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12 results on '"R. Depalo"'

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

Author

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

Subjects
Nuclear and High Energy Physics, Astrophysics, 01 natural sciences, 7. Clean energy, Hydrostatic stellar nucleosynthesis, Nucleosynthesis, Stellar hydrogen burningHydrostatic stellar nucleosynthesis, 0103 physical sciences, Nuclear astrophysics, Asymptotic giant branch, 010306 general physics, Stellar hydrogen burning, Hydrostatic stellar nucleosynthesi, Physics, Isotope, 010308 nuclear & particles physics, Resonance, Atmospheric temperature range, Physique atomique et nucléaire, lcsh:QC1-999, Stars, 13. Climate action, Center of mass, Stellar hydrogen burning, Hydrostatic stellar nucleosynthesis, lcsh:Physics
Abstract

The 18O(p,α)15N reaction affects the synthesis of 15N, 18O and 19F isotopes, whose abundances can be used to probe the nucleosynthesis and mixing processes occurring deep inside asymptotic giant branch (AGB) stars. We performed a low-background direct measurement of the 18O(p,α)15N reaction cross-section at the Laboratory for Underground Nuclear Astrophysics (LUNA) from center of mass energy Ec.m.=340 keV down to Ec.m.=55 keV, the lowest energy measured to date corresponding to a cross-section of less than 1 picobarn/sr. The strength of a key resonance at center of mass energy Er=90 keV was found to be a factor of 10 higher than previously reported. A multi-channel R-matrix analysis of our and other data available in the literature was performed. Over a wide temperature range, T=0.01–1.00 GK, our new astrophysical rate is both more accurate and precise than recent evaluations. Stronger constraints can now be placed on the physical processes controlling nucleosynthesis in AGB stars with interesting consequences on the abundance of 18O in these stars and in stardust grains, specifically on the production sites of oxygen-rich Group II grains., SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2019

2. Experimental Nuclear Astrophysics With the Light Elements Li, Be and B: A Review

Author

G.G. Rapisarda, L. Lamia, A. Caciolli, Chengbo Li, S. Degl’Innocenti, R. Depalo, S. Palmerini, R.G. Pizzone, S. Romano, C. Spitaleri, E. Tognelli, and Qungang Wen

Subjects
Nuclear reaction, lcsh:Astronomy, nuclear astrophysics, chemistry.chemical_element, Electron, activation method, 01 natural sciences, Nuclear physics, lcsh:QB1-991, Nucleosynthesis, reaction rate, 0103 physical sciences, Nuclear astrophysics, Stellar structure, 010306 general physics, Spectroscopy, 010303 astronomy & astrophysics, nuclear reactions, Physics, lcsh:QC801-809, nucleosynthesis, Astronomy and Astrophysics, electron screening effect, lcsh:Geophysics. Cosmic physics, chemistry, Stellar physics, Beryllium
Abstract

Light elements offer a unique opportunity for studying several astrophysical scenarios from Big Bang Nucleosynthesis to stellar physics. Understanding the stellar abundances of light elements is key to obtaining information on internal stellar structures and mixing phenomena in different evolutionary phases, such as the pre-main-sequence, main-sequence or red-giant branch. In such a case, light elements, i.e., lithium, beryllium and boron, are usually burnt at temperatures of the order of 2–5 × 106 K. Consequently, the astrophysical S(E)-factor and the reaction rate of the nuclear reactions responsible for the burning of such elements must be measured and evaluated at ultra-low energies (between 0 and 10 keV). The Trojan Horse Method (THM) is an experimental technique that allows us to perform this kind of measurements avoiding uncertainties due to the extrapolation and electron screening effects on direct data. A long Trojan Horse Method research program has been devoted to the measurement of light element burning cross sections at astrophysical energies. In addition, dedicated direct measurements have been performed using both in-beam spectroscopy and the activation technique. In this review we will report the details of these experimental measurements and the results in terms of S(E)-factor, reaction rate and electron screening potential. A comparison between astrophysical reaction rates evaluated here and the literature will also be given.

Published
2021

3. 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

Author

Davide Trezzi, L. Di Paolo, I. Kochanek, V. Mossa, F. Ferraro, P. Colombetti, Carlo Bruno, K. Stöckel, Paolo Prati, Sandra Zavatarelli, F. R. Pantaleo, M. Junker, J. Balibrea-Correa, E. M. Fiore, A. Formicola, Gyuri Gyürky, F. Barile, G. Gervino, T. Chillery, G. F. Ciani, R. Depalo, A. Di Leva, Z. Elekes, M. P. Takács, R. Perrino, A. Best, Oscar Straniero, Marialuisa Aliotta, Filippo Terrasi, A. Guglielmetti, László Csedreki, A. Boeltzig, P. Corvisiero, C. Gustavino, F. Cavanna, Antonio Caciolli, Zs. Fülöp, Gianluca Imbriani, Carlo Broggini, M. Lugaro, E. Masha, Luigi Schiavulli, Daniel Bemmerer, Paola Marigo, D. Piatti, Roberto Menegazzo, Tamás Szücs, V. Paticchio, and Thomas Davinson

Subjects
Physics, Nuclear and High Energy Physics, Ion beam, 010308 nuclear & particles physics, Hadron, Resonance, 01 natural sciences, 7. Clean energy, Cross section (physics), 0103 physical sciences, Nuclear astrophysics, Nuclear fusion, Atomic physics, 010306 general physics, Beam energy, Stoichiometry
Abstract

Direct measurements of reaction cross-sections at astrophysical energies often require the use of solid targets able to withstand high ion beam currents for extended periods of time. Thus, monitoring target thickness, isotopic composition, and target stoichiometry during data taking is critical to account for possible target modifications and to reduce uncertainties in the final cross-section results. A common technique used for these purposes is the Nuclear Resonant Reaction Analysis (NRRA), which however requires that a narrow resonance be available inside the dynamic range of the accelerator used. In cases when this is not possible, as for example the $$^{13}\hbox {C}(\alpha ,\hbox {n})^{16}\hbox {O}$$ reaction recently studied at low energies at the Laboratory for Underground Nuclear Astrophysics (LUNA) in Italy, alternative approaches must be found. Here, we present a new application of the shape analysis of primary $$\gamma $$ rays emitted by the $$^{13}\hbox {C}(\hbox {p},\gamma )^{14}\hbox {N}$$ radiative capture reaction. This approach was used to monitor $$^{13}\hbox {C}$$ target degradation in situ during the $$^{13}\hbox {C}(\alpha ,\hbox {n})^{16}\hbox {O}$$ data taking campaign. The results obtained are in agreement with evaluations subsequently performed at Atomki (Hungary) using the NRRA method. A preliminary application for the extraction of the $$^{13}\hbox {C}(\alpha ,\hbox {n})^{16}\hbox {O}$$ reaction cross-section at one beam energy is also reported.

