13 results on '"Bruno, C. G."'
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2. Retraction Note: Direct measurements of the 12C + 12C reactions cross-sections towards astrophysical energies
- Author
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Morales-Gallegos, L., primary, Aliotta, M., additional, Gialanella, L., additional, Best, A., additional, Bruno, C. G., additional, Buompane, R., additional, Davinson, T., additional, De Cesare, M., additional, Di Leva, A., additional, D’Onofrio, A., additional, Duarte, J. G., additional, Gasques, L. R., additional, Imbriani, G., additional, Porzio, G., additional, Rapagnani, D., additional, Romoli, M., additional, and Terrasi, F., additional
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- 2023
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3. First direct limit on the 334 keV resonance strength in $$^{22}$$Ne($$\alpha $$,$$\gamma $$)$$^{26}$$Mg reaction
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Piatti, D., primary, Masha, E., additional, Aliotta, M., additional, Balibrea-Correa, J., additional, Barile, F., additional, Bemmerer, D., additional, Best, A., additional, Boeltzig, A., additional, Broggini, C., additional, Bruno, C. G., additional, Caciolli, A., additional, Cavanna, F., additional, Chillery, T., additional, Ciani, G. F., additional, Compagnucci, A., additional, Corvisiero, P., additional, Csedreki, L., additional, Davinson, T., additional, Depalo, R., additional, Leva, A. di, additional, Elekes, Z., additional, Ferraro, F., additional, Fiore, E. M., additional, Formicola, A., additional, Fülöp, Zs., additional, Gervino, G., additional, Guglielmetti, A., additional, Gustavino, C., additional, Gyürky, Gy., additional, Imbriani, G., additional, Junker, M., additional, Lugaro, M., additional, Marigo, P., additional, Menegazzo, R., additional, Mossa, V., additional, Pantaleo, F. R., additional, Paticchio, V., additional, Perrino, R., additional, Prati, P., additional, Rapagnani, D., additional, Schiavulli, L., additional, Skowronski, J., additional, Stöckel, K., additional, Straniero, O., additional, Szücs, T., additional, Takács, M. P., additional, and Zavatarelli, S., additional
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- 2022
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4. Direct measurements of the $$^{12}$$C+$$^{12}$$C reactions cross-sections towards astrophysical energies
- Author
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Morales-Gallegos, L., primary, Aliotta, M., additional, Gialanella, L., additional, Best, A., additional, Bruno, C. G., additional, Buompane, R., additional, Davinson, T., additional, De Cesare, M., additional, Di Leva, A., additional, D’Onofrio, A., additional, Duarte, J. G., additional, Gasques, L. R., additional, Imbriani, G., additional, Porzio, G., additional, Rapagnani, D., additional, Romoli, M., additional, and Terrasi, F., additional
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- 2022
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5. Setup commissioning for an improved measurement of the D(p,$$\gamma $$)$$^3$$He cross section at Big Bang Nucleosynthesis energies
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Mossa, V., primary, Stöckel, K., additional, Cavanna, F., additional, Ferraro, F., additional, Aliotta, M., additional, Barile, F., additional, Bemmerer, D., additional, Best, A., additional, Boeltzig, A., additional, Broggini, C., additional, Bruno, C. G., additional, Caciolli, A., additional, Csedreki, L., additional, Chillery, T., additional, Ciani, G. F., additional, Corvisiero, P., additional, Davinson, T., additional, Depalo, R., additional, Di Leva, A., additional, Elekes, Z., additional, Fiore, E. M., additional, Formicola, A., additional, Fülöp, Zs., additional, Gervino, G., additional, Guglielmetti, A., additional, Gustavino, C., additional, Gyürky, G., additional, Imbriani, G., additional, Junker, M., additional, Kochanek, I., additional, Lugaro, M., additional, Marcucci, L. E., additional, Marigo, P., additional, Masha, E., additional, Menegazzo, R., additional, Pantaleo, F. R., additional, Paticchio, V., additional, Perrino, R., additional, Piatti, D., additional, Prati, P., additional, Schiavulli, L., additional, Straniero, O., additional, Szücs, T., additional, Takács, M. P., additional, Trezzi, D., additional, Zavatarelli, S., additional, and Zorzi, G., additional
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- 2020
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6. A new approach to monitor $$^{13}\hbox {C}$$-targets degradation in situ for $$^{13}\hbox {C}(\alpha ,\hbox {n})^{16}\hbox {O}$$ cross-section measurements at LUNA
