Path to metallicity: Synthesis of CNO elements in standard BBN

Iocco, Fabio; Mangano, G.; Miele, Gennaro; Pisanti, O.; Serpico, Pasquale Dario

doi:10.1103/physrevd.75.087304

Cited by 46 publications

(156 citation statements)

References 21 publications

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“…These results are consistent with those of Iocco et al [33] but slightly lower than those of Vonlanthen et al [62]. Detailed CNO, B and Be isotopic abundances, compared with those from Iocco et al [33] can be found in Table 7, together with H, He and Li isotopic abundances compared with our previous work. As expected, the extension of the network does not alleviate the 7 Li discrepancy between calculations and observations.…”

Section: Resultssupporting

confidence: 82%

“…The minimum value of the initial CNO abundance that would affect Pop III stellar evolution is estimated to be as low as 10 −13 (in number of atoms relative to hydrogen, CNO/H) for the less massive ones [32]. This is only two orders of magnitude above the Standard Big Bang Nucleosynthesis CNO yield, using the current nuclear reaction rate evaluations of Iocco et al [33]. In addition, it has been shown that Pop III stars evolution is sensitive to the triple-alpha ( 12 C producing) reaction and can be used to constrain the possible variation of the fundamental constants [34].…”

Section: Bbn Production Of Heavier Elementsmentioning

confidence: 96%

“…15 in [37]), an evolution followed by 8 Li and CNO isotopes. From this table, we can deduce that the main nuclear paths to CNO (see also [33]) proceeds from the 7 Li(α, γ) 11 B reaction followed by 11 B(p,γ) 12 C, 11 B(d,n) 12 C, 11 B(d,p) 12 B and 11 B(n,γ) 12 B reactions. Another nucleosynthesis path starts with 7 Li(n,γ) 8 Li(α,n) 11 B.…”

Section: Sensitivity Studymentioning

confidence: 99%

“…The production of CNO isotopes has been studied in the context of standard and inhomogeneous BBN. The most relevant analysis comes from Iocco et al [33] who included more than 100 nuclear reactions and predicted a CNO/H abundance ratio of approximately 6 × 10 −16 , with an upper limit of 10 −10 .…”

Section: Bbn Production Of Heavier Elementsmentioning

confidence: 99%

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Primordial Nucleosynthesis

Coc¹

2013

Acta Phys. Pol. B

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Abstract. Primordial nucleosynthesis, or Big Bang Nucleosynthesis (BBN), is one of the three evidences for the Big-Bang model, together with the expansion of the Universe and the Cosmic Microwave Background. There is a good global agreement over a range of nine orders of magnitude between abundances of 4 He, D, 3 He and 7 Li deduced from observations, and calculated in primordial nucleosynthesis. This comparison was used to determine the baryonic density of the Universe. For this purpose, it is now superseded by the analysis of the Cosmic Microwave Background (CMB) radiation anisotropies. However, there remain, a yet unexplained, discrepancy of a factor 3-5, between the calculated and observed lithium primordial abundances, that has not been reduced, neither by recent nuclear physics experiments, nor by new observations. We review here the nuclear physics aspects of BBN for the production of 4 He, D, 3 He and 7 Li, but also 6 Li, 9 Be, 11 B and up to CNO isotopes. These are, for instance, important for the initial composition of the matter at the origin of the first stars. Big-Bang nucleosynthesis, that has been used, to first constrain the baryonic density, and the number of neutrino families, remains, a valuable tool to probe the physics of the early Universe, like variation of "constants" or alternative theories of gravity.

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Section: Resultssupporting

confidence: 82%

Section: Bbn Production Of Heavier Elementsmentioning

confidence: 96%

Section: Sensitivity Studymentioning

confidence: 99%

Section: Bbn Production Of Heavier Elementsmentioning

confidence: 99%

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Primordial Nucleosynthesis

Coc¹

2013

Acta Phys. Pol. B

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“…Provided that the properties of dark matter allow the formation of dark stars, objects of this type are expected to be among the first stars forming in the history of the universe and therefore to have extremely low metallicities Z, possibly at the level given by Big Bang nucleosynthesis (this implies Z ∼ 10 −9 mainly due to Li; e.g., Iocco et al 2007). All models therefore assume primordial abundances of H and He.…”

Section: Model Atmosphere Spectramentioning

confidence: 99%

FINDING HIGH-REDSHIFT DARK STARS WITH THEJAMES WEBB SPACE TELESCOPE

Zackrisson¹,

Scott²,

Rydberg³

et al. 2010

ApJ

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The first stars in the history of the universe are likely to form in the dense central regions of ∼10 5 -10 6 M cold dark matter halos at z ≈ 10-50. The annihilation of dark matter particles in these environments may lead to the formation of so-called dark stars, which are predicted to be cooler, larger, more massive, and potentially more long-lived than conventional population III stars. Here, we investigate the prospects of detecting high-redshift dark stars with the upcoming James Webb Space Telescope (JWST). We find that all dark stars with masses up to 10 3 M are intrinsically too faint to be detected by JWST at z > 6. However, by exploiting foreground galaxy clusters as gravitational telescopes do, certain varieties of cool (T eff 30,000 K) dark stars should be within reach at redshifts up to z ≈ 10. If the lifetimes of dark stars are sufficiently long, many such objects may also congregate inside the first galaxies. We demonstrate that this could give rise to peculiar features in the integrated spectra of galaxies at high redshifts, provided that dark stars make up at least ∼1% of the total stellar mass in such objects.

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Metal Enrichment in the Reionization Epoch

Ferrara

2016

Understanding the Epoch of Cosmic Reionization

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The presence of elements heavier than helium ("metals") is of fundamental importance for a large number of astrophysical processes occurring in planet, star and galaxy formation; it also affects cosmic structure formation and evolution in several ways. Even a small amount of heavy elements can dramatically alter the chemistry of the gas, opening the path to complex molecules. Metals might enhance the ability of the gas to radiate away its thermal energy, thus favoring the formation of gravitationally bound objects; they can also condensate in a solid phase (dust grains), partly or totally blocking radiation from luminous sources. Finally, they represent useful tracers of energy deposition by stars and probe the physical properties of the environment by absorption or emission lines. Last, but certainly not least, life -- as we know it on Earth -- is tightly related to the presence of at least some of the heavy elements. In this pedagogical review I will concentrate on the connection between early metal enrichment and cosmic reionization. As we will see these two processes are intimately connected and their joint study might turn out to be fundamental in understanding the overall evolution of the Universe during the first billion years after the Big Bang, an epoch corresponding to redshifts z>6.Comment: Book chapter in Understanding the Epoch of Cosmic Reionization: Challenges and Progress, Springer International Publishing, Ed. Andrei Mesinger, ISBN 978-3-319-21956-1. arXiv admin note: text overlap with arXiv:astro-ph/0007248 by other author

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Path to metallicity: Synthesis of CNO elements in standard BBN

Cited by 46 publications

References 21 publications

Primordial Nucleosynthesis

Primordial Nucleosynthesis

FINDING HIGH-REDSHIFT DARK STARS WITH THEJAMES WEBB SPACE TELESCOPE

Metal Enrichment in the Reionization Epoch

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