Improved astrophysical rate for the 18O(p,α)15N reaction by underground measurements

Bruno, Carlo; Aliotta, M.; Descouvemont, Pierre; Best, A.; Davinson, T.; Bemmerer, D.; Boeltzig, A.; Broggini, C.; Caciolli, A.; Cavanna, F.; Chillery, T.; Ciani, G. F.; Corvisiero, P.; Depalo, R.; Leva, A. Di; Elekes, Z.; Ferraro, F.; Formicola, A.; Fülöp, Zs.; Gervino, G.; Guglielmetti, A.; Gustavino, C.; Gyürky, Gy.; Imbriani, G.; Junker, M.; Lugaro, Maria; Marigo, Paola; Menegazzo, R.; Mossa, V.; Pantaleo, F. R.; Piatti, D.; Prati, P.; Stöckel, K.; Straniero, O.; Strieder, F.; Szücs, T.; Takács, M. P.; Trezzi, D.

doi:10.1016/j.physletb.2019.01.017

Cited by 28 publications

(38 citation statements)

References 36 publications

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“…Both fits are excellent, with common parameters (energies and proton widths of resonances). The new data set (Bruno et al, 2019) suggest a new resonance at E cm = 110 keV.…”

Section: Applications Of the R-matrix Methodsmentioning

confidence: 87%

“…Some examples are 14 N(p,γ ) 15 O (Li et al, 2016) or 13 C(p, γ ) 14 N (Chakraborty et al, 2015). Here we discuss in more detail a recent R-matrix analysis of the 18 O(p,α) 15 N cross section which has been measured in the underground laboratory of the Gran Sasso (LUNA) (Bruno et al, 2019). This reaction influences the abundances of 15 N, 18 O and 19 F isotopes, critical to constrain a wide variety of stellar models.…”

Section: Applications Of the R-matrix Methodsmentioning

confidence: 99%

“…For the latter two resonances, results on their energy and partial widths are inconsistent (La Cognata et al, 2008), and important differences have also been reported between the cross sections of different datasets at low energies. The main goal of Bruno et al (2019) was to measure the non-resonant component of the cross section of the 18 O(p,α) 15 N reaction at proton beam energies from E p = 360 to 60 keV, extending the range of direct measurements to stellar energies. From the cross section measurements, the strength of resonances of astrophysical interest could be determined.…”

Section: Applications Of the R-matrix Methodsmentioning

confidence: 99%

“…The red dashed lined in the inset shows the effect of removing the new state at E = 106 keV. Reprinted fromBruno et al (2019) with permission from Elsevier.…”

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confidence: 99%

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Nuclear Reactions of Astrophysical Interest

Descouvemont

2020

Front. Astron. Space Sci.

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We present different reaction models commonly used in nuclear astrophysics, in particular for the nucleosynthesis of the light elements. Nuclear reactions involved in stellar evolution generally occur at energies much lower than the Coulomb barrier. This property makes the cross sections extremely small, and virtually impossible to be measured in the laboratory. We start with a general discussion of low-energy scattering, and define the various cross sections required for reaction networks (essentially radiative capture and transfer reactions). Then we present specific models. Microscopic theories are based on fundamental principles, such as a nucleon-nucleon interaction, and an exact account of the antisymmetrization between all nucleons. In this context, most calculations performed so far have been done in the cluster approximation, but recent works, referred to as "ab initio" models, go beyond this approximation. Microscopic models can be simplified by neglecting the internal structure of the colliding nuclei, which leads to the potential model, also named the optical model. An alternative approach for the theoretical analysis of the experimental data is based on the phenomenological R-matrix theory, where parameters are fitted to the existing data, and then used to extrapolate the cross sections down to stellar energies. Indirect approaches, such as the Trojan Horse method, are briefly outlined. Finally, we present some typical applications of the different models.

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“…Both fits are excellent, with common parameters (energies and proton widths of resonances). The new data set (Bruno et al, 2019) suggest a new resonance at E cm = 110 keV.…”

Section: Applications Of the R-matrix Methodsmentioning

confidence: 87%

Section: Applications Of the R-matrix Methodsmentioning

confidence: 99%

Section: Applications Of the R-matrix Methodsmentioning

confidence: 99%

“…The red dashed lined in the inset shows the effect of removing the new state at E = 106 keV. Reprinted fromBruno et al (2019) with permission from Elsevier.…”

mentioning

confidence: 99%

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Nuclear Reactions of Astrophysical Interest

Descouvemont

2020

Front. Astron. Space Sci.

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“…As already widely discussed in section 1, even if the cross section of the 18 O(p, α) 15 N reaction has been the subject of several experimental investigations in the past, several issues concern the 20 keV resonance. Recently, the work of Bruno et al (2019) supplied a new direct measurement of the 18 O(p, α) 15 N cross section. The authors used the thick target technique to come close to the energy region of astrophysical interest and perform the spectroscopy of 19 F. Though the 20 keV state could not be observed, the authors reported a factor of 10 larger strength for the 90 keV resonance reaching about 1.6 µeV, with respect to existing measurements (Lorenz-Wirzba et al, 1979;La Cognata et al, 2008a, 2010a.…”

Section: The 18 O(p α) 15 N Reactionmentioning

confidence: 99%

Indirect Measurements of n- and p-Induced Reactions of Astrophysical Interest on Oxygen Isotopes

Sergi

Guardo

Cognata

et al. 2020

Front. Astron. Space Sci.

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Nuclear Reactions in Evolving Stars (and Their Theoretical Prediction)

Thielemann

Rauscher

2023

Handbook of Nuclear Physics

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This chapter will go through the important nuclear reactions in stellar evolution and explosions, passing through the individual stellar burning stages and also explosive burning conditions. To follow the changes in the composition of nuclear abundances requires the knowledge of the relevant nuclear reaction rates. For light nuclei (entering in early stellar burning stages) the resonance density is generally quite low and the reactions are determined by individual resonances, which are best obtained from experiments. For intermediate mass and heavy nuclei the level density is typically sufficient to apply statistical model approaches. For this reason, while we discuss all burning stages and explosive burning, focusing on the reactions of importance, we will for light nuclei refer to the chapters by M. Wiescher, deBoer & Reifarth (Experimental Nuclear Astrophysics) and P. Descouvement (Theoretical Studies of Low-Energy Nuclear Reactions), which display many examples, experimental methods utilized, and theoretical approaches how to predict nuclear reaction rates for light nuclei. For nuclei with sufficiently high level densities we discuss statistical model methods used in present predictions of nuclear reaction cross sections and thermonuclear rates across the nuclear chart, including also the application to nuclei far from stability and fission modes.

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Improved astrophysical rate for the 18O(p,α)15N reaction by underground measurements

Cited by 28 publications

References 36 publications

Nuclear Reactions of Astrophysical Interest

Nuclear Reactions of Astrophysical Interest

Indirect Measurements of n- and p-Induced Reactions of Astrophysical Interest on Oxygen Isotopes

Nuclear Reactions in Evolving Stars (and Their Theoretical Prediction)

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