The Trojan Horse Method in nuclear astrophysics

Spitaleri, C.; Mukhamedzhanov, A. M.; Blokhintsev, L.D.; Cognata, M. La; Pizzone, R. G.; Туміно, А.

doi:10.1134/s1063778811110184

Cited by 101 publications

(107 citation statements)

References 67 publications

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“…A clear agreement is present both with the other experimental data as well as with the curve which represents the best fit to the function reported in [35]. The next step is to apply the standard procedure of the THM, as discussed in [24], to extract the energy trend of the S(E)-factor. Therefore equation 3 is applied allowing the extraction of the binary cross section from the measured three-body one.…”

Section: Data Analysis and Resultsmentioning

confidence: 59%

“…Many tests have been made to fully explore the potentiality of the method and extend as much as possible its applications: the target/projectile break-up invariance [18], the spectator invariance [19,20] and the possible use of virtual neutron beams [21,22]. Such studies are necessary, as the Trojan Horse method has become one of the major tools for the investigation of reactions of astrophysical interest (for recent reviews see [23,24]). In recent works [19,20] the spectator invariance was extensively examined for the 6 Li( 6 Li,αα) 4 He and the 6 Li( 3 He,αα)H case as well as the 7 Li(d,αα)n and 7 Li( 3 He,αα) 2 H reactions, thus comparing results arising from 6 Li and 3 He and deuteron and 3 He break-up respectively [20].…”

Section: Introductionmentioning

confidence: 99%

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Updated evidence of the Trojan horse particle invariance for the2H(d,p)3H reaction

Pizzone

Spitaleri²,

Bertulani³

et al. 2013

Phys. Rev. C

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Section: Data Analysis and Resultsmentioning

confidence: 59%

Section: Introductionmentioning

confidence: 99%

Updated evidence of the Trojan horse particle invariance for the2H(d,p)3H reaction

Pizzone

Spitaleri²,

Bertulani³

et al. 2013

Phys. Rev. C

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“…= 7 MeV. We aimed to determine the excitation function of the most major products, α+ 28 Si and p+ 31 P, of the 16 O+ 16 O reaction at stellar energies by the Trojan horse method (THM) [7].…”

Section: Abstract: Oxygen Burning Fusion Reaction Trojan Horse Methodsmentioning

confidence: 99%

“…2, which evinces the 16 O( 20 Ne, αα) 28 Si reaction. Momentum distribution |ϕ(p s )| 2 can be determined by the following relations [7];…”

Section: Abstract: Oxygen Burning Fusion Reaction Trojan Horse Methodsmentioning

confidence: 99%

Trojan Horse Method for the Oxygen-Burning Process Reactions

Hayakawa¹,

Spitaleri²,

Burtebayev³

et al. 2017

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

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The 16 O + 16 O fusion reaction is important in terms of the explosive oxygen burning process during late evolution stage of massive stars as well as understanding of the mechanism of low-energy heavyion fusion reactions. The astrophysical S factor of such a heavy-ion fusion strongly depends on energy at corresponding stellar temperatures. For the 16 O + 16 O reaction cross section, there are larger discrepancies among different experimental data as the energy decreases, and a complete lack of data below E c.m. = 7 MeV. We aim to determine the cross sections for the two main exit channels, α + 28 Si and p + 31 P, toward stellar energies. The measurements were performed indirectly by the Trojan horse method (THM) via the 16 O( 20 Ne, αα) 28 Si and 16 O( 20 Ne, pα) 31 P three-body reactions, respectively. We performed measurements twice using 20 Ne beams at Heavy Ion Laboratory (E 20Ne = 45 MeV) and at Gumilyov Eurasian National University (E 20Ne = 35 MeV). We discuss the applicability of the THM to such a heavy nuclear system showing preliminary results of the momentum distribution of α-16 O intercluster motion in the TH nucleus 20 Ne observed for the first time, which implies a possibility of a multi-step breakup of the TH nucleus. KEYWORDS: Oxygen burning, fusion reaction, Trojan horse methodThe 16 O+ 16 O fusion reaction is important in terms of the explosive oxygen burning process during late evolution stage of massive stars as well as understanding of the mechanism of heavy-ion fusion reactions at low energies. The astrophysical S factor of such a heavy-ion fusion strongly depends on energy at corresponding stellar temperatures far below the Coulomb barrier. There are large discrepancies among different experiments [1][2][3][4], and among theoretical predictions [5,6], and is a lack of data below E c.m. = 7 MeV. We aimed to determine the excitation function of the most major products, α+ 28 Si and p+ 31 P, of the 16 O+ 16 O reaction at stellar energies by the Trojan horse method (THM) [7].We

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“…The contribution from a broad resonance (a 1/2 + excited state of 17 O) close to the reaction threshold still remains a debated problem. The ASFIN collaboration performed measurements via the indirect Trojan Horse Method (THM) [3], through the 13 C( 6 Li,n 16 O)d reaction in quasi-free kinematical conditions, where the deuteron inside the 6 Li beam is a spectator in the three-body reaction [4,5]. In order to derive the S (E) factor free of effects from Coulomb suppression and electron screening, the asymptotic normalization coefficient (ANC) of the mentioned resonance was extracted [4,5].…”

Section: O Reactionmentioning

confidence: 99%

The ¹³C Neutron Source and s-Processing in AGB Stars

Trippella¹,

Busso²,

Palmerini³

et al. 2017

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

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The main component of the s-process accounts for about 50% of elements heavier than Kr, through n-captures occurring in asymptotic giant branch (AGB) stars, where the 13 C(α,n) 16 O reaction is the main neutron source. Its activation below the convective envelope at third dredge-up (TDU) and its efficiency are still matters of debate, as: (i) the astrophysical factor is affected by a broad resonance near the reaction threshold and (ii) mixing mechanisms to locally produce 13 C were so far mimicked mainly parametrically. We discuss both problems and, in particular, we adopt one of the recent model proposed for producing 13 C and based on an exact multi-D analytical solution of MHD equations, where magnetic buoyancy induces partial mixing at the envelope border. The resulting distribution of 13 C is used, together with our upgraded prescription for the reaction rate, to reproduce solar abundances through AGB models. It can account for the chemical evolution of s-elements and for the s/(C/O) ratios in low-metallicity post-AGB stars.

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The Trojan Horse Method in nuclear astrophysics

Cited by 101 publications

References 67 publications

Updated evidence of the Trojan horse particle invariance for the2H(d,p)3H reaction

Updated evidence of the Trojan horse particle invariance for the2H(d,p)3H reaction

Trojan Horse Method for the Oxygen-Burning Process Reactions

The ¹³C Neutron Source and s-Processing in AGB Stars

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The Trojan Horse Method in nuclear astrophysics

Cited by 101 publications

References 67 publications

Updated evidence of the Trojan horse particle invariance for the2H(d,p)3H reaction

Updated evidence of the Trojan horse particle invariance for the2H(d,p)3H reaction

Trojan Horse Method for the Oxygen-Burning Process Reactions

The 13C Neutron Source and s-Processing in AGB Stars

Contact Info

Product

Resources

About

The ¹³C Neutron Source and s-Processing in AGB Stars