Published
2020

4. Direct Capture Cross Section and the Ep=71 and 105 keV Resonances in the Ne22(p,γ)Na23 Reaction

Author

D. Bemmerer, C. Broggini, Amanda I. Karakas, Davide Trezzi, P. Corvisiero, Gianluca Imbriani, T. Chillery, L. Schiavulli, C. G. Bruno, A. Di Leva, V. Mossa, A. Guglielmetti, M. P. Takács, R. Depalo, A. Boeltzig, G. D'Erasmo, K. Stöckel, Gy. Gyürky, Paolo Prati, G. Gervino, Z. Elekes, E. M. Fiore, G. F. Ciani, Paola Marigo, D. Piatti, A. Formicola, Antonio Caciolli, Tamás Szücs, Zs. Fülöp, R. Perrino, V. Paticchio, A. Best, Oscar Straniero, Marialuisa Aliotta, Roberto Menegazzo, Thomas Davinson, F. Ferraro, I. Kochanek, F. Cavanna, C. Gustavino, F. R. Pantaleo, Sandra Zavatarelli, M. Junker, and Maria Lugaro

Subjects
Physics, Hydrogen, S-factor, General Physics and Astronomy, chemistry.chemical_element, Resonance, 01 natural sciences, Reaction rate, Stars, chemistry, Orders of magnitude (time), Globular cluster, 0103 physical sciences, Nuclear astrophysics, Atomic physics, 010306 general physics, 010303 astronomy & astrophysics
Abstract

The ^{22}Ne(p,γ)^{23}Na reaction, part of the neon-sodium cycle of hydrogen burning, may explain the observed anticorrelation between sodium and oxygen abundances in globular cluster stars. Its rate is controlled by a number of low-energy resonances and a slowly varying nonresonant component. Three new resonances at E_{p}=156.2, 189.5, and 259.7 keV have recently been observed and confirmed. However, significant uncertainty on the reaction rate remains due to the nonresonant process and to two suggested resonances at E_{p}=71 and 105 keV. Here, new ^{22}Ne(p,γ)^{23}Na data with high statistics and low background are reported. Stringent upper limits of 6×10^{-11} and 7×10^{-11} eV (90% confidence level), respectively, are placed on the two suggested resonances. In addition, the off-resonant S factor has been measured at unprecedented low energy, constraining the contributions from a subthreshold resonance and the direct capture process. As a result, at a temperature of 0.1 GK the error bar of the ^{22}Ne(p,γ)^{23}Na rate is now reduced by 3 orders of magnitude.

Published
2018

5. Erratum: Three New Low-Energy Resonances in the Ne22(p,γ)Na23 Reaction [Phys. Rev. Lett. 115 , 252501 (2015)]

Author

M. Junker, Z. Elekes, P. Corvisiero, F. Ferraro, C. Broggini, Antonio Caciolli, Douglas Scott, A. Di Leva, Roberto Menegazzo, D. Bemmerer, V. Mossa, Gianluca Imbriani, Davide Trezzi, A. Guglielmetti, Thomas Davinson, F. Cavanna, A. Boeltzig, Tamás Szücs, C. Gustavino, Frank Strieder, C. G. Bruno, M. P. Takács, E. Somorjai, F. R. Pantaleo, A. Formicola, Paolo Prati, M. Anders, A. Best, G. Gervino, R. Depalo, Gy. Gyürky, Oscar Straniero, Marialuisa Aliotta, and Zs. Fülöp

Subjects
Physics, Low energy, 010308 nuclear & particles physics, 0103 physical sciences, General Physics and Astronomy, Atomic physics, 010306 general physics, 01 natural sciences
Published
2018

6. Fusion hindrance for the positive Q -value system C12+Si30

Author

A. M. Stefanini, Kouichi Hagino, F. Scarlassara, A. Goasduff, Shi-Peng Hu, S. Courtin, M. Heine, S. Bottoni, Maninder Kaur, P. Čolović, F. Galtarossa, Antonio Caciolli, E. Fioretto, D. Montanari, E. Strano, G. Colucci, C. Broggini, G. Fruet, Tea Mijatović, L. Corradi, A. Gal, S. Szilner, M. Mazzocco, G. X. Zhang, G. Montagnoli, R. Depalo, and C. L. Jiang

Subjects
Physics, Nuclear reaction, Excitation function, 010308 nuclear & particles physics, Q value, S-factor, Extrapolation, Coulomb barrier, 01 natural sciences, Orders of magnitude (time), 0103 physical sciences, Nuclear fusion, Atomic physics, 010306 general physics
Abstract

Background: The fusion reaction 12C+30Si is a link between heavier cases studied in recent years, and the light heavy-ion systems, e.g., 12C+12C, 16O+16O that have a prominent role in the dynamics of stellar evolution. 12C+30Si fusion itself is not a relevant process for astrophysics, but it is important to establish its behavior below the barrier, where couplings to low-lying collective modes and the hindrance phenomenon may determine the cross sections. The excitation function is presently completely unknown below the barrier for the 12C+30Si reaction, thus no reliable extrapolation into the astrophysical regime for the C+C and O+O cases can be performed. Purpose: Our aim was to carry out a complete measurement of the fusion excitation function of 12C+30Si from well below to above the Coulomb barrier, so as to clear up the consequence of couplings to low-lying states of 30Si, and whether the hindrance effect appears in this relatively light system which has a positive Q value for fusion. This would have consequences for the extrapolated behavior to even lighter systems. Methods: The inverse kinematics was used by sending 30Si beams delivered from the XTU Tandem accelerator of INFN-Laboratori Nazionali di Legnaro onto thin 12C (50μg/cm2) targets enriched to 99.9% in mass 12. The fusion evaporation residues (ER) were detected at very forward angles, following beam separation by means of an electrostatic deflector. Angular distributions of ER were measured at Ebeam=45, 59, and 80 MeV, and they were angle integrated to derive total fusion cross sections. Results: The fusion excitation function of 12C+30Si was measured with high statistical accuracy, covering more than five orders of magnitude down to a lowest cross section ≃3μb. The logarithmic slope and the S factor have been extracted and we have convincing phenomenological evidence of the hindrance effect. These results have been compared with the calculations performed within the model that considers a damping of the coupling strength well inside the Coulomb barrier. Conclusions: The experimental data are consistent with the coupled-channels calculations. A better fit is obtained by using the Yukawa-plus-exponential potential and a damping of the coupling strengths inside the barrier. The degree of hindrance is much smaller than the one in heavier systems. Also a phenomenological estimate reproduces quite closely the hindrance threshold for 12C+30Si, so that an extrapolation to the C+C and O+O cases can be reliably performed.

Published
2018

7. Improved background suppression for radiative capture reactions at LUNA with HPGe and BGO detectors

Author

F. Ferraro, Zs. Fülöp, P. Corvisiero, Michael Wiescher, A. Formicola, A. Di Leva, Gianluca Imbriani, Oscar Straniero, I. Kochanek, L. Schiavulli, G. Gervino, Marialuisa Aliotta, C. Broggini, R. Perrino, K. Stöckel, A. Guglielmetti, László Csedreki, M. P. Takács, Z. Elekes, A. Best, A. Boeltzig, Frank Strieder, Sandra Zavatarelli, F. Cavanna, Antonio Caciolli, M. Junker, C. Gustavino, György Gyürky, F. R. Pantaleo, Davide Trezzi, D. Piatti, C. G. Bruno, Tamás Szücs, Richard deBoer, D. Bemmerer, V. Paticchio, V. Mossa, G. F. Ciani, Roberto Menegazzo, Raffaele Buompane, Thomas Davinson, T. Chillery, E. M. Fiore, Paolo Prati, R. Depalo, Boeltzig, A., Best, A., Imbriani, G., Junker, M., Aliotta, M., Bemmerer, D., Broggini, C., Bruno, C. G., Buompane, R., Caciolli, A., Cavanna, F., Chillery, T., Ciani, G. F., Corvisiero, P., Csedreki, L., Davinson, T., Deboer, R. J., Depalo, R., Leva, A Di, Elekes, Z., Ferraro, F., Fiore, E. M., Formicola, A., Fülöp, Z., Gervino, G., Guglielmetti, A., Gustavino, C., Gyürky, G., Kochanek, I., Menegazzo, R., Mossa, V., Pantaleo, F. R., Paticchio, V., Perrino, R., Piatti, D., Prati, P., Schiavulli, L., Stöckel, K., Straniero, O., Strieder, F., Szücs, T., Takács, M. P., Trezzi, D., Wiescher, M., Zavatarelli, S., Leva, A. D., Fulop, Z., Gyurky, G., Stockel, K., Szucs, T., and Takacs, M. P.

