Rate Tables for the Weak Processes of sd-Shell Nuclei in Stellar Matter

Oda, Takuya; Hino, M.; Muto, K.; Takahara, Mariko; Sato, Katsuhiko

doi:10.1006/adnd.1994.1007

Cited by 323 publications

(306 citation statements)

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“…This point seems already fixed, as the rates for sd-shell nuclei have remained almost unchanged since the work of Takahara et al (1989). However, the data of Oda et al (1994) are much richer for 24 Mg,20 Ne and other sdshell nuclei relevant for this work, such as 23 Na and 25 Mg.…”

Section: Input Physics and Initial Modelmentioning

confidence: 83%

See 1 more Smart Citation

The gravitational collapse of ONe electron-degenerate cores and white dwarfs: The role of $^\mathsf{24}$Mg and $^\mathsf{12}$C revisited

Gutiérrez¹,

Canal

Garcı́a–Berro

2005

A&A

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Abstract. The final stages of the evolution of electron-degenerate ONe cores, resulting from carbon burning in "heavy weight" intermediate-mass stars (8 M < ∼ M < ∼ 11 M ) and growing in mass, either from carbon burning in a shell or from accretion of matter in a close binary system, are examined in the light of their detailed chemical composition. In particular, we have modelled the evolution taking into account the abundances of the following minor nuclear species, which result from the previous evolutionary history: 12 C, 23 Na, 24 Mg, and 25 Mg. Both 23 Na and 25 Mg give rise to Urca processes, which are found to be unimportant for the final outcome of the evolution. 24 Mg was formerly considered a major component of ONe cores (hence called ONeMg cores), but updated evolutionary calculations in this mass range have severely reduced its abundance. Nevertheless, we have parameterized it and we have found that the minimum amount of 24 Mg required to produce NeO burning at moderate densities is ∼23%, a value exceedingly high in the light of recent evolutionary models. Finally, we have determined that models with relatively small abundances of unburnt carbon (X( 12 C) ∼ 0.015) could be a channel to explosion at low to moderate density (∼1 × 10 9 g cm −3 ). This is clearly below the current estimate for the explosion/collapse threshold and would have interesting consequences.

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Section: Input Physics and Initial Modelmentioning

confidence: 83%

“…Electron capture rates have been taken from Oda et al (1994), which provides the most up-to-date, and physically consistent determinations. This point seems already fixed, as the rates for sd-shell nuclei have remained almost unchanged since the work of Takahara et al (1989).…”

Section: Input Physics and Initial Modelmentioning

confidence: 99%

The gravitational collapse of ONe electron-degenerate cores and white dwarfs: The role of $^\mathsf{24}$Mg and $^\mathsf{12}$C revisited

Gutiérrez¹,

Canal

Garcı́a–Berro

2005

A&A

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“…Then, choose a single effective Q-value and transition strength to reproduce published neutrino production and energy loss rates [2][3][4][5][6][7]. Finally, apply eqs.…”

Section: Charged Currentmentioning

confidence: 99%

Neutrinos from Pre-Collapse Stars

Misch¹,

Fuller²

2017

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

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We show that in order to make realistic predictions of the nuclear neutrino spectra from pre-collapse stellar cores, one must properly account for nuclear structure effects; often, the dominant nuclear transitions involve excited states, sometimes in both parent and daughter nuclei. We show that the standard technique of producing a neutrino energy spectrum by using a single effective transition structured to fit published neutrino production rates and energy losses will not accurately capture important spectral features.

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“…• for compiled experimental and theoretical β-decay and electron capture rates: -the experimental β-decay rates of Katakura (1996); -the β-decay rates of Takahashi & Yokoi (1987, see also Goriely 1999; -specific electron capture rates from various published sources; -β-decay rates calculated with the revised Gross theory (Tachibana et al 1990) and Q-values from the HFB-14 mass model; -β-decay rates calculated with the QRPA plus FRDM models by Möller et al (1996); -the density-and temperature-dependent β-decay rates calculated by Oda et al (1994) or Langanke & Martinez-Pinedo (2000).…”

Section: Contentmentioning

confidence: 99%

Databases and tools for nuclear astrophysics applications

Goriely

Jorissen

et al. 2013

A&A

128

118

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An update of a previous description of the BRUSLIB + NACRE package of nuclear data for astrophysics and of the web-based nuclear network generator NETGEN is presented. The new version of BRUSLIB contains the latest predictions of a wide variety of nuclear data based on the most recent version of the Brussels-Montreal Skyrme-Hartree-Fock-Bogoliubov model. The nuclear masses, radii, spin/parities, deformations, single-particle schemes, matter densities, nuclear level densities, E1 strength functions, fission properties, and partition functions are provided for all nuclei lying between the proton and neutron drip lines over the 8 ≤ Z ≤ 110 range, whose evaluation is based on a unique microscopic model that ensures a good compromise between accuracy, reliability, and feasibility. In addition, these various ingredients are used to calculate about 100 000 Hauser-Feshbach neutron-, proton-, α-, and γ-induced reaction rates based on the reaction code TALYS. NACRE is superseded by the NACRE II compilation for 15 charged-particle transfer reactions and 19 charged-particle radiative captures on stable targets with mass numbers A < 16. NACRE II features the inclusion of experimental data made available after the publication of NACRE in 1999 and up to 2011. In addition, the extrapolation of the available data to the very low energies of astrophysical relevance is improved through the systematic use of phenomenological potential models. Uncertainties in the rates are also evaluated on this basis. Finally, the latest release v10.0 of the web-based tool NETGEN is presented. In addition to the data already used in the previous NETGEN package, it contains in a fully documented form the new BRUSLIB and NACRE II data, as well as new experiment-based radiative neutron capture cross sections. The full new versions of BRUSLIB, NACRE II, and NETGEN are available electronically from the nuclear database at http://www. astro.ulb.ac.be/NuclearData. The nuclear material is presented in an extended tabular form complemented with a variety of graphical interfaces.

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Rate Tables for the Weak Processes of sd-Shell Nuclei in Stellar Matter

Cited by 323 publications

References 0 publications

The gravitational collapse of ONe electron-degenerate cores and white dwarfs: The role of $^\mathsf{24}$Mg and $^\mathsf{12}$C revisited

The gravitational collapse of ONe electron-degenerate cores and white dwarfs: The role of $^\mathsf{24}$Mg and $^\mathsf{12}$C revisited

Neutrinos from Pre-Collapse Stars

Databases and tools for nuclear astrophysics applications

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