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45 results on '"Nuclear astrophysic"'

1. NEAR: A New Station to Study Neutron-Induced Reactions of Astrophysical Interest at CERN-n_TOF

Author

Gianpiero Gervino, Oliver Aberle, Ana-Paula Bernardes, Nicola Colonna, Sergio Cristallo, Maria Diakaki, Salvatore Fiore, Alice Manna, Cristian Massimi, Pierfrancesco Mastinu, Alberto Mengoni, Riccardo Mucciola, Elizabeth Musacchio González, Nikolas Patronis, Elisso Stamati, Pedro Vaz, Rosa Vlastou, Gianpiero Gervino, Oliver Aberle, Ana-Paula Bernarde, Nicola Colonna, Sergio Cristallo, Maria Diakaki, Salvatore Fiore, Alice Manna, Cristian Massimi, Pierfrancesco Mastinu, Alberto Mengoni, Riccardo Mucciola, Elizabeth Musacchio Gonz??lez, Nikolas Patroni, Elisso Stamati, Pedro Vaz, Rosa Vlastou, ITA, and GRC

Subjects
Astrophysics and Astronomy, s-proce, r-process, NEAR, General Physics and Astronomy, Nuclear Physics - Experiment, n_TOF, neutron activation, Detectors and Experimental Techniques, nuclear astrophysics, s-process, Nuclear Experiment, nuclear astrophysic
Abstract

We present NEAR, a new experimental area at the CERN-n_TOF facility and a possible setup for cross section measurements of interest to nuclear astrophysics. This was recently realized with the aim of performing spectral-averaged neutron-capture cross section measurements by means of the activation technique. The recently commissioned NEAR station at n_TOF is now ready for the physics program, which includes a preliminary benchmark of the proposed idea. Based on the results obtained by dedicated Monte Carlo simulations and calculation, a suitable filtering of the neutron beam is expected to enable measurements of Maxwellian Averaged Cross Section (MACS) at different temperatures. To validate the feasibility of these studies we plan to start the measurement campaign by irradiating several isotopes whose MACS at different temperatures have recently been or are planned to be determined with high accuracy at n_TOF, as a function of energy in the two time-of-flight measurement stations. For instance, the physical cases of 88Sr(n,γ), 89Y(n,γ), 94Zr(n,γ) and 64Ni(n,γ) are discussed. As the neutron capture on 89Y produces a pure β-decay emitter, we plan to test the possibility to perform activation measurements on such class of isotopes as well. The expected results of these measurements would open the way to challenging measurements of MACS by the activation technique at n_TOF, for rare and/or exotic isotopes of interest for nuclear astrophysics.

Published
2022
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2. Characterization of the LUNA neutron detector array for the measurement of the 13C(α,n)16O reaction

Author

Csedreki L., Ciani G. F., Balibrea-Correa J., Best A., Aliotta M., Barile F., Bemmerer D., Boeltzig A., Broggini C., Bruno C. G., Caciolli A., Cavanna F., Chillery T., Colombetti P., Corvisiero P., Davinson T., Depalo R., Di Leva A., Elekes Z., Ferraro F., Fiore E. M., Formicola A., Fulop Z., Gervino G., Guglielmetti A., Gustavino C., Gyurky G., Imbriani G., Janas Z., Junker M., Kochanek I., Lugaro M., Marigo P., Masha E., Mazzocchi C., Menegazzo R., Mossa V., Pantaleo F. R., Paticchio V., Perrino R., Piatti D., Prati P., Schiavulli L., Stockel K., Straniero O., Szucs T., Takacs M. P., Terrasi F., Zavatarelli S., Csedreki, L., Ciani, G. F., Balibrea-Correa, J., Best, A., Aliotta, M., Barile, F., Bemmerer, D., Boeltzig, A., Broggini, C., Bruno, C. G., Caciolli, A., Cavanna, F., Chillery, T., Colombetti, P., Corvisiero, P., Davinson, T., Depalo, R., Di Leva, A., Elekes, Z., Ferraro, F., Fiore, E. M., Formicola, A., Fulop, Z., Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, G., Imbriani, G., Janas, Z., Junker, M., Kochanek, I., Lugaro, M., Marigo, P., Masha, E., Mazzocchi, C., Menegazzo, R., Mossa, V., Pantaleo, F. R., Paticchio, V., Perrino, R., Piatti, D., Prati, P., Schiavulli, L., Stockel, K., Straniero, O., Szucs, T., Takacs, M. P., Terrasi, F., and Zavatarelli, S.