Subjects
Physics, Nuclear and High Energy Physics, 010308 nuclear & particles physics, shielding, BGO, Radiative capture, Detector, nuclear astrophysics, 01 natural sciences, background reduction, gamma ray spectroscopy, Semiconductor detector, Nuclear physics, HPGe, summing detector, gamma ray spectroscopy, nuclear astrophysics, background reduction, shielding, HPGe, BGO, summing detector, 0103 physical sciences, Electromagnetic shielding, Background suppression, Nuclear astrophysics, Gamma spectroscopy, 010306 general physics, nuclear astrophysic
Abstract

Direct measurements of small nuclear reaction cross sections require a low background in the signal region of interest to achieve the necessary sensitivity. We describe two complementary detector setups that have been used for studies of $({\rm{p}},\gamma )$ reactions with solid targets at the Laboratory for Underground Nuclear Astrophysics (LUNA): a high-purity germanium detector and a bismuth germanate (BGO) detector. We present the effect of a customised lead shielding on the measured background spectra in the two detector setups at LUNA. We developed a model to describe the contributions of environmental and intrinsic backgrounds in the BGO detector measurements. Furthermore we present an upgrade of the data acquisition system for our BGO detector, which allows us to exploit the features of the segmented detector and overcome some of the limitations encountered in previous experiments. We conclude with a discussion on the improved sensitivity of the presented setups, and the benefits for ongoing and possible future measurements.

Published
2018

8. A high-efficiency gas target setup for underground experiments, and redetermination of the branching ratio of the 189.5 keV 22Ne(p, γ)23Na resonance

Author

Maria Lugaro, V. Paticchio, A. Formicola, A. Guglielmetti, László Csedreki, A. Boeltzig, Paola Marigo, T. Chillery, Zs. Fülöp, Z. Elekes, F. Ferraro, Gianluca Imbriani, L. Schiavulli, Antonio Caciolli, G. F. Ciani, K. Stöckel, V. Mossa, Sandra Zavatarelli, F. Cavanna, Oscar Straniero, M. Junker, D. Piatti, M. P. Takács, C. Gustavino, R. Perrino, Marialuisa Aliotta, Tamás Szücs, F. R. Pantaleo, C. G. Bruno, P. Corvisiero, G. D'Erasmo, Davide Trezzi, Paolo Prati, A. Di Leva, C. Broggini, R. Depalo, Gy. Gyürky, E. M. Fiore, D. Bemmerer, Laura Elisa Marcucci, Roberto Menegazzo, Thomas Davinson, A. Best, I. Kochanek, G. Gervino, Ferraro, F., Takács, M. P., Piatti, D., Mossa, V., Aliotta, M., Bemmerer, D., Best, A., Boeltzig, A., Broggini, C., Bruno, C. G., Caciolli, A., Cavanna, F., Chillery, T., Ciani, G. F., Corvisiero, P., Csedreki, L., Davinson, T., Depalo, R., D’Erasmo, G., Di Leva, A., Elekes, Z., Fiore, E. M., Formicola, A., Fülöp, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Gyürky, Gy., Imbriani, G., Junker, M., Kochanek, I., Lugaro, M., Marcucci, L. E., Marigo, P., Menegazzo, R., Pantaleo, F. R., Paticchio, V., Perrino, R., Prati, P., Schiavulli, L., Stöckel, K., Straniero, O., Szücs, T., Trezzi, D., and Zavatarelli, S.

Subjects
Nuclear reaction, Nuclear and High Energy Physics, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, 01 natural sciences, Temperature measurement, Bismuth germanate, Ion, Nuclear physics, chemistry.chemical_compound, 0103 physical sciences, undeground, Nuclear astrophysics, Nuclear fusion, low energy accelerators, 010306 general physics, Nuclear Experiment, detectors, Physics, 010308 nuclear & particles physics, Branching fraction, chemistry, nuclear atrophysics, nuclear atrophysics, undeground, detectors, low energy accelerators, Astrophysics - Instrumentation and Methods for Astrophysics, Beam (structure)
Abstract

The experimental study of nuclear reactions of astrophysical interest is greatly facilitated by a low-background, high-luminosity setup. The Laboratory for Underground Nuclear Astrophysics (LUNA) 400 kV accelerator offers ultra-low cosmic-ray induced background due to its location deep underground in the Gran Sasso National Laboratory (INFN-LNGS), Italy, and high intensity, 250-500 $\mu$A, proton and $\alpha$ ion beams. In order to fully exploit these features, a high-purity, recirculating gas target system for isotopically enriched gases is coupled to a high-efficiency, six-fold optically segmented bismuth germanate (BGO) $\gamma$-ray detector. The beam intensity is measured with a beam calorimeter with constant temperature gradient. Pressure and temperature measurements have been carried out at several positions along the beam path, and the resultant gas density profile has been determined. Calibrated $\gamma$-intensity standards and the well-known $E_p$ = 278 keV $\mathrm{^{14}N(p,\gamma)^{15}O}$ resonance were used to determine the $\gamma$-ray detection efficiency and to validate the simulation of the target and detector setup. As an example, the recently measured resonance at $E_p$ = 189.5 keV in the $^{22}$Ne(p,$\gamma$)$^{23}$Na reaction has been investigated with high statistics, and the $\gamma$-decay branching ratios of the resonance have been determined., Comment: 11 pages, 11 figures, accepted in Eur. Phys. Journal A

Published
2018

9. Origin of meteoritic stardust unveiled by a revised proton-capture rate of $^{17}$O

Author

C. G. Bruno, A. Best, A. Guglielmetti, M. Junker, A. Boeltzig, Gianluca Imbriani, Tamás Szücs, P. Corvisiero, Maria Lugaro, David Scott, Roberto Menegazzo, Carlo Broggini, A. Di Leva, A. Formicola, Thomas Davinson, Paolo Prati, G. Gervino, Larry R. Nittler, Oscar Straniero, Marialuisa Aliotta, F. Ferraro, R. Depalo, Gy. Gyürky, F. Cavanna, C. Gustavino, F. R. Pantaleo, D. Bemmerer, M. P. Takács, Davide Trezzi, Amanda I. Karakas, V. Mossa, Zs. Fülöp, D. Piatti, G. F. Ciani, F. Strieder, Z. Elekes, Antonio Caciolli, Lugaro, M., Karakas, A. I., Bruno, C. G., Aliotta, M., Nittler, L. R., Bemmerer, D., Best, A., Boeltzig, A., Broggini, C., Caciolli, A., Cavanna, F., Ciani, G. F., Corvisiero, P., Davinson, T., Depalo, R., Di Leva, A., Elekes, Z., Ferraro, F., Formicola, A., Fã¼lã¶p, Z. S., Gervino, G., Guglielmetti, A., Gustavino, C., Gyã¼rky, G. Y., Imbriani, G., Junker, M., Menegazzo, R., Mossa, V., Pantaleo, F. R., Piatti, D., Prati, P., Scott, D. A., Straniero, O., Strieder, F., Szã¼cs, T., Takã¡cs, M. P., and Trezzi, D.

Subjects
Physics, Solar mass, Proton, 010308 nuclear & particles physics, Presolar grains, nuclear astrophysics, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, nuclear reactions, nucleosynthesis, abundances, stars: abundances, stars: AGB and post-AGB, stars: carbon, stars: evolution, stars: mass loss, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrobiology, Stars, Astrophysics - Solar and Stellar Astrophysics, nuclear astrophysics, stellar grains, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, stellar grains, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

We investigate the impact of the new LUNA rate for the nuclear reaction Ne-22(p, gamma) Na-23 on the chemical ejecta of intermediate-mass stars, with particular focus on the thermally pulsing asymptotic giant branch (TP-AGB) stars that experience hot-bottom burning. To this aim, we use the PARSEC and COLIBRI codes to compute the complete evolution, from the premain sequence up to the termination of the TP-AGB phase, of a set of stellar models with initial masses in the range 3.0-6.0M(circle dot) and metallicities Z(i) = 0.0005, 0.006 and 0.014. We find that the new LUNA measures have much reduced the nuclear uncertainties of the Ne-22 and Na-23 AGB ejecta that drop from factors of similar or equal to 10 to only a factor of few for the lowest metallicity models. Relying on the most recent estimations for the destruction rate of Na-23, the uncertainties that still affect the Ne-22 and Na-23 AGB ejecta are mainly dominated by the evolutionary aspects (efficiency of mass-loss, third dredge-up, convection). Finally, we discuss how the LUNA results impact on the hypothesis that invokes massive AGB stars as the main agents of the observed O-Na anticorrelation in Galactic globular clusters. We derive quantitative indications on the efficiencies of key physical processes (mass-loss, third dredgeup, sodium destruction) in order to simultaneously reproduce both the Na-rich, O-poor extreme of the anticorrelation and the observational constraints on the CNO abundance. Results for the corresponding chemical ejecta are made publicly available.

