The p-process in supernovae

Woosley, S. E.; Howard, W. M.

doi:10.1086/190501

Cited by 426 publications

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“…Considerable efforts have been devoted in recent years to improve the α + nucleus optical potential parametrizations for astrophysical applications [7][8][9]. In the present work, a comprehensive experimental test of the most recent global OMPs used in γ process network simulations is carried out for the target nucleus 113 In, which is traditionally considered a so-called p nucleus [10][11][12]. Typically, 113 In is underproduced in nucleosynthesis calculations of the p or γ process.…”

Section: Introductionmentioning

confidence: 99%

High precision113In(α,α)113In elastic scattering at energies near the Coulomb barrie

et al. 2013

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Background:The γ process in supernova explosions is thought to explain the origin of proton-rich isotopes between Se and Hg, the so-called p nuclei. The majority of the reaction rates for γ process reaction network studies have to be predicted in Hauser-Feshbach statistical model calculations using global optical potential parametrizations. While the nucleon + nucleus optical potential is fairly well known, for the α + nucleus optical potential several different parametrizations exist and large deviations are found between the predictions calculated using different parameter sets. Purpose: By the measurement of elastic α-scattering angular distributions at energies around the Coulomb barrier a comprehensive test for the different global α + nucleus optical potential parameter sets is provided. Methods: Between 20 • and 175 • complete elastic alpha scattering angular distributions were measured on the 113 In p nucleus with high precision at E c.m. = 15.59 and 18.82 MeV. Results: The elastic scattering cross sections of the 113 In(α,α) 113 In reaction were measured for the first time at energies close to the astrophysically relevant energy region. The high precision experimental data were used to evaluate the predictions of the recent global and regional α + nucleus optical potentials. Parameters for a local α + nucleus optical potential were derived from the measured angular distributions. Conclusions: Predictions for the reaction cross sections of 113 In(α, γ ) 117 Sb and 113 In(α,n) 116 Sb at astrophysically relevant energies were given using the global and local optical potential parametrizations.

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Section: Introductionmentioning

confidence: 99%

High precision113In(α,α)113In elastic scattering at energies near the Coulomb barrie

et al. 2013

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“…Using laser with an energy greater than 1 J, it is possible to study explosive nucleosyntheses in core-collapse supernovae (SNe). Some rare isotopes are synthesized by photodisintegration reactions with gamma-rays with energies in 7-9 MeV in SNe (gamma-process) [6,7].…”

Section: Discussionmentioning

confidence: 99%

Proposal of Direct Reaction Cross Section Measurements on an Excited State to Study Explosive Nucleosyntheses

Hayakawa

Nakamura

2017

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

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“…Later, however, it was recognized that there is no single process which can explain the synthesis of all p nuclei. This has led to the suggestion of a number of possible subprocesses: the rp process [3], the γ process [4], the ν process [5], and the νp process [6] (see also [7,8] and references therein). The favored scenario for synthesizing heavy p nuclei (A > 100) is the γ process.…”

Section: Introductionmentioning

confidence: 99%

“…The favored scenario for synthesizing heavy p nuclei (A > 100) is the γ process. Characterized by a combination of photodissociation reactions on existing heavy s-and r-seed nuclei, the γ process requires temperatures of around 2-3 × 10 9 K [4,9]. These conditions are met in explosive stellar environments, such as the O/Ne layers of type-II supernovae [4,10] or sub-Chandrasekhar-mass type-Ia supernovae environments [11,12].…”

Section: Introductionmentioning

confidence: 99%

Proton capture reaction cross section measurements on Er162 as a probe of statistical model calculations

et al. 2017

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It is crucial to measure reaction cross sections relevant to the astrophysical γ process so that theoretical reaction rates can be tested and validated with experimental data. The total cross sections for the 162 Er(p,γ ) 163 Tm and the 162 Er(p,n) 162 Tm reactions have been measured by the activation method in center-of-mass energies from 3.973 to 8.944 MeV and from 5.962 to 8.944 MeV, respectively. The nucleus 162 Er is the heaviest p nuclide to be measured by the activation method using γ -ray spectroscopy, so far. It is important to note that the energy range for the (p,γ ) reaction measurement covers a large fraction of the astrophysically relevant energy region between 2.71 and 5.34 MeV. The targets were prepared by evaporating 28.2% isotopically enriched 162 Er 2 O 3 powder onto carbon backing foils, and bombarded with proton beams provided by the FN Tandem Accelerator at the University of Notre Dame. The reaction yields have been determined by the observed activity of produced radioactive isotopes, which was detected offline by a high-purity germanium detector. The results are presented and compared with calculations from two statistical model codes: NON-SMOKER and TALYS.

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The p-process in supernovae

Cited by 426 publications

References 0 publications

High precision113In(α,α)113In elastic scattering at energies near the Coulomb barrie

High precision113In(α,α)113In elastic scattering at energies near the Coulomb barrie

Proposal of Direct Reaction Cross Section Measurements on an Excited State to Study Explosive Nucleosyntheses

Proton capture reaction cross section measurements on Er162 as a probe of statistical model calculations

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