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Kelmar, R.; Simón, A.; Olivas-Gomez, O.; Millican, Patrick; Reingold, Craig; Churchman, E.; Clark, Adam M.; Henderson, S. L.; Kelly, Sean; Robertson, Daniel; Stech, E.; Tan, Wanpeng

doi:10.1103/physrevc.101.015801

Cited by 6 publications

(1 citation statement)

References 29 publications

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“…constrained by a broad range of measurements at (mostly stable beam) facilities across the world [231]. Direct measurements of the inverse p-process reactions with total absorption spectrometers at the University of Notre Dame have constrained properties of p-process nuclei near A = 100 [264,265], and measurements combining γ-spectroscopy and activation techniques performed at the University of Cologne and ATOMKI have focused on heavier p-process nuclei [266,267]. Measurements on unstable nuclei involved in p-process nucleosynthesis have recently become possible with novel recoil separation techniques, such as the EMMA separator at TRIUMF [268] and the ESR storage ring at GSI [269].…”

Section: How Did We Get Here?mentioning

confidence: 99%

Horizons: nuclear astrophysics in the 2020s and beyond

Schatz

Reyes

Best

et al. 2022

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

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Nuclear astrophysics is a field at the intersection of nuclear physics and astrophysics, which seeks to understand the nuclear engines of astronomical objects and the origin of the chemical elements. This white paper summarizes progress and status of the field, the new open questions that have emerged, and the tremendous scientific opportunities that have opened up with major advances in capabilities across an ever growing number of disciplines and subfields that need to be integrated. We take a holistic view of the field discussing the unique challenges and opportunities in nuclear astrophysics in regards to science, diversity, education, and the interdisciplinarity and breadth of the field. Clearly nuclear astrophysics is a dynamic field with a bright future that is entering a new era of discovery opportunities.

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Section: How Did We Get Here?mentioning

confidence: 99%

Horizons: nuclear astrophysics in the 2020s and beyond

Schatz

Reyes

Best

et al. 2022

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

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The γ-process nucleosynthesis in core-collapse supernovae

Roberti¹,

M.²,

Psaltis³

et al. 2023

A&A

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Context. The γ-process nucleosynthesis in core-collapse supernovae is generally accepted as a feasible process for the synthesis of neutron-deficient isotopes beyond iron. However, crucial discrepancies between theory and observations still exist: the average yields of γ-process nucleosynthesis from massive stars are still insufficient to reproduce the solar distribution in galactic chemical evolution calculations, and the yields of the Mo and Ru isotopes are a factor of ten lower than the yields of the other γ-process nuclei. Aims. We investigate the γ-process in five sets of core-collapse supernova models published in the literature with initial masses of 15, 20, and 25 M⊙ at solar metallicity. Methods. We compared the γ-process overproduction factors from the different models. To highlight the possible effect of nuclear physics input, we also considered 23 ratios of two isotopes close to each other in mass relative to their solar values. Further, we investigated the contribution of C–O shell mergers in the supernova progenitors as an additional site of the γ-process. Results. Our analysis shows that a large scatter among the different models exists for both the γ-process integrated yields and the isotopic ratios. We find only ten ratios that agree with their solar values, all the others differ by at least a factor of three from the solar values in all the considered sets of models. The γ-process within C–O shell mergers mostly influences the isotopic ratios that involve intermediate and heavy proton-rich isotopes with A > 100. Conclusions. We conclude that there are large discrepancies both among the different data sets and between the model predictions and the solar abundance distribution. More calculations are needed; particularly updating the nuclear network, because the majority of the models considered in this work do not use the latest reaction rates for the γ-process nucleosynthesis. Moreover, the role of C–O shell mergers requires further investigation.

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