Nuclear Physics of Stars

Iliadis, Christian

doi:10.1002/9783527692668

Cited by 317 publications

(482 citation statements)

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“…However, the quantity that will ultimately be used in calculations of resonance strengths and DC cross sections is the stopping cross section of the 22 Ne-Ta combination in the center-of-mass frame, ef f . This quantity is related to n 22 through the relation [42] c.m. where ∆E is the energy loss in the center-of-mass frame.…”

Section: Targetsmentioning

confidence: 99%

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New measurements of low-energy resonances in theNe22(p,γ)Na23reaction

et al. 2017

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The 22 Ne(p,γ) 23 Na reaction is one of the most uncertain reactions in the NeNa cycle and plays a crucial role in the creation of 23 Na, the only stable Na isotope. Uncertainties in the low-energy rates of this and other reactions in the NeNa cycle lead to ambiguities in the nucleosynthesis predicted from models of thermally pulsing AGB stars. This in turn complicates the interpretation of anomalous Na-O trends in globular cluster evolutionary scenarios. (2015) and is attributed to the interplay between the 23 Na(p,α) 20 Ne and 20 Ne(p,γ) 21 Na reactions, both of which remain fairly uncertain at the relevant temperature range.

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Section: Targetsmentioning

confidence: 99%

“…Direction-direction correlations were calculated according to Refs. [39,42,47] and incorporated into the all simulations. The energy resolution of the detector was measured as a function of γ-ray energy by populating the E c.m.…”

Section: A Standard Tfractionfitter Routinementioning

confidence: 99%

New measurements of low-energy resonances in theNe22(p,γ)Na23reaction

et al. 2017

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“…The observation of 1809 keV gamma-rays from the beta decay of 26 Al ground state is one of the direct proofs of the ongoing nucleosynthesis in the universe [1]. The distribution of 26 Al in the Galaxy has shown a dominant concentration around massive star and supernovae but also a contribution from classical novae.…”

Section: Introductionmentioning

confidence: 99%

High-Precision Proton-Capture Q Values for²⁵Al(p, γ)²⁶Si and³⁰P(p, γ)³¹Si

Cañete¹,

Kankainen²,

Eronen³

et al. 2017

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

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The masses of astrophysically relevant nuclei, 25 Al and 30 P, have recently been measured with the JYFLTRAP double Penning trap at the new IGISOL-4 facility at the University of Jyväskylä. Unparalleled precisions of 63eV and 64eV were achieved for the 25 Al and 30 P masses, respectively. The proton-capture Q values for 25 Al(p,γ) 26 Si and 30 P(p,γ) 31 S were also determined, and their precisions improved by a factor of 4 and 2, respectively, in comparison with AME12. The impact of the more precise values on the resonant proton-capture rate has also been studied.

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“…Nuclei heavier than iron cannot be produced in stars by fusing lighter nuclei; instead, they are synthesized through a sequence of neutron capture reactions on seed nuclei [1]. Regarding 90 A 208 nuclei, a major nucleosynthesis site has been identified in low-mass ( 3M ) asymptotic giant branch (AGB) stars [2], where the presence of a 13 C pocket [3] allows for neutron production through the 13 C(α, n) 16 O reaction.…”

Section: Introductionmentioning

confidence: 99%

“…The 13 C pocket forms after the quenching of the H-burning shell, since protons are mixed downward and quickly captured by 12 C nuclei, eventually leading to the formation of 13 C. Because of the relatively low neutron fluxes generated by the 13 C(α, n) 16 O reaction (on the order of 10 5 to 10 11 neutrons per cm 2 per second), the neutron accretion rate is slower than the β-decay rate, thus only heavy elements along the stability valley can be produced (s-process, s for slow) [4]. At 0.9 10 8 K, a typical temperature characterizing 13 C-burning [5], the energy range where the 13 C(α, n) 16 O reaction is most effective, the Gamow window [1], is ∼ 100 − 270 keV.…”

Section: Introductionmentioning

confidence: 99%

Measurement of the¹³C(α,n)¹⁶O reaction at astrophysical energies using the Trojan Horse Method. Focus on the -3 keV sub-threshold resonance

Cognata

Spitaleri

Trippella

et al. 2014

EPJ Web of Conferences

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Abstract. Most of the nuclei in the mass range 90 A 208 are produced through the so-called s-process, namely through a series of neutron capture reactions on seed nuclei followed by β-decays. The 13 C(α, n) 16 O reaction is the neutron source for the main component of the s-process. It is active inside the helium-burning shell of asymptotic giant branch stars, at temperatures 10 8 K, corresponding to an energy interval of 140 − 230 keV. In this region, the astrophysical S (E)-factor is dominated by the −3 keV sub-threshold resonance due to the 6.356 MeV level in 17 O. Direct measurements could not soundly establish its contribution owing to the cross section suppression at astrophysical energies determined by the Coulomb barrier between interacting nuclei. Indirect measurements and extrapolations yielded inconsistent results, calling for further investigations. The Trojan Horse Method turns out to be very suited for the study of the 13 C(α, n) 16 O reaction as it allows us to access the low as well as the negative energy region, in particular in the case of resonance reactions. We have applied the Trojan Horse Method to the 13 C( 6 Li, n 16 O)d quasi-free reaction. By using the modified R-matrix approach, the asymptotic normalization coefficient (C 17 O(1/2 + ) α 13 C ) 2 of the 6.356 MeV level has been deduced as well as the n-partial width, allowing to attain an unprecedented accuracy for the 13 C(α, n) 16 O astrophysical factor. A preliminary analysis of a partial data set has lead to (C 17 O(1/2 + ) α 13 C ) 2 = 6.7 +0.9 −0.6 fm −1 , slightly larger than the values in the literature, determining a 13 C(α, n) 16 O reaction rate in agreement with the most results in the literature at ∼ 10 8 K, with enhanced accuracy thanks to this innovative approach. a

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Nuclear Physics of Stars

Cited by 317 publications

References 0 publications

New measurements of low-energy resonances in theNe22(p,γ)Na23reaction

New measurements of low-energy resonances in theNe22(p,γ)Na23reaction

High-Precision Proton-Capture Q Values for²⁵Al(p, γ)²⁶Si and³⁰P(p, γ)³¹Si

Measurement of the¹³C(α,n)¹⁶O reaction at astrophysical energies using the Trojan Horse Method. Focus on the -3 keV sub-threshold resonance

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Nuclear Physics of Stars

Cited by 317 publications

References 0 publications

New measurements of low-energy resonances in theNe22(p,γ)Na23reaction

New measurements of low-energy resonances in theNe22(p,γ)Na23reaction

High-Precision Proton-Capture Q Values for25Al(p, γ)26Si and30P(p, γ)31Si

Measurement of the13C(α,n)16O reaction at astrophysical energies using the Trojan Horse Method. Focus on the -3 keV sub-threshold resonance

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High-Precision Proton-Capture Q Values for²⁵Al(p, γ)²⁶Si and³⁰P(p, γ)³¹Si

Measurement of the¹³C(α,n)¹⁶O reaction at astrophysical energies using the Trojan Horse Method. Focus on the -3 keV sub-threshold resonance