Centroids of Gamow–Teller Transitions at Finite Temperature in fp-shell Neutron-rich Nuclei

Civitarese, O.; Ray, Anne E.

doi:10.1238/physica.regular.059a00352

Cited by 6 publications

(3 citation statements)

References 23 publications

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“…[23] for collective excitations in hot exotic nuclei. The finite temperature RPA has often been used to estimate e.g., beta decay rates in a stellar environment [19,20,24]. In order to make quantitative calculations for nuclear astrophysical purposes, especially for r-process nucleosynthesis, it is necessary to know the accuracy of finite temperature RPA also at relatively low temperatures.…”

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confidence: 99%

Test of finite temperature random-phase approximation on a Lipkin model

Hagino

Minato

2009

Phys. Rev. C

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We investigate the applicability of the finite temperature random phase approximation (RPA) using a solvable Lipkin model. We show that the finite temperature RPA reproduces reasonably well the temperature dependence of total strength, both for the positive energy (i.e., the excitation) and the negative energy (i.e., the de-excitation) parts. This is the case even at very low temperatures, which may be relevant to astrophysical purposes.

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confidence: 99%

Test of finite temperature random-phase approximation on a Lipkin model

Hagino

Minato

2009

Phys. Rev. C

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“…This makes the unblocking sensitive to temperature and lowers the energy threshold for the capture (see e.g. Civitarese & Ray 1999;Dzhioev et al 2010;Radha et al 1997). It is thus necessary to include these finite temperature effects in numerical simulations of core collapse to judge which among them can substantially modify the outcome of the simulations.…”

Section: Discussionmentioning

confidence: 99%

Effects of the temperature dependence of the in-medium nucleon mass on core-collapse supernovae

Fantina

Blottiau

Margueron

et al. 2012

A&A

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Aims. A complete description of the core collapse supernova mechanism requires an appropriate treatment of both the hydrodynamics and the microphysics. We study the influence of a nuclear physics input, namely the temperature dependence of the nucleon effective mass in nuclei induced by the in-medium effects, in the core collapse of a massive star. Methods. We present here the first implementation of this nuclear input in a hydrodynamical one-dimensional simulation. The simulations are performed with a spherically symmetric Newtonian model, with neutrino transport treated in the multi-group flux-limited diffusion approximation. Results. The inclusion of the temperature dependence of the in-medium nucleon mass has an impact on the equation of state of the system and reduces the deleptonisation during the collapse. This results in a non-negligible effect on the shock wave energetics. The shock wave is formed more outwards, and in the first few milliseconds after bounce the shock front has propagated further out.

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“…The centroids in fp-shell nuclei, found from experimental data from (n,p) reactions have been used for characterizing GT transitions in these nuclei [93] and are close to the value (3 MeV) used here. The GT centroid in the e-capture direction is itself a function of the ambient temperatures as a quasi-particle random phase approximation (QRPA) calculation shows [95]. At the relevant high densities, when neutron rich nuclei with A > 65, are abundant and the electron chemical potential is noticeably larger than typical nuclear Q-values, electron capture rates are mainly sensitive to the centroid and total strength of the GT+ distributions -these are reasonably well described within the random phase approximation [96].…”

Section: Electron Capture On Nuclei and Protons: A Core Thermometermentioning

confidence: 99%

Massive stars as thermonuclear reactors and their explosions following core collapse

Ray

2010

Astrophysics and Space Science Proceedings

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Summary. Nuclear reactions transform atomic nuclei inside stars. This is the process of stellar nucleosynthesis. The basic concepts of determining nuclear reaction rates inside stars are reviewed. How stars manage to burn their fuel so slowly most of the time are also considered. Stellar thermonuclear reactions involving protons in hydrostatic burning are discussed first. Then I discuss triple alpha reactions in the helium burning stage. Carbon and oxygen survive in red giant stars because of the nuclear structure of oxygen and neon. Further nuclear burning of carbon, neon, oxygen and silicon in quiescent conditions are discussed next. In the subsequent core-collapse phase, neutronization due to electron capture from the top of the Fermi sea in a degenerate core takes place. The expected signal of neutrinos from a nearby supernova is calculated. The supernova often explodes inside a dense circumstellar medium, which is established due to the progenitor star losing its outermost envelope in a stellar wind or mass transfer in a binary system. The nature of the circumstellar medium and the ejecta of the supernova and their dynamics are revealed by observations in the optical, IR, radio, and X-ray bands, and I discuss some of these observations and their interpretations.

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Centroids of Gamow–Teller Transitions at Finite Temperature in fp-shell Neutron-rich Nuclei

Cited by 6 publications

References 23 publications

Test of finite temperature random-phase approximation on a Lipkin model

Test of finite temperature random-phase approximation on a Lipkin model

Effects of the temperature dependence of the in-medium nucleon mass on core-collapse supernovae

Massive stars as thermonuclear reactors and their explosions following core collapse

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