Published
2017
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10. Direct measurement of low-energyNe22(p,γ)Na23resonances

Author

Davide Trezzi, M. P. Takács, R. Depalo, M. Anders, M. Junker, Gianluca Imbriani, A. Di Leva, G. F. Ciani, A. Boeltzig, Roberto Menegazzo, Oscar Straniero, Zs. Fülöp, Marialuisa Aliotta, A. Guglielmetti, Thomas Davinson, Paolo Prati, Tamás Szücs, F. R. Pantaleo, Daniel Bemmerer, D. Piatti, G. Gervino, A. Best, Carlo Broggini, A. Formicola, C. G. Bruno, V. Mossa, Gy. Gyürky, C. Gustavino, F. Cavanna, F. Ferraro, Z. Elekes, P. Corvisiero, and Antonio Caciolli

Subjects
Physics, Hydrogen, Proton, 010308 nuclear & particles physics, chemistry.chemical_element, 01 natural sciences, Nuclear physics, Stars, Low energy, chemistry, Nucleosynthesis, 0103 physical sciences, Radiative transfer, Asymptotic giant branch, Sensitivity (control systems), Atomic physics, 010306 general physics
Abstract

The authors perform a direct measurement of radiative proton capture on ${}^{22}$Ne at the LUNA underground laboratory whose low background allows unprecedented sensitivity. They report detailed experimental information for three recently observed new resonances in the ${}^{22}$Ne($p$,$\ensuremath{\gamma}$)${}^{23}$Na reaction which is the most uncertain process in the neon-sodium cycle of stellar hydrogen burning. At temperatures relevant for nucleosynthesis in asymptotic giant branch stars and classical novae, its uncertainty is mainly due to a large number of predicted but hitherto unobserved resonances at low energy. The updated thermonuclear reaction rate is significantly higher than previous evaluations at temperatures below 0.3 GK.

Published
2016

11. Shell and explosive hydrogen burning

Author

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

Subjects
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.

