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Leva, A. Di; Scott, D. A.; Caciolli, A.; Formicola, A.; Strieder, F.; Aliotta, M.; Anders, M.; Bemmerer, D.; Broggini, C.; Corvisiero, P.; Elekes, Z.; Fülöp, Zs.; Gervino, G.; Guglielmetti, A.; Gustavino, C.; Gyürky, Gy.; Imbriani, G.; José, J.; Junker, M.; Laubenstein, M.; Menegazzo, R.; Napolitani, E.; Prati, P.; Rigato, V.; Roca, V.; Somorjai, E.; Salvo, C.; Straniero, O.; Szücs, T.; Terrasi, F.; Trezzi, D.

doi:10.1103/physrevc.90.019902

Cited by 19 publications

(56 citation statements)

References 1 publication

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“…The results are in perfect agreement reducing considerably the systematics [39]. New results on the non resonant component and on the 183.3 keV resonance have been obtained (ωγ = (1.67 ± 0.12)µeV [39,40]) reducing the uncertainties of isotopes production in nova explosion models to a 10% level [40]. The very low uncertainty obtained in this experiment was possible thank to an intensive study of the target, realised and tested directly by the LUNA group with ion beam analysis and secondary induced mass spectroscopy techniques [41].…”

Section: The Other Cno Cyclessupporting

confidence: 69%

Nuclear Astrophysics in underground laboratories: the LUNA experiment

Simpson¹,

Simenel²,

Cook³

et al. 2017

EPJ Web Conf.

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Abstract. One of the main ingredients of nuclear astrophysics is the knowledge of the thermonuclear reactions responsible for powering the stellar engine and for the synthesis of the chemical elements. At astrophysical energies the cross section of nuclear processes is extremely reduced by the effect of the Coulomb barrier. The low value of cross sections prevents their measurement at stellar energies on Earth surface and often extrapolations are needed. The Laboratory for Underground Nuclear Astrophysics (LUNA) is placed under the Gran Sasso mountain and thanks to the cosmic-ray background reduction provided by its position can investigate cross sections at energies close to the Gamow peak in stellar scenarios. Many crucial reactions involved in hydrogen burning has been measured directly at astrophysical energies with both the LUNA-50kV and the LUNA-400kV accelerators, and this intense work will continue with the installation of a MV machine able to explore helium and carbon burnings. Based on this progress, currently there are efforts in several countries to construct new underground accelerators. In this talk, the typical techniques adopted in underground nuclear astrophysics will be described and the most relevant results achieved by LUNA will be reviewed. The exciting science that can be probed with the new facilities will be highlighted.

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Section: The Other Cno Cyclessupporting

confidence: 69%

Nuclear Astrophysics in underground laboratories: the LUNA experiment

Simpson¹,

Simenel²,

Cook³

et al. 2017

EPJ Web Conf.

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show abstract

“…The reaction rate uncertainty attained is now below the required precision for nova models. We verified, following a full set of hydrodynamic nova models, that the abundances of oxygen and fluorine isotopes obtained with the present reaction rate are determined with 10% precision and put firmer constraints on observational signatures of novae events [8].…”

Section: Thementioning

confidence: 97%

“…The reaction has been measured in the energy range E cm = 160 − 370 keV and the resonance strength of the 183 keV resonance determined with unprecedented precision to be ω γ = (1.67 ± 0.12) μeV [7,8]. The contribution of Eugene Wigner in this field is very relevant, especially for what concerns the description of the resonance strength.…”

Section: Thementioning

confidence: 99%

The LUNA experiment at Gran Sasso Laboratory

Guglielmetti

2014

EPJ Web of Conferences

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Abstract. Accurate knowledge of thermonuclear reaction rates is a key issue in nuclear astrophysics since it is important for understanding the energy generation, neutrino production and the synthesis of the elements in stars. Cross-section measurements are mainly hampered by the very low counting rate and cosmic background. An underground location is extremely advantageous for such studies, as demonstrated by the LUNA experiment in the Gran Sasso Laboratory (Italy). This paper reports on the results recently obtained by such an experiment and on the future perspectives in this field.

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“…Thanks to the most recent results of Iliadis et al (2010) [21] and of Di Leva et al (2014) [28], the (p,α) and (p,γ) THM rates will be evaluated.…”

Section: B State Of the Artmentioning

confidence: 99%

“…For the E R =183 keV resonance, the weighted average values of the energies and strengths measured by [12,25,26] were adopted. For the higher energy resonances above E R =500 keV, the partial widths have been adopted from the R-matrix analysis (see Table 3 of [24] [27] and Di Leva et al (2014) [28]. In these studies, the reaction cross section has been measured directly in a wide energy range, E cm =200-370 keV, appropriate for hydrogen burning in classical novae.…”

Section: B State Of the Artmentioning

confidence: 99%