Subjects
Underground laboratory, Nuclear Astrophysics, Helium-3 counter, Low-background, Neutron, Nuclear Astrophysic, Nuclear Experiment
Abstract

We introduce the LUNA neutron detector array developed for the investigation of the 13C(α, n)16O reaction towards its astrophysical s-process Gamow peak in the low-background environment of the Laboratori Nazionali del Gran Sasso (LNGS). Eighteen 3He counters are arranged in two different configurations (in a vertical and a horizontal orientation) to optimize neutron detection efficiency, target handling and target cooling over the investigated energy range Eα,lab=300−400 keV (En=2.2−2.6MeV in emitted neutron energy). As a result of the deep underground location, the passive shielding of the setup and active background suppression using pulse shape discrimination, we reached a total background rate of 1.23±0.12 counts/hour. This resulted in an improvement of two orders of magnitude over the state of the art allowing a direct measurement of the 13C(α, n)16O cross-section down to Eα,lab=300 keV. The absolute neutron detection efficiency of the setup was determined using the 51V(p,n)51Cr reaction and an AmBe radioactive source, and completed with a Geant4 simulation. We determined a (34 ± 3)% and (38 ± 3)% detection efficiency for the vertical and horizontal configurations, respectively, for En=2.4MeV neutrons.

Published
2021
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3. Direct Measurement of the (formula presented) Reaction at LUNA

Author

Ciani G. F., Csedreki L., Balibrea-Correa J., Best A., Ciani, G. F., Csedreki, L., Balibrea-Correa, J., and Best, A.

Subjects
LUNA, Nuclear astrophysic, Neutron, s-process
Abstract

The (formula presented) reaction is the main neutron source for the s-process in low mass AGB stars. Although several direct measurements have been performed, no dataset reaches the Gamow window (140–230 keV) due to the exponential drop of the cross section (formula presented)(E) with decreasing energy. The reaction rate becomes so low that the strong cosmic background would become predominant. In order to measure the (formula presented) cross section at low energies, ancillary measurements to understand the behaviour of 99% enriched (formula presented) evaporated targets, under a high intensity alpha beam (100–200 (formula presented)A). These measurements were carried out in deep underground laboratories of Laboratori Nazionali del Gran Sasso (LNGS) in the framework of the LUNA experiment. The preliminary results are reported in this contribution.

Published
2020

4. Recent Achievements of the ERNA Collaboration

Author

Raffaele Buompane, Antonino Di Leva, Lucio Gialanella, Gianluca Imbriani, Lizeth Morales-Gallegos, Mauro Romoli, Buompane, R., Di Leva, A., Gialanella, L., Imbriani, G., Morales-Gallegos, L., and Romoli, M.

Subjects
Nuclear astrophysic, Recoil mass separator, Charge particle spectroscopy, Astrophysics::Solar and Stellar Astrophysics, General Physics and Astronomy, Carbon burning
Abstract

For more than two decades, the ERNA collaboration has investigated nuclear processes of astrophysical interest through the direct measurement of cross sections or the identification of the nucleosynthesis effects. Measurements of cross-section, reported in this publication, of radiative capture reactions have been mainly conducted using the ERNA Recoil Mass Separator, and more recently with an array of charged particle detector telescopes designed for nuclear astrophysics measurements. Some results achieved with ERNA will be reviewed, with a focus on the results most relevant for nucleosynthesis in AGB and advanced burning phases.