Published
2016

12. AGATA-Advanced GAmma Tracking Array

Author

A. Colombo, Y. Mariette, A. Johnson, W. Korten, A. Brondi, T. Faul, J. Robin, R. Depalo, M. Slee, J. Gre¸bosz, H. C. Boston, H. Harroch, B. Rossé, M. Filliger, M. Gulmini, A. Korichi, S. Brambilla, J.R. Cresswell, C. Parisel, P. Edelbruck, F. Ameil, F. Camera, C. Oziol, Matthew Richard Dimmock, G. Salvato, F. Morbiducci, J. Ropert, M. Borsato, E. Legay, Marco Bellato, C. Santos, Gheorghe Pascovici, L. Charles, J. Pancin, G. Casati, P. G. Bizzeti, T. Stanios, S. Lhenoret, Diego Barrientos, P.M. Jones, Andreas Görgen, V. Chambert, S. Aydin, K. Hauschild, B. Hervieu, R. Nicolini, J. Simpson, H. J. Wollersheim, L. Lavergne, Pär-Anders Söderström, G. S. Simpson, G. Jaworski, F. Filmer, R. Griffiths, P.S. Morrall, M. Petcu, G. Lo Bianco, D. Linget, A. Givechev, D. C. Oxley, M. Kogimtzis, F. Salomon, J. Jolie, D. Wells, S. Moon, C. Aufranc, A. Corsi, T. Descombes, N. Goel, J. Thornhill, N. Warr, Serkan Akkoyun, B. Birkenbach, F. Dorangeville, Joël Chavas, P. Medina, Roberto Isocrate, C. Weber, E. Merchan, Bo Cederwall, I. Kojouharov, Enrique Sanchis, A. Lopez-Martens, Oliver Wieland, F. Le Blanc, D. Seddon, S. C. Letts, D. Bazzacco, J. Leske, B. Bruyneel, Alberto Pullia, L. Nelson, G. La Rana, B. Travers, I. Burrows, G. Maron, S. Coelli, J. J. Valiente-Dobón, F. Saillant, Piotr Bednarczyk, V.L. Ngo, J. Mierzejewski, Norbert Pietralla, R.S. Kempley, N. Kurz, M. Rebeschini, S. Fantinel, D. L. Balabanski, A. J. Boston, F. Tomasi, R. Berthier, M. D. Salsac, B. Dulny, C. Stahl, N. Dosme, C. Fanin, R. Baumann, S. Pietri, A. Astier, M. Nicoletto, J. van der Marel, A. Bracco, Björn Jonson, D. Mengoni, D. Bloor, Luna Pellegri, F. Lefebvre, D. Pugnére, J. Egea, S. Cabaret, D. Curien, M. Reese, C. Commeaux, Dirk Rudolph, A. Giannatiempo, F. Recchia, L. Ramina, A. Lermitage, C. A. Ur, R. M. Lieder, I.P. Brawn, R. Menegazzo, R. Raine, Krasimir Mitev, D. R. Napoli, G. Suliman, M. Kebbiri, Y. Drouen, Susan Rigby, W. Me¸czyński, R. Wadsworth, F. Didierjean, P. Desesquelles, Ch. Veyssiere, S. Leoni, Vicente González, P. Gros, Y. Le Noa, M. Castoldi, O. Möller, R. Orlandi, Thomas Beck, M. Şenyiğit, A. Jungclaus, L. Gibelin, Mohammed Kaci, Zs. Podolyák, J. Gerl, S. Erturk, W. Gast, B. Melon, V. Mendéz, R. Peghin, P. Molini, M. N. Erduran, D. Conventi, Pankaj S. Joshi, E. Clément, F.A. Beck, A. Austin, A. Cortesi, J. Palin, P. Cocconi, L. J. Harkness, F. C. L. Crespi, Dirk Weisshaar, P. Sona, A. Czermak, D. Lersch, N. Blasi, Anton Khaplanov, O. Stezowski, B. Rubio, R. Venturelli, M.-H. Sigward, E. Viscione, José Salt, C. S. Özben, Giancarlo Ripamonti, P. Spolaore, Johan Nyberg, S. M. Lenzi, L. Legeard, N. Redon, C. Rossi Alvarez, C. He, R. Chapman, P. Le Pouhalec, C. Diarra, Herbert Hess, T. Engert, A. Kaşkaş, Stanislav Tashenov, S. Klupp, C. Michelagnoli, Elif Ince, A. Algora, J. F. Smith, M. Ozille, Alessandro Zucchiatti, Angelo Geraci, A. Olariu, M. Labiche, N. Karkour, Stefano Riboldi, P. Bourgault, C. M. Petrache, M. Palacz, M. El Chambit, J.-L. Cercus, M. Zie¸bliński, Alex Wiens, R. Beunard, X. Lafay, T. Habermann, M. Karolak, L. Costa, Y. Aubert, Begoña Quintana, A P Robinson, V. F. E. Pucknell, D. Rosso, A. Capsoni, Emanuele Vardaci, L. Mihailescu, M. Tripon, E. Farnea, Ch. Theisen, Enrico Calore, G. Duchêne, N. V. Zamfir, X. Grave, S. Lunardi, I.H. Lazarus, José Blasco, D. Montanari, J.A. Sampson, P. H. Regan, N. Marginean, M. Pignanelli, L. Arnold, G. Benzoni, R. Krücken, G. de Angelis, D.P. Scraggs, I. Piqueras, D. M. Cullen, A. Obertelli, A. Bürger, D. Bortolato, G. Rainovski, A.R. Mather, P. Reiter, C. Unsworth, G. Baulieu, P. J. Coleman-Smith, C. Boiano, M. Richer, Sébastien Perrier, Agnese Giaz, Reynold J. Cooper, V. Vandone, S. Tanguy, C. Domingo-Pardo, A. Bouty, A. N. Grint, A. Maj, A. Gottardo, L. Berti, E. Pachoud, R. Marginean, E. A. Stefanova, A. Triossi, M. Nespolo, D. Bucurescu, R. Moro, H.T.M. Ha, D. S. Judson, J. L. Tain, A. Perego, Francesco Lelli, P. Detistov, B.Y. Ky, J. Ljungvall, B. Sowicki, M. Schlarb, F. Azaiez, P. Pariset, Ertan Şahin, R. Gernhäuser, M. Turcato, John Paul Strachan, B. Million, A. Atac, F. Carrio, D. Delbourg, F. Veronese, Th. Kröll, B. Cahan, A. Hernandez-Prieto, M. A. Bentley, K.M.M. Tun-Lanoë, B. Alikhani, P. Boutachkov, S. Leboutelier, Maria Doncel, A. M. Bizzeti-Sona, R. Touzery, A. Nannini, A. Lotode, P. J. Nolan, G. Rampazzo, F. Zocca, H. Schaffner, J. Eberth, A. Gadea, N. Toniolo, T. Hüyük, Q.T. Doan, P. Petkov, S. Broussard, S. Badoer, M. Rigato, Philip M Walker, J. Pouthas, Ch. Finck, L. Milechina, M. Norman, E. Pierre, J. Roccaz, S.J. Colosimo, Lázaro Guevara, Glyn Wittwer, Millan, Vicente Gonzalez -- 0000-0001-6014-2586, Rainovski, Georgi -- 0000-0002-1729-0249, Jaworski, Grzegorz -- 0000-0003-2241-0329, KORTEN, Wolfram -- 0000-0002-3940-0816, Domingo-Pardo, Cesar -- 0000-0002-2915-5466, Triossi, Andrea -- 0000-0001-5140-9154, Huyuk, Tayfun -- 0000-0003-0597-9767, Ince, Elif -- 0000-0003-4821-5441, Algora, Alejandro -- 0000-0002-5199-1794, Calore, Enrico -- 0000-0002-2301-3838, Rubio, Berta -- 0000-0002-9149-4151, THEISEN, Christophe -- 0000-0002-8509-1022, Rudolph, Dirk -- 0000-0003-1199-3055, Gadea, Andres -- 0000-0002-4233-1970, santos, cayetano -- 0000-0003-0727-1914, nannini, adriana -- 0000-0003-0659-7648, Depalo, Rosanna -- 0000-0003-3943-7982, Suliman, gabriel -- 0000-0001-8475-1992, Blasco, Jose-Maria -- 0000-0002-7663-9092, Petrache, Costel -- 0000-0001-8419-1390, Pietralla, Norbert -- 0000-0002-4797-3032, Cederwall, Bo -- 0000-0003-1771-2656, Zucchiatti, Alessandro -- 0000-0002-3647-596X, Mendez Munoz, Victor -- 0000-0002-9044-1189, Kruecken, Reiner -- 0000-0002-2755-8042, Napoli, Daniel Ricardo -- 0000-0002-8154-6958, Tain, Jose L. -- 0000-0002-3263-6965, SANCHIS, ENRIQUE -- 0000-0002-9689-9131, Zieblinski, Miroslaw -- 0000-0002-8693-7317, Hauschild, Karl -- 0000-0003-2862-2445, Montanari, Daniele -- 0000-0002-1980-7686, senyigit, menekse -- 0000-0002-2408-4419, La Rana, Giovanni -- 0000-0003-2814-4113, Menegazzo, Roberto -- 0000-0002-3060-5276, Soderstrom, Par-Anders -- 0000-0002-9504-2814, Unsworth, Carl -- 0000-0002-4100-7466, Camera, Franco -- 0000-0003-1731-4834, Gorgen, Andreas -- 0000-0003-1916-9941, Hernandez Prieto, Alvaro -- 0000-0002-0340-0240, Recchia, Francesco -- 0000-0002-8428-0112, de France, Gilles -- 0000-0002-7439-1759, GOTTARDO, Andrea -- 0000-0002-0390-5767, Perrier, Sebastien -- 0000-0001-5055-9046, Sowicki, Bogdan -- 0000-0002-7208-0690, Robinson, Andrew -- 0000-0002-2510-1321, Sahin, Eda -- 0000-0003-0683-5140, Pullia, Alberto -- 0000-0002-6393-747X, Lelli, Francesco -- 0000-0003-1900-9171, Clement, Emmanuel -- 0000-0003-1887-717X, benzoni, giovanna -- 0000-0002-7938-0338, Jonson, Bjorn -- 0000-0002-9697-9115, Bednarczyk, Piotr -- 0000-0002-5699-5292, Jones, Pete -- 0000-0001-7480-6603, Nicoletto, Marino -- 0000-0001-9301-0782, Ripamonti, Giancarlo -- 0000-0002-9406-021X, Bentley, Michael -- 0000-0001-8401-3455, Pellegri, Luna -- 0000-0002-3227-3332, Barrientos, Diego -- 0000-0001-9693-2942, GIAZ, Agnese -- 0000-0002-2550-450X, [Boston, A. J. -- Boston, H. C. -- Colosimo, S. -- Cooper, R. J. -- Cresswell, J. R. -- Dimmock, M. R. -- Filmer, F. -- Grint, A. N. -- Harkness, L. J. -- Judson, D. S. -- Mather, A. R. -- Moon, S. -- Nelson, L. -- Nolan, P. J. -- Norman, M. -- Oxley, D. C. -- Rigby, S. -- Sampson, J. -- Scraggs, D. P. -- Seddon, D. -- Slee, M. -- Stanios, T. -- Thornhill, J. -- Unsworth, C. -- Wells, D.] Univ Liverpool, Oliver Lodge Lab, Liverpool L69 7ZE, Merseyside, England -- [Akkoyun, S. -- Atac, A. -- Kaskas, A. -- Senyigit, M.] Ankara Univ, Fac Sci, Dept Phys, TR-06100 Ankara, Turkey -- [Algora, A. -- Barrientos, D. -- Domingo-Pardo, C. -- Egea, J. -- Gadea, A. -- Hueyuek, T. -- Kaci, M. -- Mendez, V. -- Rubio, B. -- Salt, J. -- Tain, J. L.] Univ Valencia, CSIC, IFIC, E-46980 Paterna, Spain -- [Alikhani, B. -- Boutachkov, P. -- Givechev, A. -- Goel, N. -- Leske, J. -- Merchan, E. -- Moeller, O. -- Pietralla, N. -- Reese, M. -- Stahl, C.] Tech Univ Darmstadt, IKP, D-64289 Darmstadt, Germany -- [Ameil, F. -- Beck, T. -- Boutachkov, P. -- Domingo-Pardo, C. -- Engert, T. -- Gerl, J. -- Goel, N. -- Habermann, T. -- Kojouharov, I. -- Kurz, N. -- Merchan, E. -- Pietri, S. -- Schaffner, H. -- Tashenov, S. -- Wollersheim, H. J.] GSI Helmholtzzentrum Schwerionenforsch GmbH, D-64291 Darmstadt, Germany -- [de Angelis, G. -- Badoer, S. -- Berti, L. -- Calore, E. -- Cocconi, P. -- Conventi, D. -- Costa, L. -- Fantinel, S. -- Gadea, A. -- Gottardo, A. -- Gulmini, M. -- He, C. -- Ince, E. -- Kroell, Th. -- Lelli, F. -- Maron, G. -- Molini, P. -- Napoli, D. R. -- Rigato, M. -- Rosso, D. -- Sahin, E. -- Spolaore, P. -- Toniolo, N. -- Valiente-Dobon, J. J.] Ist Nazl Fis Nucl, Lab Nazl Legnaro, IT-35020 Padua, Italy -- [Arnold, L. -- Baumann, R. -- Beck, F. A. -- El Chambit, M. -- Charles, L. -- Curien, D. -- Didierjean, F. -- Duchene, G. -- Faul, T. -- Filliger, M. -- Finck, Ch. -- Medina, P. -- Pachoud, E. -- Parisel, C. -- Piqueras, I. -- Richer, M. -- Robin, J. -- Santos, C. -- Sigward, M. -H. -- Weber, C.] Univ Strasbourg, IPHC, F-67037 Strasbourg, France -- [Arnold, L. -- Baumann, R. -- Beck, F. A. -- El Chambit, M. -- Charles, L. -- Curien, D. -- Didierjean, F. -- Duchene, G. -- Faul, T. -- Filliger, M. -- Finck, Ch. -- Medina, P. -- Pachoud, E. -- Parisel, C. -- Piqueras, I. -- Richer, M. -- Robin, J. -- Santos, C. -- Sigward, M. -H. -- Weber, C.] CNRS, UMR 7178, F-67037 Strasbourg, France -- [Astier, A. -- Cabaret, S. -- Desesquelles, P. -- Dosme, N. -- Gibelin, L. -- Ha, H. T. M. -- Hauschild, K. -- Karkour, N. -- Korichi, A. -- Lafay, X. -- Leboutelier, S. -- Legay, E. -- Lhenoret, S. -- Linget, D. -- Ljungvall, J. -- Lopez-Martens, A. -- Morbiducci, F. -- Ngo, V. L. -- Pariset, P. -- Perrier, S. -- Pierre, E. -- Roccaz, J. -- Travers, B.] Univ Paris 11, CNRS, IN2P3, CSNSM, F-91405 Orsay, France -- [Atac, A. -- Nyberg, J. -- Soderstrom, P. -A.] Uppsala Univ, Dept Phys & Astron, Uppsala, Sweden -- [Atac, A. -- Cederwall, B. -- Johnson, A. -- Khaplanov, A. -- van der Marel, J. -- Milechina, L. -- Tashenov, S.] Royal Inst Technol, SE-10691 Stockholm, Sweden -- [Aubert, Y. -- Azaiez, F. -- Le Blanc, F. -- Cercus, J. -L. -- Chambert, V. -- Commeaux, C. -- Delbourg, D. -- Diarra, C. -- Dorangeville, F. -- Edelbruck, P. -- Grave, X. -- Guevara, L. -- Harroch, H. -- Ky, B. Y. -- Lavergne, L. -- Lefebvre, F. -- Lermitage, A. -- Olariu, A. -- Oziol, C. -- Petrache, C. -- Pouthas, J. -- Salomon, F. -- Tanguy, S. -- Tun-Lanoe, K. M. M.] Univ Paris 11, CNRS, IN2P3, IPNO, F-91406 Orsay, France -- [Aufranc, C. -- Baulieu, G. -- Doan, Q. T. -- Pugnere, D. -- Redon, N. -- Rosse, B. -- Stezowski, O.] Univ Lyon 1, CNRS, IN2P3, Inst Phys Nucl Lyon, F-69622 Villeurbanne, France -- [Austin, A. -- Burrows, I. -- Coleman-Smith, P. J. -- Griffiths, R. -- Kogimtzis, M. -- Labiche, M. -- Lazarus, I. H. -- Letts, S. C. -- Morrall, P. S. -- Palin, J. -- Pucknell, V. F. E. -- Simpson, J. -- Strachan, J.] STFC Daresbury Lab, Warrington WA4 4AD, Cheshire, England -- [Aydin, S. -- Bazzacco, D. -- Bellato, M. -- Bortolato, D. -- Chavas, J. -- Colombo, A. -- Fanin, C. -- Farnea, E. -- Isocrate, R. -- Kroell, Th. -- Lenzi, S. M. -- Lunardi, S. -- Marginean, R. -- Menegazzo, R. -- Mengoni, D. -- Michelagnoli, C. -- Nespolo, M. -- Nicoletto, M. -- Peghin, R. -- Ramina, L. -- Rampazzo, G. -- Rebeschini, M. -- Recchia, F. -- Rossi Alvarez, C. -- Salvato, G. -- Triossi, A. -- Turcato, M. -- Ur, C. A. -- Venturelli, R. -- Veronese, F.] Ist Nazl Fis Nucl, Sez Padova, IT-35131 Padua, Italy -- [Balabanski, D. L. -- Detistov, P. -- Petkov, P. -- Stefanova, E.] Bulgarian Acad Sci, Inst Nucl Res & Nucl Energy, Sofia, Bulgaria -- [Bednarczyk, P. -- Czermak, A. -- Dulny, B. -- Grebosz, J. -- Maj, A. -- Meczynski, W. -- Sowicki, B. -- Zieblinski, M.] Polish Acad Sci, Henryk Niewodniczanski Inst Nucl Phys, PL-31342 Krakow, Poland -- [Bentley, M. A. -- Bloor, D. -- Joshi, P. -- Wadsworth, R.] Univ York, Dept Phys, York YO10 5DD, N Yorkshire, England -- [Benzoni, G. -- Blasi, N. -- Boiano, C. -- Bracco, A. -- Brambilla, S. -- Camera, F. -- Capsoni, A. -- Casati, G. -- Coelli, S. -- Corsi, A. -- Cortesi, A. -- Crespi, F. C. L. -- Geraci, A. -- Giaz, A. -- Leoni, S. -- Million, B. -- Montanari, D. -- Nicolini, R. -- Pellegri, L. -- Pignanelli, M. -- Pullia, A. -- Riboldi, S. -- Ripamonti, G. -- Tomasi, F. -- Vandone, V. -- Viscione, E. -- Wieland, O. -- Zocca, F.] Ist Nazl Fis Nucl, Sez Milano, IT-20133 Milan, Italy -- [Berthier, R. -- Bouty, A. -- Broussard, S. -- Buerger, A. -- Drouen, Y. -- Gros, P. -- Goergen, A. -- Hervieu, B. -- Karolak, M. -- Kebbiri, M. -- Korten, W. -- Ljungvall, J. -- Lotode, A. -- Mariette, Y. -- Le Noa, Y. -- Obertelli, A. -- Le Pouhalec, P. -- Salsac, M. -D. -- Theisen, Ch. -- Touzery, R. -- Veyssiere, Ch.] CEA, Ctr Saclay, IRFU, F-91191 Gif Sur Yvette, France -- [Beunard, R. -- Bourgault, P. -- Cahan, B. -- Clement, E. -- de France, G. -- Legeard, L. -- Ozille, M. -- Pancin, J. -- Raine, R. -- Ropert, J. -A. -- Saillant, F. -- Tripon, M. -- Wittwer, G.] CEA DSM CNRS IN2P3, GANIL, F-14076 Caen, France -- [Birkenbach, B. -- Bruyneel, B. -- Eberth, J. -- Hess, H. -- Jolie, J. -- Lersch, D. -- Pascovici, G. -- Reiter, P. -- Warr, N. -- Weisshaar, D. -- Wiens, A.] Univ Cologne, IKP, D-50937 Cologne, Germany -- [Bizzeti, P. G. -- Bizzeti-Sona, A. M. -- Giannatiempo, A. -- Melon, B. -- Perego, A. -- Sona, P.] Univ Florence, Dipartimento Fis & Astron, IT-50019 Florence, Italy -- [Bizzeti, P. G. -- Bizzeti-Sona, A. M. -- Giannatiempo, A. -- Melon, B. -- Nannini, A. -- Perego, A. -- Sona, P.] Ist Nazl Fis Nucl, Sez Firenze, IT-50019 Florence, Italy -- [Blasco, J. M. -- Carrio, F. -- Egea, J. -- Gonzalez, V. -- Sanchis, E.] Univ Valencia, Dept Elect Engn, E-46100 Burjassot, Valencia, Spain -- [Borsato, M. -- Bortolato, D. -- Lenzi, S. M. -- Lunardi, S. -- Marginean, R. -- Mengoni, D. -- Michelagnoli, C. -- Nespolo, M. -- Recchia, F. -- Salvato, G. -- Triossi, A. -- Venturelli, R.] Univ Padua, Dipartimento Fis, IT-35131 Padua, Italy -- [Bracco, A. -- Camera, F. -- Corsi, A. -- Crespi, F. C. L. -- Giaz, A. -- Leoni, S. -- Montanari, D. -- Nicolini, R. -- Pellegri, L. -- Pignanelli, M. -- Pullia, A. -- Riboldi, S. -- Vandone, V.] Univ Milan, Dipartimento Fis, IT-20133 Milan, Italy -- [Brawn, I. P.] STFC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England -- [Brondi, A. -- Moro, R. -- La Rana, G. -- Vardaci, E.] Univ Naples Federico II, Dipartimento Fis, IT-80126 Naples, Italy -- [Brondi, A. -- Moro, R. -- La Rana, G. -- Vardaci, E.] Ist Nazl Fis Nucl, Sez Napoli, IT-80126 Naples, Italy -- [Bucurescu, D. -- Marginean, N. -- Marginean, R. -- Petcu, M. -- Ur, C. A.] Natl Inst Phys & Nucl Engn, Bucharest, Romania -- [Buerger, A. -- Suliman, G. -- Zamfir, N. V.] Univ Bonn, Helmholtz Inst Strahlen & Kernphys, D-53115 Bonn, Germany -- [Buerger, A.] Univ Oslo, Dept Phys, N-0316 Oslo, Norway -- [Casati, G. -- Geraci, A. -- Ripamonti, G.] Politecn Milan, Dipartimento Elettron & Informaz, IT-20133 Milan, Italy -- [Castoldi, M. -- Zucchiatti, A.] Ist Nazl Fis Nucl, Sez Genova, IT-16146 Genoa, Italy -- [Chapman, R. -- Mengoni, D. -- Orlandi, R. -- Smith, J. F.] Univ W Scotland, Sch Engn, Paisley PA1 2BE, Renfrew, Scotland -- [Cullen, D. M. -- Robinson, A. P.] Univ Manchester, Sch Phys & Astron, Schuster Lab, Manchester M13 9PL, Lancs, England -- [Depalo, R.] Univ Padua, Dipartimento Astron, IT-35131 Padua, Italy -- [Descombes, T. -- Simpson, G.] Univ Grenoble 1, CNRS, IN2P3, LPSC,INP Grenoble, F-38026 Grenoble, France -- [Doncel, M. -- Hernandez-Prieto, A. -- Quintana, B.] Univ Salamanca, Dept Fis Fundamental, E-37008 Salamanca, Spain -- [Erduran, M. N. -- Ince, E.] Istanbul Univ, Istanbul, Turkey -- [Erturk, S.] Nigde Univ, Fac Sci, Dept Phys, TR-51200 Nigde, Turkey -- [Gast, W. -- Lieder, R. M. -- Mihailescu, L.] Forschungszentrum Julich, Inst Kernphys, D-52425 Julich, Germany -- [Gernhaeuser, R. -- Klupp, S. -- Kruecken, R. -- Schlarb, M.] Tech Univ Munich, Phys Dept E12, D-85748 Garching, Germany -- [Jaworski, G.] Warsaw Univ Technol, Fac Phys, PL-00662 Warsaw, Poland -- [Jaworski, G. -- Mierzejewski, J. -- Palacz, M.] Univ Warsaw, Heavy Ion Lab, PL-02093 Warsaw, Poland -- [Jones, P.] Univ Jyvaskyla, Dept Phys, FI-40014 Jyvaskyla, Finland -- [Jonson, B.] Chalmers, S-41296 Gothenburg, Sweden -- [Jungclaus, A. -- Orlandi, R.] CSIC, Inst Estruct Mat, E-28006 Madrid, Spain -- [Kempley, R. S. -- Podolyak, Z. -- Regan, P. H. -- Walker, P. M.] Univ Surrey, Dept Phys, Guildford GU2 7XH, Surrey, England -- [Mitev, K. -- Rainovski, G.] Sofia Univ St Kliment Ohridski, Fac Phys, Sofia, Bulgaria -- [Ozben, C.] Istanbul Tech Univ, TR-80626 Istanbul, Turkey -- [Rudolph, D.] Lund Univ, Dept Phys, SE-22100 Lund, Sweden, Research Group: Information Management, CSNSM SNO, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), informatique, Institut de Physique Nucléaire de Lyon (IPNL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Grand Accélérateur National d'Ions Lourds (GANIL), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Département de Physique Nucléaire (ex SPhN) (DPHN), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, CSNSM MECA, Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), CSNSM INFOR, CSNSM ELEC, Matière Nucléaire, Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), AGATA, Akkoyun, S., Algora, A., Alikhani, B., Ameil, F., De Angelis, G, Arnold, L., Astier, A., Ataç, A., Aubert, Y., Aufranc, C., Austin, A., Aydin, S., Azaiez, F., Badoer, S., Balabanski, D. L., Barrientos, D., Baulieu G., L, Baumann, R., Bazzacco, D., Beck, F. A., Beck, T., Bednarczyk, P., Bellato, M., Bentley, M. A., Benzoni, G., Berthier, R., Berti, L., Beunard, R., Lo Bianco, G., Birkenbach, B., Bizzeti, P. G., Bizzeti Sona, A. M., Le Blanc, F., Blasco, J. M., Blasi, N., Bloor, D., Boiano, C., Borsato, M., Bortolato, D., Boston, A. J., Boston, H. C., Bourgault, P., Boutachkov, P., Bouty, A., Bracco, A., Brambilla, S., Brawn, I. P., Brondi, Augusto, Broussard, S., Bruyneel, B., Bucurescu, D., Burrows, I., Bürger, A., Cabaret, S., Cahan, B., Calore, E., Camera, F., Capsoni, A., Carrió, F., Casati, G., Castoldi, M., Cederwall, B., Cercus J., L, Chambert, V., El Chambit, M., Chapman, R., Charles, L., Chavas, J., Clément, E., Cocconi, P., Coelli, S., Coleman Smith, P. J., Colombo, A., Colosimo, S., Commeaux, C., Conventi, D., Cooper, R. J., Corsi, A., Cortesi, A., Costa, L., Crespi, F. C. L., Cresswell, J. R., Cullen, D. M., Curien, D., Czermak, A., Delbourg, D., Depalo, R., Descombes, T., Désesquelles, P., Detistov, P., Diarra, C., Didierjean, F., Dimmock, M. R., Doan, Q. T., Domingo Pardo, C., Doncel, M., Dorangeville, F., Dosme, N., Drouen, Y., Duchêne, G., Dulny, B., Eberth, J., Edelbruck, P., Egea, J., Engert, T., Erduran, M. N., Ertürk, S., Fanin, C., Fantinel, S., Farnea, E., Faul, T., Filliger, M., Filmer, F., Finck, C., De France, G., Gadea, A., Gast, W., Geraci, A., Gerl, J., Gernhäuser, R., Giannatiempo, A., Giaz, A., Gibelin, L., Givechev, A., Goel, N., González, V., Gottardo, A., Grave, X., Grȩbosz, J., Griffiths, R., Grint, A. N., Gros, P., Guevara, L., Gulmini, M., Görgen, A., Ha, H. T. M., Habermann, T., Harkness, L. J., Harroch, H., Hauschild, K., He, C., Hernández Prieto, A., Hervieu, B., Hess, H., Hüyük, T., Ince, E., Isocrate, R., Jaworski, G., Johnson, A., Jolie, J., Jones, P., Jonson, B., Joshi, P., Judson, D. S., Jungclaus, A., Kaci, M., Karkour, N., Karolak, M., Kaşkaş, A., Kebbiri, M., Kempley, R. S., Khaplanov, A., Klupp, S., Kogimtzis, M., Kojouharov, I., Korichi, A., Korten, W., Kröll, T., Krücken, R., Kurz, N., Ky, B. Y., Labiche, M., Lafay, X., Lavergne, L., Lazarus, I. H., Leboutelier, S., Lefebvre, F., Legay, E., Legeard, L., Lelli, F., Lenzi, S. M., Leoni, S., Lermitage, A., Lersch, D., Leske, J., Letts, S. C., Lhenoret, S., Lieder, R. M., Linget, D., Ljungvall, J., Lopez Martens, A., Lotodé, A., Lunardi, S., Maj, A., Van Der Marel, J., Mariette, Y., Marginean, N., Marginean, R., Maron, G., Mather, A. R., Mȩczyński, W., Mendéz, V., Medina, P., Melon, B., Menegazzo, R., Mengoni, D., Merchan, E., Mihailescu, L., Michelagnoli, C., Mierzejewski, J., Milechina, L., Million, B., Mitev, K., Molini, P., Montanari, D., Moon, S., Morbiducci, F., Moro, RENATA EMILIA MARIA, Morrall, P. S., Möller, O., Nannini, A, Napoli, D. R., Nelson, L., Nespolo, M., Ngo, V. L., Nicoletto, M., Nicolini, R., Le Noa, Y., Nolan, P. J., Norman, M., Nyberg, J., Obertelli, A., Olariu, A., Orlandi, R., Oxley, D. C., Özben, C., Ozille, M., Oziol, C., Pachoud, E., Palacz, M., Palin, J., Pancin, J., Parisel, C., Pariset, P., Pascovici, G., Peghin, R., Pellegri, L., Perego, A., Perrier, S., Petcu, M., Petkov, P., Petrache, C., Pierre, E., Pietralla, N., Pietri, S., Pignanelli, M., Piqueras, I., Podolyak, Z., Le Pouhalec, P., Pouthas, J., Pugnére D., L, Pucknell, V. F. E., Pullia, A., Quintana, B., Raine, R., Rainovski, G., Ramina, L., Rampazzo, G., LA RANA, Giovanni, Rebeschini, M., Recchia, F., Redon N., L, Reese M., C, Reiter, P., Regan, P. H., Riboldi, S., Richer, M., Rigato, M., Rigby, S., Ripamonti, G., Robinson, A., Robin, J., Roccaz, J., Ropert, J. A., Rossé, B. l., Rossi Alvarez, C., Rosso, D., Rubio, B., Rudolph, D., Saillant, F., Şahin, E., Salomon, F., Salsac, M. D., Salt, J., Salvato, G., Sampson, J., Sanchis, E., Santos, C., Schaffner, H., Schlarb, M., Scraggs, D. P., Seddon, D., Şenyiǧit, M., Sigward, M. H., Simpson, G., Simpson, J., Slee, M., Smith, J. F., Sona, P., Sowicki, B., Spolaore, P., Stahl, C., Stanios, T., Stefanova, E., Stézowski, O., Strachan, J., Suliman, G., Söderström, P. A., Tain, J. L., Tanguy, S., Tashenov, S., Theisen, C. h., Thornhill, J., Tomasi, F., Toniolo, N., Touzery, R., Travers, B., Triossi, A., Tripon, M., Tun Lanoë, K. M. M., Turcato, M., Unsworth, C., Ur, C. A., Valiente Dobon, J. J., Vandone, V., Vardaci, Emanuele, Venturelli, R., Veronese, F., Veyssiere, C., Viscione, E., Wadsworth, R., Walker, P. M., Warr, N., Weber, C., Weisshaar, D., Wells, D., Wieland, O., Wiens A., U, Wittwer, G., Wollersheim, H. J., Zocca, F., Zamfir, N. V., Ziȩbliński, M., Zucchiatti, A., Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), and 0-Belirlenecek

