The12C+12C reaction at subcoulomb energies (II)

Becker, Hans‐Werner; Kettner, K. U.; Rolfs, C.; Trautvetter, H. P.

doi:10.1007/bf01421528

Cited by 130 publications

(193 citation statements)

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“…14 to the measured cross sections of Ref. [28][29][30][31]. The Ch12 calculation exceeds the data substantially between 3 and 5.5 MeV, whereas the Ch10 calculation is lower and intersects with some of the measured peak cross sections.…”

Section: Predictions Of the Fusion Of 12 C+ 12 Cmentioning

confidence: 81%

“…15 to the data of five experiments [28][29][30][31][32]. The symbols for the four measurements [28][29][30][31] are the same as in Fig.…”

Section: Predictions Of the Fusion Of 12 C+ 12 Cmentioning

confidence: 99%

“…[30]. [28][29][30][31][32] are compared to the coupled-channels calculations described in the text. The 13 C+ 13 C data have been divided by Sc = 0.843 which optimizes the fit to the data.…”

Section: Appendix: Couplingsmentioning

confidence: 99%

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Effects of mutual excitations in the fusion of carbon isotopes

2011

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Fusion data for 13 C+ 13 C, 12 C+ 13 C and 12 C+ 12 C are analyzed by coupled-channels calculations that are based on the M3Y+repulsion, double-folding potential. The fusion is determined by ingoingwave-boundary conditions (IWBC) that are imposed at the minimum of the pocket in the entrance channel potential. Quadrupole and octupole transitions to low-lying states in projectile and target are included in the calculations, as well as mutual excitations of these states. The effect of oneneutron transfer is also considered but the effect is small in the measured energy regime. It is shown that mutual excitations to high-lying states play a very important role in developing a comprehensive and consistent description of the measurements. Thus the shapes of the calculated cross sections for 12 C+ 13 C and 13 C+ 13 C are in good agreement with the data. The fusion cross sections for 12 C+ 12 C determined by the IWBC are generally larger than the measured cross sections but they are consistent with the maxima of some of the observed peak cross sections. They are therefore expected to provide an upper limit for the extrapolation into the low-energy regime of interest to astrophysics.

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Section: Predictions Of the Fusion Of 12 C+ 12 Cmentioning

confidence: 81%

“…15 to the data of five experiments [28][29][30][31][32]. The symbols for the four measurements [28][29][30][31] are the same as in Fig.…”

Section: Predictions Of the Fusion Of 12 C+ 12 Cmentioning

confidence: 99%

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Effects of mutual excitations in the fusion of carbon isotopes

2011

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“…When Khokhlov (1991) formulated the delayed detonation paradigm, the calculation of the carbon fusion rate was based on the Caughlan & Fowler (1988, hereafter CF88) fit to experimental cross-sections down to the same energy E cm (∼2.5 MeV), although with higher resolution (e.g. Becker et al 1981). The rate from CF88 differs from that of FCZ75 by less than 20% at T 10 9 K, and by less than a factor 2.5 at T 10 8 K. In the past 30 years, the lower limit to E cm reached experimentally has decreased to only 2.10 MeV Barrón-Palos et al 2006;Spillane et al 2007), because of experimental difficulties in reducing the background related to secondary reactions induced by hydrogen and deuterium contamination in the carbon targets.…”