Published
2022
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5. Cross section of the reaction 18O(p,γ)19F at astrophysical energies: The 90 keV resonance and the direct capture component

Author

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

Subjects
Nuclear reaction, Nuclear and High Energy Physics, Experimental nuclear astrophysics, 01 natural sciences, Resonance (particle physics), Isotopes of oxygen, Stellar evolution, Reaction rate, Nuclear physics, Cross section (physics), Hydrogen burning, Underground nuclear physics, 0103 physical sciences, Experimental nuclear astrophysics Underground nuclear physics Hydrogen burning Stellar evolution, Nuclear astrophysics, 010306 general physics, Nuclear Experiment, Physics, Experimental nuclear astrophysic, 010308 nuclear & particles physics, Giant star, lcsh:QC1-999, Orders of magnitude (time), lcsh:Physics
Abstract

The observation of oxygen isotopes in giant stars sheds light on mixing processes operating in their interiors. Due to the very strong correlation between nuclear burning and mixing processes it is very important to reduce the uncertainty on the cross sections of the nuclear reactions that are involved. In this paper we focus our attention on the reaction O 18 ( p , γ ) 19 F . While the O 18 ( p , α ) 15 N channel is thought to be dominant, the (p,γ) channel can still be an important component in stellar burning in giants, depending on the low energy cross section. So far only extrapolations from higher-energy measurements exist and recent estimates vary by orders of magnitude. These large uncertainties call for an experimental reinvestigation of this reaction. We present a direct measurement of the O 18 ( p , γ ) 19 F cross section using a high-efficiency 4π BGO summing detector at the Laboratory for Underground Nuclear Astrophysics (LUNA). The reaction cross section has been directly determined for the first time from 140 keV down to 85 keV and the different cross section components have been obtained individually. The previously highly uncertain strength of the 90 keV resonance was found to be 0.53 ± 0.07 neV, three orders of magnitude lower than an indirect estimate based on nuclear properties of the resonant state and a factor of 20 lower than a recently established upper limit, excluding the possibility that the 90 keV resonance can contribute significantly to the stellar reaction rate.

Published
2019
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6. Direct measurements of low-energy resonance strengths of the 23Na(p,γ)24Mg reaction for astrophysics

Author

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

Subjects
Nuclear and High Energy Physics, Experimental nuclear astrophysics, Cosmic ray, 01 natural sciences, Stellar evolution, Reaction rate, Hydrogen burning, Underground nuclear physics, Nucleosynthesis, 0103 physical sciences, Experimental nuclear astrophysics Underground nuclear physics Hydrogen burning Stellar evolution, Nuclear astrophysics, Asymptotic giant branch, 010306 general physics, Physics, Experimental nuclear astrophysic, 010308 nuclear & particles physics, Gamma ray, Resonance, Atmospheric temperature range, lcsh:QC1-999, LUNA, 13. Climate action, Nuclear Astrophysiscs, Atomic physics, lcsh:Physics
Abstract

The NeNa and the MgAl cycles play a fundamental role in the nucleosynthesis of asymptotic giant branch stars undergoing hot bottom burning. The Na 23 ( p , γ ) 24 Mg reaction links these two cycles and a precise determination of its rate is required to correctly estimate the contribution of these stars to the chemical evolution of various isotopes of Na, Mg and Al. At temperatures of 50 ≲ T ≲ 110 MK , narrow resonances at E p = 140 and 251 keV are the main contributors to the reaction rate, in addition to the direct capture that dominates in the lower part of the temperature range. We present new measurements of the strengths of these resonances at the Laboratory for Underground Nuclear Astrophysics (LUNA). We have used two complementary detection approaches: high efficiency with a 4π BGO detector for the 140 keV resonance, and high resolution with a HPGe detector for the 251 keV resonance. Thanks to the reduced cosmic ray background of LUNA, we were able to determine the resonance strength of the 251 keV resonance as ω γ = 482 ( 82 ) μ eV and observed new gamma ray transitions for the decay of the corresponding state in Mg 24 at E x = 11931 keV . With the highly efficient BGO detector, we observed a signal for the 140 keV resonance for the first time in a direct measurement, resulting in a strength of ω γ 140 = 1.46 − 0.53 + 0.58 neV (68% CL). Our measurement reduces the uncertainty of the Na 23 ( p , γ ) 24 Mg reaction rate in the temperature range from 0.05 to 0.1 GK to at most − 35 % + 50 % at 0.07 GK. Accordingly, our results imply a significant reduction of the uncertainties in the nucleosynthesis calculations.