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Ciani, G. F., primary, Csedreki, L., additional, Balibrea-Correa, J., additional, Best, A., additional, Aliotta, M., additional, Barile, F., additional, Bemmerer, D., additional, Boeltzig, A., additional, Broggini, C., additional, Bruno, C. G., additional, Caciolli, A., additional, Cavanna, F., additional, Chillery, T., additional, Colombetti, P., additional, Corvisiero, P., additional, Davinson, T., additional, Depalo, R., additional, Di Leva, A., additional, Di Paolo, L., additional, Elekes, Z., additional, Ferraro, F., additional, Fiore, E. M., additional, Formicola, A., additional, Fülöp, Zs., additional, Gervino, G., additional, Guglielmetti, A., additional, Gustavino, C., additional, Gyürky, Gy., additional, Imbriani, G., additional, Junker, M., additional, Kochanek, I., additional, Lugaro, M., additional, Marigo, P., additional, Masha, E., additional, Menegazzo, R., additional, Mossa, V., additional, Pantaleo, F. R., additional, Paticchio, V., additional, Perrino, R., additional, Piatti, D., additional, Prati, P., additional, Schiavulli, L., additional, Stöckel, K., additional, Straniero, O., additional, Szücs, T., additional, Takács, M. P., additional, Terrasi, F., additional, Trezzi, D., additional, and Zavatarelli, S., additional
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- 2020
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7. Development of a two-stage detection array for low-energy light charged particles in nuclear astrophysics applications
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Romoli, M., primary, Morales-Gallegos, L., additional, Aliotta, M., additional, Bruno, C. G., additional, Buompane, R., additional, D’Onofrio, A., additional, Davinson, T., additional, De Cesare, M., additional, Di Leva, A., additional, Di Meo, P., additional, Duarte, J., additional, Gasques, L., additional, Gialanella, L., additional, Imbriani, G., additional, Porzio, G., additional, Rapagnani, D., additional, and Vanzanella, A., additional
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- 2018
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8. Reduction of deuterium content in carbon targets for 12C + 12C reaction studies of astrophysical interest
- Author
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Morales-Gallegos, L., primary, Aliotta, M., additional, Bruno, C. G., additional, Buompane, R., additional, Davinson, T., additional, De Cesare, M., additional, Di Leva, A., additional, D’Onofrio, A., additional, Duarte, J. G., additional, Gasques, L. R., additional, Gialanella, L., additional, Imbriani, G., additional, Porzio, G., additional, Rapagnani, D., additional, Romoli, M., additional, Schürmann, D., additional, Terrasi, F., additional, and Zhang, L. Y., additional
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- 2018
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9. Shell and explosive hydrogen burning
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Boeltzig, A., primary, Bruno, C. G., additional, Cavanna, F., additional, Cristallo, S., additional, Davinson, T., additional, Depalo, R., additional, deBoer, R. J., additional, Di Leva, A., additional, Ferraro, F., additional, Imbriani, G., additional, Marigo, P., additional, Terrasi, F., additional, and Wiescher, M., additional
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- 2016
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10. Direct measurements of the $$^{12}$$C+$$^{12}$$C reactions cross-sections towards astrophysical energies
- Author
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L. Morales-Gallegos, M. Aliotta, L. Gialanella, A. Best, C. G. Bruno, R. Buompane, T. Davinson, M. De Cesare, A. Di Leva, A. D’Onofrio, J. G. Duarte, L. R. Gasques, G. Imbriani, G. Porzio, D. Rapagnani, M. Romoli, F. Terrasi, Morales-Gallegos, L., Aliotta, M., Gialanella, L., Best, A., Bruno, C. G., Buompane, R., Davinson, T., De Cesare, M., Di Leva, A., D'Onofrio, A., Duarte, J. G., Gasques, L. R., Imbriani, G., Porzio, G., Rapagnani, D., Romoli, M., and Terrasi, F.
- Subjects
Nuclear and High Energy Physics ,Experimental Nuclear Astrophysics Carbon burning in stars ,ASTROFÍSICA - Abstract
Carbon fusion reactions $$^{12}$$ 12 C($$^{12}$$ 12 C,p)$$^{23}$$ 23 Na and $$^{12}$$ 12 C($$^{12}$$ 12 C,$$\alpha $$ α )$$^{20}$$ 20 Ne play a key role in the evolution of massive stars and in explosive scenarios such as type-Ia supernovae and super-bursts in binary stars. A direct determination of their cross sections is extremely challenging and discrepancies exist between different data sets in the literature. Here we report the results of a direct measurement performed at the CIRCE Tandem Accelerator Laboratory in Caserta (Italy), using $$\varDelta E-E$$ Δ E - E detectors for unambiguous charge identification. Cross sections were measured in the energy range $$E_{\mathrm{c.m.}} =2.51{-}4.36$$ E c . m . = 2.51 - 4.36 MeV with energy steps between 10 and 25 keV in the centre of mass. To our knowledge these represent the finest energy steps to date. Results are presented in the form of partial and summed astrophysical $${\tilde{S}}$$ S ~ -factors for individual proton- and $$\alpha $$ α -particle channels. Branching ratios of individual proton- and $$\alpha $$ α -particle groups were found to vary significantly with energy. Angular distributions, albeit limited to three angles, were also found to be non-isotropic, which could be a potential explanation for the discrepancies observed among different data sets. Further efforts are ongoing to extend measurements to lower energies.
- Published
- 2022
11. Reduction of deuterium content in carbon targets for 12C + 12C reaction studies of astrophysical interest
- Author
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Raffaele Buompane, J. G. Duarte, A. Di Leva, L Y Zhang, Thomas Davinson, Gianluca Imbriani, Antonio D'Onofrio, Lucio Gialanella, G. Porzio, D. Rapagnani, Leandro Gasques, L. Morales-Gallegos, C. G. Bruno, D Schurmann, Marialuisa Aliotta, Filippo Terrasi, M. De Cesare, M. Romoli, Morales-Gallegos, L., Aliotta, M., Bruno, C. G., Buompane, R., Davinson, T., De Cesare, M., Di Leva, A., D’Onofrio, A., Duarte, J. G., Gasques, L. R., Gialanella, L., Imbriani, G., Porzio, G., Rapagnani, D., Romoli, M., Schürmann, D., Terrasi, F., Zhang, L. Y., Aliotta, M, T., Davinson, Leva, Di, D'Onofrio, A., G., Imbriani, Schurmann, D., Zhang, And, and Y., L.
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Physics ,Nuclear and High Energy Physics ,Hydrogen ,chemistry.chemical_element ,Atmospheric temperature range ,01 natural sciences ,Deuterium ,chemistry ,0103 physical sciences ,Content (measure theory) ,Nuclear and High Energy Physics, Particle detection, Nuclear astrophysics, nuclear fusion ,Nuclear fusion ,Pyrolytic carbon ,Atomic physics ,010306 general physics ,010303 astronomy & astrophysics ,Carbon ,Stellar evolution - Abstract
The 12C(12C,p)23Na and 12C(12C, $\alpha$ )20Ne fusion reactions are among the most important in stellar evolution since they determine the destiny of massive ( $ M \simeq 8-10 M_{\odot}$ ) stars. However, experimental low-energy investigations of such reactions are significantly hampered by ubiquitous natural hydrogen and deuterium contaminants in the carbon targets. The associated beam-induced background completely masks the reaction products of interest thus preventing cross-section measurements at the relevant energies of astrophysical interest, $E_{\mathrm{cm}} < 2$ MeV. In this work, we report about an investigation aimed at assessing possible deuterium reductions on both natural graphite and Highly Ordered Pyrolytic Graphite targets as a function of target temperature. Our results indicate that reductions up to about 80% can be attained on both targets in the temperature range investigated, $ T \simeq 200-1200 {}^{\circ}$ C. A further reduction by a factor of 2.5 in absolute deuterium content is observed when the scattering chamber is surrounded by a dry nitrogen atmosphere so as to minimise light-particles uptake within the chamber rest gas (and thus on target) through air leaks. The results from this study will inform the choice of optimal experimental conditions and procedures for improved measurements of the 12C + 12C reactions cross-sections at the low energies of astrophysical interest.
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- 2018
12. Shell and explosive hydrogen burning
- Author
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A. Di Leva, Thomas Davinson, Gianluca Imbriani, A. Boeltzig, F. Ferraro, Sergio Cristallo, C. G. Bruno, Richard deBoer, F. Cavanna, Filippo Terrasi, Michael Wiescher, Paola Marigo, R. Depalo, Boeltzig, A., Bruno, C. G., Cavanna, F., Cristallo, S., Davinson, T., Depalo, R., Deboer, R. J., Di Leva, A., Ferraro, F., Imbriani, G., Marigo, P., Terrasi, Filippo, Wiescher, M., ITA, and USA
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Nuclear reaction ,Physics ,Nuclear and High Energy Physics ,Hydrogen ,010308 nuclear & particles physics ,Red giant ,chemistry.chemical_element ,Astrophysics ,01 natural sciences ,7. Clean energy ,Stars ,chemistry ,Nucleosynthesis ,0103 physical sciences ,Asymptotic giant branch ,Nuclide ,010303 astronomy & astrophysics ,Helium - Abstract
The nucleosynthesis of light elements, from helium up to silicon, mainly occurs in Red Giant and Asymptotic Giant Branch stars and Novae. The relative abundances of the synthesized nuclides critically depend on the rates of the nuclear processes involved, often through non-trivial reaction chains, combined with complex mixing mechanisms. In this review, we summarize the contributions made by LUNA experiments in furthering our understanding of nuclear reaction rates necessary for modeling nucleosynthesis in AGB stars and Novae explosions.