Subjects
Nuclear and High Energy Physics, Physics - Instrumentation and Detectors, Pulse-shape and gamma-ray tracking algorithms, FOS: Physical sciences, Semiconductor detector performance and simulations, Integrated circuit, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], Tracking (particle physics), gamma-Ray tracking, 01 natural sciences, Pulse-shape and γ-ray tracking algorithms, law.invention, Data acquisition, law, 0103 physical sciences, ddc:530, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Nuclear Experiment (nucl-ex), 010306 general physics, γ-Ray spectroscopy, Nuclear Experiment, Instrumentation, Digital signal processing, Event reconstruction, gamma-Ray spectroscopy, Physics, sezele, Spectrometer, Spectrometers, 010308 nuclear & particles physics, business.industry, Detector, AGATA, Digital signals, HPGe detectors, Pulse-shape, Ray tracking, HPGe detectors, Algorithms, Crystals, Germanium, Semiconductor detectors, Signal processing, Spectrometry, Tracking (position), γ-Ray tracking, Instrumentation and Detectors (physics.ins-det), AGATA, Física nuclear, business, Computer hardware
Abstract

WOS: 000300864200005, The Advanced GAmma Tracking Array (AGATA) is a European project to develop and operate the next generation gamma-ray spectrometer. AGATA is based on the technique of gamma-ray energy tracking in electrically segmented high-purity germanium crystals. This technique requires the accurate determination of the energy, time and position of every interaction as a gamma ray deposits its energy within the detector volume. Reconstruction of the full interaction path results in a detector with very high efficiency and excellent spectral response. The realisation of gamma-ray tracking and AGATA is a result of many technical advances. These include the development of encapsulated highly segmented germanium detectors assembled in a triple cluster detector cryostat, an electronics system with fast digital sampling and a data acquisition system to process the data at a high rate. The full characterisation of the crystals was measured and compared with detector-response simulations. This enabled pulse-shape analysis algorithms, to extract energy, time and position, to be employed. In addition, tracking algorithms for event reconstruction were developed. The first phase of AGATA is now complete and operational in its first physics campaign. In the future AGATA will be moved between laboratories in Europe and operated in a series of campaigns to take advantage of the different beams and facilities available to maximise its science output. The paper reviews all the achievements made in the AGATA project including all the necessary infrastructure to operate and support the spectrometer. (C) 2011 Elsevier B.V. All rights reserved., EU [RII3-CT-2004-506065]; German BMBF [06K-167, 06KY2051]; Swedish Research Council; Knut and Alice Wallenberg Foundation; UK EPSRC Engineering and Physical Sciences Research Council; UK STFC Science and Technology Facilities Council; AWE plc; Scientific and Technological Research Council of Turkey [106T055]; Ankara University [05B4240002]; Polish Ministry of Science and Higher Education [DPN/N190/AGATA/2009]; Spanish MICINN [FPA2008-06419, FPA2009-13377-C02-02]; Spanish Consolider-Ingenio Programme CPAN [CSD2007-00042]; Generalitat Valenciana [PROMETEO/2010/101]; MICINN, Spain; INFN, Italy [AIC10-D-000568]; Science and Technology Facilities Council [ST/F012039/1, ST/J000094/1, ST/F004192/1, ST/J000159/1, ST/I504940/1, NuSTAR, ST/F006950/1, ST/I504916/1, ST/G000670/1, ST/F004060/1, ST/J000051/1, ST/J000108/1, ST/G000670/1 NuSTAR, ST/I504959/1, ST/G000727/1, ST/F004052/1, ST/F004184/1], AGATA and this work is supported by the European funding bodies and the EU Contract RII3-CT-2004-506065, the German BMBF under Grants 06K-167 and 06KY2051, the Swedish Research Council and the Knut and Alice Wallenberg Foundation, UK EPSRC Engineering and Physical Sciences Research Council, UK STFC Science and Technology Facilities Council, AWE plc, Scientific and Technological Research Council of Turkey (Proj. nr. 106T055) and Ankara University (BAP Proj. nr. 05B4240002), the Polish Ministry of Science and Higher Education under Grant DPN/N190/AGATA/2009, the Spanish MICINN under grants FPA2008-06419 and FPA2009-13377-C02-02, the Spanish Consolider-Ingenio 2010 Programme CPAN (contract number CSD2007-00042) the Generalitat Valenciana under Grant PROMETEO/2010/101, and research performed in the frame of the GSI-IN2P3 collaboration agreement number 02-42. A. Gadea and E. Farnea acknowledge the support of MICINN, Spain, and INFN, Italy, through the AIC10-D-000568 bilateral action.

Published
2012

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