Section: Introductionmentioning

confidence: 99%

Type Ia supernovae and the¹²C+¹²C reaction rate

Bravo

Piersanti

Domínguez

et al. 2011

A&A

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Context. Even if the 12 C+ 12 C reaction plays a central role in the ignition of type Ia supernovae (SNIa), the experimental determination of its cross-section at astrophysically relevant energies (E 2 MeV) has never been made. The profusion of resonances throughout the measured energy range has led to speculation that there is an unknown resonance at E 0 ∼ 1.5 MeV possibly as strong as the one measured for the resonance at 2.14 MeV, i.e. (ωγ) R = 0.13 meV. Aims. We study the implications that such a resonance would have for our knowledge of the physics of SNIa, paying special attention to the phases that go from the crossing of the ignition curve to the dynamical event.Methods. We use one-dimensional hydrostatic and hydrodynamic codes to follow the evolution of accreting white dwarfs until they grow close to the Chandrasekhar mass and explode as SNIa. In our simulations, we account for a low-energy resonance by exploring the parameter space allowed by experimental data. Results. A change in the 12 C+ 12 C rate similar to the one explored here would have profound consequences for the physical conditions in the SNIa explosion, namely the central density, neutronization, thermal profile, mass of the convective core, location of the runaway hot spot, or time elapsed since crossing the ignition curve. For instance, with the largest resonance strength we use, the time elapsed since crossing the ignition curve to the supernova event is shorter by a factor ten than for models using the standard rate of 12 C+ 12 C, and the runaway temperature is reduced from ∼8.14 × 10 8 K to ∼4.26 × 10 8 K. On the other hand, a resonance at 1.5 MeV, with a strength ten thousand times smaller than the one measured at 2.14 MeV, but with an α/p yield ratio substantially different from 1 would have a sizeable impact on the degree of neutronization of matter during carbon simmering. Conclusions. A robust understanding of the links between SNIa properties and their progenitors will not be attained until the 12 C+ 12 C reaction rate is measured at energies ∼1.5 MeV.

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“…Below a center of mass energy E cm of 2.5 MeV there is not enough energy to feed 23 Mg even in its ground state and α and p channel are the only relevant ones at low energies. Considerable efforts have been devoted to measure the 12 C + 12 C cross section at astrophysical energies, involving both, charged particle [11][12][13] and gamma ray spectroscopy [14][15][16][17][18][19]. Nevertheless, it has only been previously measured down to E cm = 2.5 MeV, still at the beginning of the region of astrophysical interest.…”

Section: Introductionmentioning

confidence: 99%

The¹²C(¹²C,α)²⁰Ne and¹²C(¹²C,p)²³Na reactions at the Gamow peak via the Trojan Horse Method

Туміно

Spitaleri

Cherubini

et al. 2016

EPJ Web of Conferences

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A measurement of the 12 C( 14 N,α 20 Ne) 2 H and 12 C( 14 N,p 23 Na) 2 H reactions has been performed at a 14 N beam energy of 30.0 MeV. The experiment aims to explore the extent to which contributing 24 Mg excited states can be populated in the quasi-free reaction off the deuteron in 14 N. In particular, the 24 Mg excitation region explored in the measurement plays a key role in stellar carbon burning whose cross section is commonly determined by extrapolating high-energy fusion data. From preliminary results, α and proton channels are clearly identified. In particular, ground and first excited states of 20 Ne and 23 Na play a major role.

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The12C+12C reaction at subcoulomb energies (II)

Cited by 130 publications

References 10 publications

Effects of mutual excitations in the fusion of carbon isotopes

Effects of mutual excitations in the fusion of carbon isotopes

Type Ia supernovae and the¹²C+¹²C reaction rate

The¹²C(¹²C,α)²⁰Ne and¹²C(¹²C,p)²³Na reactions at the Gamow peak via the Trojan Horse Method

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The12C+12C reaction at subcoulomb energies (II)

Cited by 130 publications

References 10 publications

Effects of mutual excitations in the fusion of carbon isotopes

Effects of mutual excitations in the fusion of carbon isotopes

Type Ia supernovae and the12C+12C reaction rate

The12C(12C,α)20Ne and12C(12C,p)23Na reactions at the Gamow peak via the Trojan Horse Method

Contact Info

Product

Resources

About

Type Ia supernovae and the¹²C+¹²C reaction rate

The¹²C(¹²C,α)²⁰Ne and¹²C(¹²C,p)²³Na reactions at the Gamow peak via the Trojan Horse Method