R-process nucleosynthesis in the high-entropy supernova bubble

Meyer, B. S.; Mathews, Grant J.; Howard, W. M.; Woosley, S. E.; Hoffman, Robert D.

doi:10.1086/171957

Cited by 324 publications

(328 citation statements)

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“…In a radiation-dominated environment the entropy is given by a relation including temperature and density: S w ∝ T 3 /ρ. This is proportional to the photon-to-baryon ratio [26,27]. At high entropies the temperature is also high for densities which permit three body reactions.…”

Section: Wind Dynamics: Entropy and Expansion Time Scalementioning

confidence: 99%

“…They suggested that the later evolution could lead to high entropy and low electron fractions and thus to a successful r-process. In a following paper, Meyer et al (1992) [26] followed the evolution and nucleosynthesis after the alpha-rich freezeout based on different values of Y e . The final abundances, based on a superposition of various trajectories with different neutron excess, agreed rather well with the solar system abundances.…”

Section: Historical Overviewmentioning

confidence: 99%

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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: Wind Dynamics: Entropy and Expansion Time Scalementioning

confidence: 99%

Section: Historical Overviewmentioning

confidence: 99%

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 importance of the ααn reaction has been pointed out in the r-process in the hot bubble of a core-collapse supernova [2,3]. After the core bounce in the supernova, a nascent neutron star is formed at the center.…”

Section: Introductionmentioning

confidence: 99%

Astrophysical reaction rate for α(αn,γ)9Be by photodisintegration

et al. 2002

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We study the astrophysical reaction rate for the formation of 9 Be through the three body reaction α(αn, γ). This reaction is one of the key reactions which could bridge the mass gap at A = 8 nuclear systems to produce intermediate-to-heavy mass elements in alpha-and neutron-rich environments such as r-process nucleosynthesis in supernova explosions, s-process nucleosynthesis in asymptotic giant branch (AGB) stars, and primordial nucleosynthesis in baryon inhomogeneous cosmological models. To calculate the thermonuclear reaction rate in a wide range of temperatures, we numerically integrate the thermal average of cross sections assuming a two-steps formation through a metastable 8 Be, α + α ⇀ ↽ 8 Be(n,γ) 9 Be. Off-resonant and on-resonant contributions from the ground state in 8 Be are taken into account. As input cross section, we adopt the latest experimental data by photodisintegration of 9 Be with laser-electron photon beams, which covers all relevant resonances in 9 Be. Experimental data near the neutron threshold are added with γ-ray flux corrections and a new least-squares analysis is made to deduce resonance parameters in the Breit-Wigner formulation. Based on the photodisintegration cross section, we provide the reaction rate for α(αn, γ) 9 Be in the temperature range from T 9 =10 −3 to T 9 =10 1 (T 9 is the temperature in units of 10 9 K) both in the tabular form and in the analytical form for potential usage in nuclear reaction network calculations.The calculated reaction rate is compared with the reaction rates of the CF88 and the NACRE compilations. The CF88 rate, which is based on the photoneutron cross section for the 1/2 + state in 9 Be by Berman et al., is valid at T 9 > 0.028 due to lack of the off-resonant contribution. The CF88 rate differs from the present rate by a factor of two in a temperature range T 9 ≥ 0.1. The NACRE rate, which adopted different sources of experimental information on resonance states in 9 Be, is 4-12 times larger than the present rate at T 9 ≤ 0.028, but is consistent with the present rate to within ±20% at T 9 ≥ 0.1. 2

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“…These nuclei then become the seed nuclei to capture the remaining neutrons during the subsequent r-process. This is the neutrino-driven wind model of r-process nucleosynthesis in supernovae (e.g., [9,10,11,12]). …”

Section: Astrophysical Models and Observationsmentioning

confidence: 99%

Nuclear physics and astrophysics of the r-process

Qian

2005

Nuclear Physics A

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Some nuclear and astrophysical aspects of the r-process are discussed. Particular attention is paid to observations of abundances in metal-poor stars and their implications for the astrophysical site and yield patterns of the r-process. The effects of supernova neutrinos and related nuclear processes on the yield patterns are explored. The uncertainties in the theoretical nuclear input for the r-process are discussed and the need for experimental data is emphasized.

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R-process nucleosynthesis in the high-entropy supernova bubble

Cited by 324 publications

References 0 publications

Neutrino-driven wind simulations and nucleosynthesis of heavy elements

Neutrino-driven wind simulations and nucleosynthesis of heavy elements

Astrophysical reaction rate for α(αn,γ)9Be by photodisintegration

Nuclear physics and astrophysics of the r-process

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