Neutrino-Induced Nucleosynthesis of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>A</mml:mi><mml:mo>&gt;</mml:mo><mml:mn>64</mml:mn></mml:math>Nuclei: The<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>ν</mml:mi><mml:mi>p</mml:mi></mml:math>Process

Fröhlich, C.; Martı́nez-Pinedo, G.; Liebendörfer, M.; Thielemann, Friedrich‐Karl; Bravo, Eduardo; Hix, W. R.; Langanke, K.; Zinner, N. T.

doi:10.1103/physrevlett.96.142502

Cited by 537 publications

(465 citation statements)

References 26 publications

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“…Under such conditions the rapid neutron capture process to form the heaviest nuclei cannot occur, ruling out the spherically symmetric neutrino-driven winds as its astrophysical site. However, this conditions become very favourable for the νp-process [28].…”

Section: Weak Interactions: Electron Fractionmentioning

confidence: 99%

“…Hydrodynamical simulations of core-collapse supernovae with sophisticated neutrino transport indicate that the early ejecta may be proton rich instead of neutron-rich [118,119,120,121,28,122,123]. Even long-time simulations suggest that spherically symmetric neutrino-driven winds could stay proton rich during several seconds [13,12].…”

Section: νP-processmentioning

confidence: 99%

“…In proton-rich condition elements beyond iron group can be synthesized by the νp-process [120,28,123]. Proton and alpha captures drive the matter flow up to 64 Ge which is a waiting point as its beta-decay half live is long compared to the expansion time scale of the wind.…”

Section: νP-processmentioning

confidence: 99%

See 2 more Smart Citations

Neutrino-driven wind simulations and nucleosynthesis of heavy elements

Arcones

Thielemann

2012

J. Phys. G: Nucl. Part. Phys.

195

201

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Abstract. Neutrino-driven winds, which follow core-collapse supernova explosions, present a fascinating nuclear astrophysics problem that requires understanding advanced astrophysics simulations, the properties of matter and neutrino interactions under extreme conditions, the structure and reactions of exotic nuclei, and comparisons against forefront astronomical observations. The neutrino-driven wind has attracted vast attention over the last 20 years as it was suggested to be a candidate for the astrophysics site where half of the heavy elements are produced via the r-process. In this review, we summarize our present understanding of neutrino-driven winds from the dynamical and nucleosynthesis perspectives. Rapid progress has been made during recent years in understanding the wind with improved simulations and better micro physics. The current status of the fields is that hydrodynamical simulations do not reach the extreme conditions necessary for the r-process and the proton or neutron richness of the wind remains to be investigated in more detail. However, nucleosynthesis studies and observations point already to neutrino-driven winds to explain the origin of lighter heavy elements, such as Sr, Y, Zr.

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Section: Weak Interactions: Electron Fractionmentioning

confidence: 99%

Section: νP-processmentioning

confidence: 99%

See 1 more Smart Citation

Neutrino-driven wind simulations and nucleosynthesis of heavy elements

Arcones

Thielemann

2012

J. Phys. G: Nucl. Part. Phys.

195

201

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“…the lightest elements beyond the iron group [1][2][3]. The νp-process occurs in proton-rich neutrino-driven winds from core-collapse supernovae.…”

Section: Introductionmentioning

confidence: 99%

Nuclear Reactions and the \(\nu \)p-Process

Fröhlich¹,

Hatcher²,

Perdikakis³

et al. 2017

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016)

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In understanding the origin of the heavy elements, the "light heavy elements" pose a particular challenge: The two neutron-capture processes, r-process and s-process, cannot explain the abundances patterns seen in very old galactic halo stars. A proposed solution to this problem is the νp-process, which takes place in the strong neutrino-driven winds of core-collapse supernovae. In the νp-process, a sequence of (n,p) and (p,γ) reactions allows for the synthesis of elements with atomic numbers A > 64, which includes Sr, Y, Zr, and others possibly up to Sn. The relevant reaction rates are all based on statistical model predictions and carry some uncertainty. Here, the sensitivity of the final νp-process abundance pattern on modifications of (n,p), (p,γ), and (n,γ) reactions are characterized. Only few reactions affect the final abundance pattern and hence warrant a more detailed study of the reaction rate.

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“…Nevertheless, it has benefited greatly from models of massive ( 8 M ⊙ ) star evolution (e.g., [8]), core-collapse supernovae (e.g., [9]), and neutron star mergers (e.g., [10,11]), from recognition of the importance of neutrinos to these models (e.g., [12,13]), and from observations of elemental abundances in stars formed over the Galactic history (e.g., [14]) as well as meteoritic measurements of radioactive isotopes present in the early solar system (e.g., [15,16]). The above efforts not only have improved our understanding of the r process, but also have led to discoveries of new processes that make elements heavier than Fe not in the same way as the classical r or s process (e.g., [17,18]). …”

Section: Introductionmentioning

confidence: 99%