Published
2019
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7. Observatory science with eXTP

Author

in't Zand, Jean J. M., Bozzo, Enrico, Qu, Jinlu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen A., Hernanz, Margarita, Jenke, Peter A., Maccarone, Thomas J., Mahmoodifar, Simin, De Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena M., Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas M., Wilms, Joern, Wu, Xuefeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils A., Baglio, M. Cristina, Ballantyne, David R., Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, Joao, Brandt, Søren, Brown, Edward F., Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward M., Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, Chichuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D'Aì, Antonino, Dai, Zi-Gao, D'Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D'Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, Xilong, Ferdman, Robert D., Feroci, Marco, Fraschetti, Federico, Galloway, Duncan K., Gambino, Angelo F., Gandhi, Poshak, Ge, Mingyu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig O., Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter G., José, Jordi, Kaastra, Jelle S., Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Laurens, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, Fangjun, Lutovinov, Alexander A., Malyshev, Denys, Malzac, Julien, Manousakis, Antonios, McHardy, Ian, Mehdipour, Missagh, Men, Yunpeng, Méndez, Mariano, Mignani, Roberto P., Mikusincova, Romana, Miller, M. Coleman, Miniutti, Giovanni, Motch, Christian, Nättilä, Joonas, Nardini, Emanuele, Neubert, Torsten, O'Brien, Paul T., Orlandini, Mauro, Osborne, Julian P., Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif E., Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel A., Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuomas, Schanne, Stéphane, Schatz, Hendrik, Shao, Lijing, Shearer, Andy, Shore, Steven N., Stappers, Ben W., Strohmayer, Tod E., Suleimanov, Valery F., Svoboda, Jir̆í, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego F., Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, Junfeng, Watts, Anna L., Weng, Shanshan, Weinberg, Nevin N., Wheatley, Peter J., Wijnands, Rudy, Woods, Tyrone E., Woosley, Stan E., Xiong, Shaolin, Xu, Yupeng, Yan, Zhen, Younes, George, Yu, Wenfei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, Zingale, Michael, in ’t Zand, Jean, Drake, Stephen, Jenke, Peter, Maccarone, Thomas, Rossi, Elena, Tauris, Thomas, Andersson, Nils, Ballantyne, David, Brown, Edward, Cackett, Edward, D’Aì, Antonino, D’Ammando, Filippo, D’Elia, Valerio, Ferdman, Robert, Galloway, Duncan, Gambino, Angelo, Heinke, Craig, Jonker, Peter, Kaastra, Jelle, Lutovinov, Alexander, Mignani, Roberto, O’Brien, Paul, Osborne, Julian, Papadakis, Iossif, Pérez Torres, Miguel, Shore, Steven, Stappers, Ben, Strohmayer, Tod, Suleimanov, Valery, Torres, Diego, Watts, Anna, Weinberg, Nevin, Wheatley, Peter, Woods, Tyrone, Woosley, Stan, Zdziarski, Andrzej, in ’t Zand, Jean J. M., Bozzo, Enrico, Qu, JinLu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen A., Hernanz, Margarita, Jenke, Peter A., Maccarone, Thomas J., Mahmoodifar, Simin, de Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena M., Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas M., Wilms, Joern, Wu, XueFeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils A., Baglio, M. Cristina, Ballantyne, David R., Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, João, Brandt, Søren, Brown, Edward F., Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward M., Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, ChiChuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D’Aì, Antonino, Dai, Zi-Gao, D’Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D’Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, XiLong, Ferdman, Robert D., Feroci, Marco, Fraschetti, Federico, Galloway, Duncan K., Gambino, Angelo F., Gandhi, Poshak, Ge, MingYu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig O., Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter G., José, Jordi, Kaastra, Jelle S., Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Lauren, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, FangJun, Lutovinov, Alexander A., Malyshev, Deny, Malzac, Julien, Manousakis, Antonio, McHardy, Ian, Mehdipour, Missagh, Men, YunPeng, Méndez, Mariano, Mignani, Roberto P., Mikusincova, Romana, Miller, M. Coleman, Miniutti, Giovanni, Motch, Christian, Nättilä, Joona, Nardini, Emanuele, Neubert, Torsten, O’Brien, Paul T., Orlandini, Mauro, Osborne, Julian P., Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif E., Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel A., Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuoma, Schanne, Stéphane, Schatz, Hendrik, Shao, LiJing, Shearer, Andy, Shore, Steven N., Stappers, Ben W., Strohmayer, Tod E., Suleimanov, Valery F., Svoboda, Jirí, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego F., Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, JunFeng, Watts, Anna L., Weng, ShanShan, Weinberg, Nevin N., Wheatley, Peter J., Wijnands, Rudy, Woods, Tyrone