOLD model atmospheres have been used to determine the abundances of C and O from molecular CH and OH bands. Results. The abundances of these light elements relative to iron in HD 84937 are found to agree well with the abundances of these elements in classical metal-poor stars. Our HD 84937 carbon abundance determination points toward a solar (or mildly enhanced above solar) value of [C/Fe]. The modest overabundance of the α elements of even atomic number Z, typical of halo turnoff stars, is confirmed in this example. The odd-Z element P is found to be somewhat deficient in HD 84937, at [P/Fe] = −0.32, which is again consistent with the handful of existing determinations for turnoff stars of such low metallicity. We show that the abundance of oxygen, deduced from the OH band from 3D computations, is not compatible with the abundance deduced from the red oxygen triplet. This incompatibility is explained by the existence of a chromosphere heating the shallow layers of the atmosphere where the OH band, in 3D computations, is mainly formed. Conclusions. The abundance ratios are compared to the predictions of models of galactic nucleosynthesis and evolution.

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“…It is a cosmically relatively abundant element, P/H ∼ 3 × 10 −7 (Grevesse & Sauval 1998). It has been detected toward the atmospheres of stars (Caffau et al 2011(Caffau et al , 2016Roederer et al 2014), but it is barely detected in the ISM. The ion P + has been detected in several diffuse clouds (Jura & York 1978) and only a few simple P-bearing species (PN, PO, CP, HCP, C 2 P, PH 3 ) have been identified toward the circumstellar envelopes of very evolved objects (Tenenbaum et al 2007;De Beck et al 2013;Agúndez et al 2014).…”

Section: Introductionmentioning

confidence: 99%

The First Detections of the Key Prebiotic Molecule Po in Star-Forming Regions

Rivilla

Fontani

Beltrán

et al. 2016

ApJ

106

135

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Phosphorus is a crucial element in biochemistry, in particular the P−O bond, which is key in the formation of the backbone of deoxyribonucleic acid. So far, PO has only been detected toward the envelope of evolved stars, but never toward star-forming regions. We report the first detection of PO toward two massive star-forming regions, W51 e1/e2 and W3(OH), using data from the IRAM 30 m telescope. PN has also been detected toward the two regions. The abundance ratio PO/PN is 1.8 and 3 for W51 and W3(OH), respectively. Our chemical model indicates that the two molecules are chemically related and are formed via gas-phase ion-molecule and neutralneutral reactions during cold collapse. The molecules freeze out onto grains at the end of the collapse and desorb during the warm-up phase once the temperature reaches ∼35 K. Similar abundances of the two species are expected during a period of ∼5 × 10 4 yr at the early stages of the warm-up phase, when the temperature is in the range 35-90 K. The observed molecular abundances of 10 −10 are predicted by the model if a relatively high initial abundance of 5 × 10 −9 of depleted phosphorus is assumed.

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The Galactic evolution of phosphorus

Cited by 39 publications

References 30 publications

Phosphorus Abundances in the Hyades and Galactic Disk

Phosphorus Abundances in the Hyades and Galactic Disk

Abundances of the light elements from UV (HST) and red (ESO) spectra in the very old star HD 84937

The First Detections of the Key Prebiotic Molecule Po in Star-Forming Regions

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