Large collection of astrophysical<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>S</mml:mi></mml:math>factors and their compact representation

Afanasjev, A. V.; Beard, M.; Chugunov, A. I.; Wiescher, M.; Yakovlev, D. G.

doi:10.1103/physrevc.85.054615

Cited by 31 publications

(50 citation statements)

References 32 publications

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“…(16) where σ(E) is the calculated cross section using DFM and DFC potentials in comparison with the analytical S-factor of Afanasjev et. al [34] and Gasques et. al [35].…”

Section: Astrophysical Aspectsmentioning

confidence: 87%

“…al. [34]. Another analytical expression of S(E) for the fusion [35] whereas the dashed-dotted line is the results of Afanasjev et.…”

Section: Astrophysical Aspectsmentioning

confidence: 93%

“…All the extrapolations give a good description of the average of the data in the energy range of E = 2.5 MeV to 7 MeV with very small order of magnitude differences between A-W and the double folding potentials calculations. Only the analytical prediction from Afanasjev [34] gives very low extrapolation of the data at very low energy. The predictions of S * (E) by different potential models are presented in Figures 5 One of the important basic quantity needed for understanding the nature of stellar evolution and nucleosynthesis is the reaction rate.…”

Section: Astrophysical Aspectsmentioning

confidence: 95%

“…Another analytical expression of S(E) for the fusion [35] whereas the dashed-dotted line is the results of Afanasjev et. al [34]. The experimental data are taken from Ref.…”

Section: Astrophysical Aspectsmentioning

confidence: 99%

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Reliability of the double-folding potential for fusion cross sections of light systems

et al. 2015

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We study the fusion reaction of light systems with one dimensional barrier penetration model using the α − α double folding cluster (DFC) potential. We especially analyze the fusion cross sections of the 12 C+ 12 C, 16 O, 24 Mg, 28 Si, 16 O + 16 O, 24 Mg + 24 Mg, 28 Si, and 28 Si + 28 Si reactions. The results are compared with the one obtained with M3Y double folding (DFM) and the Akyüz-Winther (A-W) potentials. It is found that the calculations with DFM and DFC potentials can reproduced the experimental data much better than the calculations using the A-W potential. We also carried out an analysis on the astrophysical aspect of the 12 C + 12 C, 16 O, and 16 O + 16 O reactions. The calculations using DFC and DFM potentials could fit the S-factor data reasonably well. However, the calculated reaction rates are lower than the compilation of Caughlan and Fowler at low temperatures. In the important range of temperatures in stellar evolution, the DFC potential reproduce very satisfactory fitting to the experimental cross section and the S-factor data and gives a consistent prediction of astrophysical reaction rates. This finding indicates that the DFC potential could be used as an alternative potential to study the fusion reactions in the astrophysical interest.

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“…(16) where σ(E) is the calculated cross section using DFM and DFC potentials in comparison with the analytical S-factor of Afanasjev et. al [34] and Gasques et. al [35].…”

Section: Astrophysical Aspectsmentioning

confidence: 87%

“…al. [34]. Another analytical expression of S(E) for the fusion [35] whereas the dashed-dotted line is the results of Afanasjev et.…”

Section: Astrophysical Aspectsmentioning

confidence: 93%

Section: Astrophysical Aspectsmentioning

confidence: 95%

“…Another analytical expression of S(E) for the fusion [35] whereas the dashed-dotted line is the results of Afanasjev et. al [34]. The experimental data are taken from Ref.…”

Section: Astrophysical Aspectsmentioning

confidence: 99%

See 2 more Smart Citations

Reliability of the double-folding potential for fusion cross sections of light systems

et al. 2015

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“…Heavy-ion fusion at low energies is very important in the physics of stars [8,11,12]. As a result, the nucleus-nucleus interaction potential is a key ingredient for the description of various nuclear reactions in the nature.…”

Section: Introductionmentioning

confidence: 99%

Nucleus-nucleus potential with shell-correction contribution

Denisov

2015

Phys. Rev. C

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The full relaxed-density potential between spherical nuclei is considered as a sum of the macroscopic and shell-correction contributions. The macroscopic part of the potential is related to a nucleus-nucleus potential obtained in the framework of the extended Thomas-Fermi approach with the Skyrme and Coulomb forces and the relaxed-density ansatz for evaluation of proton and neutron densities of interacting nuclei. A simple prescription for the shell-correction part of the total potential is discussed. The parameters of the shell-correction and macroscopic parts of the relaxed-density potential are found by fitting the empirical barrier heights of the 89 nucleus-nucleus systems as well as macroscopic potentials evaluated for 1485 nucleus-nucleus systems at 12 distances around touching points.Comment: 11 pages, 4 figure

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Reaction Rates and Transport in Neutron Stars

Schmitt

Shternin

2018

The Physics and Astrophysics of Neutron Stars

119

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Understanding signals from neutron stars requires knowledge about the transport inside the star. We review the transport properties and the underlying reaction rates of dense hadronic and quark matter in the crust and the core of neutron stars and point out open problems and future directions. arXiv:1711.06520v3 [astro-ph.HE] 29 Oct 2018 65 References 66 I. INTRODUCTION A. ContextTransport describes how conserved quantities such as energy, momentum, particle number, or electric charge are transferred from one region to another. Such a transfer occurs if the system is out of equilibrium, for instance through a temperature gradient or a non-uniform chemical composition. Different theoretical methods are used to understand transport, depending on how far the system is away from its equilibrium state. If the system is close to equilibrium locally and perturbations are on large scales in space and time, hydrodynamics is a powerful technique. Further away from equilibrium other techniques are required, for example kinetic theory, which can also be used to provide the transport coefficients needed in the hydrodynamic equations. In any case, transport is determined by interactions on a microscopic level, and it is the resulting transport properties that we are concerned with in this review.Signals from neutron stars are sensitive to equilibrium properties such as the equation of state but also, to a large extent, to transport properties -here, by neutron stars we mean all objects with a radius of about 10 km and a mass of about 1-2 solar masses, including the possibilities of hybrid stars, which have a quark matter core, and pure quark stars. Therefore, understanding transport is crucial to interpret astrophysical observations, and, turning the argument around, we can use astrophysical observations to improve our understanding of transport in dense matter and thus ultimately our understanding of the microscopic interactions.Transport properties are most commonly computed from particle collisions. (Although, in strongly coupled systems, the picture of well-defined particles scattering off each other has to be taken with care.) These can be scattering processes in which energy and momentum is exchanged without changing the chemical composition of the system, or these can be flavor-changing processes from the electroweak interaction. Understanding transport thus amounts to understanding the rates of these processes, as a function of temperature and density. Electroweak processes are well understood, but large uncertainties arise if the strong interaction is involved in a reaction that contributes to transport. Therefore, approximations such as weak-coupling techniques or one-pion exchange for nucleon-nucleon collisions are being used, and efforts in current research aim at improving these approximations.In a neutron star, most of the particles involved in these processes are fermions: electrons, muons, neutrinos, neutrons, protons, hyperons, and quarks. Since the Fermi momenta of these fermions are typically much larger tha...

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Large collection of astrophysicalSfactors and their compact representation

Cited by 31 publications

References 32 publications

Reliability of the double-folding potential for fusion cross sections of light systems

Reliability of the double-folding potential for fusion cross sections of light systems

Nucleus-nucleus potential with shell-correction contribution

Reaction Rates and Transport in Neutron Stars

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