E., Woosley, Stan E., Xiong, ShaoLin, Xu, YuPeng, Yan, Zhen, Younes, George, Yu, WenFei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, Zingale, Michael, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), eXTP, Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre de Recherche en Information Biomédicale sino-français (CRIBS), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Southeast University [Jiangsu]-Institut National de la Santé et de la Recherche Médicale (INSERM), Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), ASI Science Data Center (ASDC), Italian Space Agency, INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Anthropobiologie (LA), École des hautes études en sciences sociales (EHESS)-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), SRON Netherlands Institute for Space Research (SRON), Istituto di Radioastronomia [Bologna] (IRA), KAUST Catalysis Center (KCC), King Abdullah University of Sciences & Technologie, IASF, Area di Ricerca di Tor Vergata, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Southampton], University of Southampton, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut für Astrophysik [Wien], Universität Wien, Sabanci University [Istanbul], The George Washington University (GW), Department of Physics, Tokyo Institute of Technology [Tokyo] (TITECH), Deakin University [Burwood], Copernicus Astronomical Center of the Polish Academy of Sciences (CAMK), Polish Academy of Sciences (PAN), University of New Hampshire (UNH), Department of Mechanical and Industrial Engineering [Trondheim] (MTP NTNU), Norwegian University of Science and Technology [Trondheim] (NTNU), Norwegian University of Science and Technology (NTNU)-Norwegian University of Science and Technology (NTNU), Ethoikos, Radicondoli, Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Sichuan University [Chengdu] (SCU), University of Warwick [Coventry], U.S. Department of Energy [Washington] (DOE), University College of London [London] (UCL), Medical School (University of Nanjing), Nanjing University (NJU), Beijing Municipal Climate Center, Max-Planck-Institut für Radioastronomie (MPIFR), Laboratorio de Investigación y Formación en Informática Avanzada [La Plata] (LIFIA), Facultad de Informática [La Plata], Universidad Nacional de la Plata [Argentine] (UNLP)-Universidad Nacional de la Plata [Argentine] (UNLP), NLD, Unidad de Excelencia Científica María de Maeztu Instituto de Ciencias del Cosmos (ICCUB), MDM-2014-0369, National Natural Science Foundation of China (NSFC), European Research Council (ERC), National Aeronautics and Space Administration (NASA), Agencia Estatal de Investigación (AEI), Royal Society, Strategic Priority Research Program of the Chinese Academy of Sciences, National Science Centre, Poland (NCN), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Royal Society (UK), European Research Council, European Commission, National Natural Science Foundation of China, National Basic Research Program (China), National Science Foundation (US), Ministerio de Economía y Competitividad (España), Polish Academy of Sciences, Astronomy, Discrete Technology and Production Automation, in't Zand, Jean J. M., Qu, Jinlu, Tauris, Thomas M., Wilm, Joern, Wu, Xuefeng, Jin, Chichuan, D'Aì, Antonino, D'Ammando, Filippo, D'Elia, Valerio, Fan, Xilong, Ge, Mingyu, Lu, Fangjun, Mchardy, Ian, Men, Yunpeng, O'Brien, Paul T., Shao, Lijing, Svoboda, Jir̆í, Thielemann, F. -K., Wang, Junfeng, Weng, Shanshan, Xiong, Shaolin, Xu, Yupeng, Yu, Wenfei, Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica, Institut de Mathématiques de Toulouse UMR5219 (IMT), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Osservatorio Astronomico di Brera, Istituto di Radioastronomia (IRA), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), George Washington University (GW), Department of Mechanical and Industrial Engineering [Trondheim], Sichuan University, U.S. Department of Energy (DOE), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), SRON Netherlands Institute for Space Research, University of Geneva, CAS - Institute of High Energy Physics, Nanjing University, INAF/IASF Bologna, National Institute for Astrophysics, University of Tübingen, NASA Goddard Space Flight Center, ICREA, University of Alabama in Huntsville, Texas Tech University, Osservatorio Astronomico di Capodimonte, Leiden University, University of Amsterdam, Polytechnic University of Catalonia, University of Urbino, Max Planck Institute for Radio Astronomy, Friedrich-Alexander University Erlangen-Nürnberg, CAS - Purple Mountain Observatory, CSIC, IRAP, New York University Abu Dhabi, Georgia Institute of Technology, Middle East Technical University, Technion-Israel Institute of Technology, Tata Institute of Fundamental Research, Roma Tre University, Instituto de Astrofísica de Canarias, Instituto Nacional de Pesquisas Espaciais, Danmarks Tekniske Universitet, Michigan State University, Osservatorio Astrofisico Di Arcetri, Florence, University of Cagliari, Wayne State University, Osservatorio Astronomico Roma, CAS - Shanghai Astronomical Observatory, Department of Electronics and Nanoengineering, Aalto-yliopisto, and Aalto University