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- 2016
13. First direct limit on the 334 keV resonance strength in $$^{22}$$Ne($$\alpha $$,$$\gamma $$)$$^{26}$$Mg reaction
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D. Piatti, E. Masha, M. Aliotta, J. Balibrea-Correa, F. Barile, D. Bemmerer, A. Best, A. Boeltzig, C. Broggini, C. G. Bruno, A. Caciolli, F. Cavanna, T. Chillery, G. F. Ciani, A. Compagnucci, P. Corvisiero, L. Csedreki, T. Davinson, R. Depalo, A. di Leva, Z. Elekes, F. Ferraro, E. M. Fiore, A. Formicola, Zs. Fülöp, G. Gervino, A. Guglielmetti, C. Gustavino, Gy. Gyürky, G. Imbriani, M. Junker, M. Lugaro, P. Marigo, R. Menegazzo, V. Mossa, F. R. Pantaleo, V. Paticchio, R. Perrino, P. Prati, D. Rapagnani, L. Schiavulli, J. Skowronski, K. Stöckel, O. Straniero, T. Szücs, M. P. Takács, S. Zavatarelli, Piatti, D., Masha, E., Aliotta, M., Balibrea-Correa, J., Barile, F., Bemmerer, D., Best, A., Boeltzig, A., Broggini, C., Bruno, C. G., Caciolli, A., Cavanna, F., Chillery, T., Ciani, G. F., Compagnucci, A., Corvisiero, P., Csedreki, L., Davinson, T., Depalo, R., di Leva, A., Elekes, Z., Ferraro, F., Fiore, E. M., Formicola, A., F??l??p, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Gy??rky, Gy., Imbriani, G., Junker, M., Lugaro, M., Marigo, P., Menegazzo, R., Mossa, V., Pantaleo, F. R., Paticchio, V., Perrino, R., Prati, P., Rapagnani, D., Schiavulli, L., Skowronski, J., St??ckel, K., Straniero, O., Sz??cs, T., Tak??cs, M. P., and Zavatarelli, S.
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Nuclear and High Energy Physics ,Evolution ,nuclear astrophysics ,S-Process Nucleosynthesis ,FOS: Physical sciences ,Magnesium Isotopes ,Reaction-Rates ,AGB and post-AGB [abundances – Stars] ,AGB-Stars ,Nuclear Astrophysics ,MG Isotopic-Ratios ,Massive Stars ,nuclear astrophysics, detectors, neon ,Abundances ,Nuclear reactions ,neon ,giant branch stars ,Nuclear Experiment (nucl-ex) ,Nuclear Experiment ,Nucleosynthesis ,detectors - Abstract
In stars, the fusion of $^{22}$Ne and $^4$He may produce either $^{25}$Mg, with the emission of a neutron, or $^{26}$Mg and a $\gamma$ ray. At high temperature, the ($\alpha,n$) channel dominates, while at low temperature, it is energetically hampered. The rate of its competitor, the $^{22}$Ne($\alpha$,$\gamma$)$^{26}$Mg reaction, and, hence, the minimum temperature for the ($\alpha,n$) dominance, are controlled by many nuclear resonances. The strengths of these resonances have hitherto been studied only indirectly. The present work aims to directly measure the total strength of the resonance at $E$_{r}$\,=\,$334$\,$keV (corresponding to $E$_{x}$\,=\,$10949$\,$keV in $^{26}$Mg). The data reported here have been obtained using high intensity $^4$He$^+$ beam from the INFN LUNA 400 kV underground accelerator, a windowless, recirculating, 99.9% isotopically enriched $^{22}$Ne gas target, and a 4$\pi$ bismuth germanate summing $\gamma$-ray detector. The ultra-low background rate of less than 0.5 counts/day was determined using 67 days of no-beam data and 7 days of $^4$He$^+$ beam on an inert argon target. The new high-sensitivity setup allowed to determine the first direct upper limit of 4.0$\,\times\,$10$^{-11}$ eV (at 90% confidence level) for the resonance strength. Finally, the sensitivity of this setup paves the way to study further $^{22}$Ne($\alpha$,$\gamma$)$^{26}$Mg resonances at higher energy., Comment: Submitted to Eur. Phys. J. A
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