NSR Query Results
Output year order : Descending NSR database version of April 27, 2024. Search: Author = E.Napolitani Found 6 matches. 2021BE19 Eur.Phys.J. A 57, 177 (2021) S.Bertoldo, G.Maggioni, W.Raniero, C.Carraro, S.Riccetto, F.Sgarbossa, D.Scarpa, A.Andrighetto, A.Mazzolari, A.Gadea, D.R.Napoli, E.Napolitani, D.De Salvador New method for the production of thin and stable, segmented n+contacts in HPGe detectors
doi: 10.1140/epja/s10050-021-00487-8
2018MA23 Eur.Phys.J. A 54, 34 (2018) G.Maggioni, S.Carturan, W.Raniero, S.Riccetto, F.Sgarbossa, V.Boldrini, R.Milazzo, D.R.Napoli, D.Scarpa, A.Andrighetto, E.Napolitani, D.De Salvador Pulsed laser diffusion of thin hole-barrier contacts in high purity germanium for gamma radiation detectors
doi: 10.1140/epja/i2018-12471-0
2017NA09 Acta Phys.Pol. B48, 387 (2017) D.R.Napoli, G.Maggioni, S.Carturan, J.Eberth, V.Boldrini, D.De Salvador, E.Napolitani, P.Cocconi, G.Della Mea, M.Gelain, R.Gunnella, M.G.Grimaldi, M.Loriggiola, G.Mariotto, N.Pinto, W.Raniero, S.J.Rezvani, S.Riccetto, D.Rosso, F.Sgarbossa, S.Tati New Developments in HPGe Detectors for High Resolution Detection
doi: 10.5506/APhysPolB.48.387
2016BE14 Eur.Phys.J. A 52, 72 (2016) A.Best, A.Caciolli, Zs.Fulop, Gy.Gyurky, M.Laubenstein, E.Napolitani, V.Rigato, V.Roca, T.Szucs Underground nuclear astrophysics: Why and how
doi: 10.1140/epja/i2016-16072-7
2015BR09 Eur.Phys.J. A 51, 94 (2015) C.G.Bruno, D.A.Scott, A.Formicola, M.Aliotta, T.Davinson, M.Anders, A.Best, D.Bemmerer, C.Broggini, A.Caciolli, F.Cavanna, P.Corvisiero, R.Depalo, A.Di Leva, Z.Elekes, Zs.Fulop, G.Gervino, C.J.Griffin, A.Guglielmetti, C.Gustavino, Gy.Gyurky, G.Imbriani, M.Junker, R.Menegazzo, E.Napolitani, P.Prati, E.Somorjai, O.Straniero, F.Strieder, T.Szucs, D.Trezzi, for the LUNA Collaboration Resonance strengths in the 17, 18O(p, α)14, 15N reactions and background suppression underground - Commissioning of a new setup for charged-particle detection at LUNA NUCLEAR REACTIONS 17,18O(p, α), E=151, 193 keV; measured Eα, Iα; deduced resonance strength, energy, thick target yield as a by-product of commissioning of new setup.
doi: 10.1140/epja/i2015-15094-y
2014DI01 Phys.Rev. C 89, 015803 (2014), Erratum Phys.Rev. C 90, 019902 (2014) A.Di Leva, D.A.Scott, A.Caciolli, A.Formicola, F.Strieder, M.Aliotta, M.Anders, D.Bemmerer, C.Broggini, P.Corvisiero, Z.Elekes, Zs.Fulop, G.Gervino, A.Guglielmetti, C.Gustavino, Gy.Gyurky, G.Imbriani, J.Jose, M.Junker, M.Laubenstein, R.Menegazzo, E.Napolitani, P.Prati, V.Rigato, V.Roca, E.Somorjai, C.Salvo, O.Straniero, T.Szucs, F.Terrasi, D.Trezzi Underground study of the 17O(p, γ)18F reaction relevant for explosive hydrogen burning NUCLEAR REACTIONS 17O(p, γ)18F, E(cm)=160-370 keV; measured Eγ, Iγ, on- and off-resonance γ spectra, γ-branching ratios from decay of resonances, half-life using activation method at underground LUNA accelerator at Gran Sasso National Laboratory; deduced S factors for secondary transitions, total S factor, resonance strength, astrophysical S factor and reaction rates. 18F; deduced levels, analysis of astrophysically important 183-keV resonance. Comparison with previous experimental results. 15N, 18,19F, 18O; evaluated abundances by Nova model calculations. RADIOACTIVITY 18F(β+)[from 17O(p, γ), E(cm)=160-370 keV]; measured Eγ, Iγ, half-life.
doi: 10.1103/PhysRevC.89.015803
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