Subjects
cataclysmic binaries, Astronomy, FIELD CAMERAS OBSERVATIONS, space research instruments nuclear astrophysics flare stars accretion and accretion disks mass loss and stellar winds cataclysmic binaries X-ray binaries supernova remnants active galactic nuclei X-ray bursts gamma-ray bursts gravitational waves, General Physics and Astronomy, gamma-ray burst, space research instrument, 01 natural sciences, Gamma ray bursts, Observatory, Accretion and accretion disks, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, gravitational wave, accretion and accretion disk, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), supernova remnants, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], flare stars, gamma-ray bursts, Astrophysics::Instrumentation and Methods for Astrophysics, accretion and accretion disks, active galactic nuclei, gravitational waves, mass loss and stellar winds, nuclear astrophysics, space research instruments, X-ray binaries, X-ray bursts, Physics and Astronomy (all), Space research instruments, X ray burst, Supernova, QUIET, High mass, X-ray binarie, Mass loss and stellar winds, Nuclear astrophysics, Gamma-ray bursts, Astrophysics - High Energy Astrophysical Phenomena, PULSAR-WIND NEBULAE, FAST RADIO-BURSTS, Astrofísica nuclear, Active galactic nucleus, TIDAL DISRUPTION, Supernova remnants, Astrophysics::High Energy Astrophysical Phenomena, Polarimetry, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, ACCRETING NEUTRON-STARS, Gravitational waves, cataclysmic binarie, Settore FIS/05 - Astronomia e Astrofisica, SUPERMASSIVE BLACK-HOLES, 0103 physical sciences, 010306 general physics, X-ray burst, Astrophysics::Galaxy Astrophysics, Cataclysmic binaries, Active galactic nuclei, flare star, White dwarf, Flare stars, Stars, supernova remnant, QB460-466 Astrophysics, [SDU]Sciences of the Universe [physics], mass loss and stellar wind, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], X-RAY, Supernova remmants, X ray binaries, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], SEYFERT 1 GALAXY, nuclear astrophysic
Abstract

Disponible preprint en: arXiv:1812.04023v1 [astro-ph.HE] [v1] Mon, 10 Dec 2018 19:00:52 UTC (4,376 KB), In this White Paper we present the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to Observatory Science targets. These include flaring stars, supernova remnants, accreting white dwarfs, low and high mass X-ray binaries, radio quiet and radio loud active galactic nuclei, tidal disruption events, and gamma-ray bursts. eXTP will be excellently suited to study one common aspect of these objects: their often transient nature. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s.© 2018, Science China Press and Springer-Verlag GmbH Germany, part of Springer Nature., This work was supported by the Royal Society, ERC Starting (Grant No. 639217), the European Union Horizon 2020 Research and Innovation Programme under the Marie Sklodowska-Curie Global Fellowship (Grant No. 703916), the National Natural Science Foundation of China (Grant Nos. 11233001, 11773014, 11633007, 11403074, 11333005, 11503008, and 11590781), the National Basic Research Program of China (Grant No. 2015CB857100), NASA (Grant No. NNX13AD28A), an ARC Future Fellowship (Grant No. FT120100363), the National Science Foundation (Grant No. PHY-1430152), the Spanish MINECO (Grant No. AYA2016-76012-C3-1-P), the ICCUB (Unidad de Excelencia 'Maria de Maeztu') (Grant No. MDM-2014-0369), EU's Horizon Programme through a Marie Sklodowska-Curie Fellowship (Grant No. 702638), the Polish National Science Center (Grant Nos. 2015/17/B/ST9/03422, 2015/18/M/ST9/00541, 2013/10/M/ST9/00729, and 2015/18/A/ST9/00746), the Strategic Priority Research Program of the Chinese Academy of Sciences (Grant No. XDA15020100), and the NWO Veni Fellowship (Grant No. 639.041.647).

Published
2019
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8. 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

9. The e-ASTROGAM mission: Exploring the extreme Universe with gamma rays in the MeV – GeV range

Author

Barbara Patricelli, V. Bonvicini, Riccardo Rando, Sandro Mereghetti, Andrea Vacchi, Kazuhiro Nakazawa, Claudio Labanti, Jordi Isern, M. Hayashida, Josep M. Paredes, J. Eric Grove, C. Hamadache, Andreas Zoglauer, Olivier Limousin, Julie McEnery, Andrei M. Bykov, G. Ambrosi, D. de Martino, Francesco Longo, Irfan Kuvvetli, Alexander Moiseev, Xin Wu, Fabrizio Tavecchio, I. Donnarumma, M. I. Martínez, Marco Tavani, J. Peyré, Elisa Bernardini, A. Argan, Roland Walter, J. Kiener, Piotr Orleanski, Mark Pearce, Ignasi Reichardt, A. Morselli, Andrzej A. Zdziarski, Martino Marisaldi, Vincent Tatischeff, Andrea Bulgarelli, Marica Branchesi, Uwe Oberlack, Rui Curado da Silva, Dieter H. Hartmann, Lorraine Hanlon, Philippe Laurent, Marco Ajello, D. Bernard, Valentina Fioretti, Martin Pohl, Alessio Aboudan, Gottfried Kanbach, Alessandro De Angelis, Gabriele Ghisellini, Stefan Funk, Peter von Ballmoos, Michele Doro, M. N. Mazziotta, Marco Roncadelli, Harald Ramarijaona, Roland Diehl, Margarita Hernanz, Alexei Ulyanov, G. Minervini, G. Piano, Riccardo Campana, Carl Budtz-Jørgensen, D. J. Thompson, M. Cardillo, Paolo De Coppi, Karl Mannheim, Roberto Turolla, Jürgen Knödlseder, Isabelle Grenier, A. Brogna, De Angelis, A., Tatischeff, V., Tavani, M., Oberlack, U., Grenier, I., Hanlon, L., Walter, R., Argan, A., von Ballmoos, P., Bulgarelli, A., Donnarumma, I., Hernanz, M., Kuvvetli, I., Pearce, M., Zdziarski, A., Aboudan, A., Ajello, M., Ambrosi, G., Bernard, D., Bernardini, E., Bonvicini, V., Brogna, A., Branchesi, M., Budtz-Jorgensen, C., Bykov, A., Campana, R., Cardillo, M., Coppi, P., De Martino, D., Diehl, R., Doro, M., Fioretti, V., Funk, S., Ghisellini, G., Grove, E., Hamadache, C., Hartmann, D. H., Hayashida, M., Isern, J., Kanbach, G., Kiener, J., Knödlseder, J., Labanti, C., Laurent, P., Limousin, O., Longo, F., Mannheim, K., Marisaldi, M., Martinez, M., Mazziotta, M. N., Mcenery, J., Mereghetti, S., Minervini, G., Moiseev, A., Morselli, A., Nakazawa, K., Orleanski, P., Paredes, J. M., Patricelli, B., Peyré, J., Piano, G., Pohl, M., Ramarijaona, H., Rando, R., Reichardt, I., Roncadelli, M., Silva, R., Tavecchio, F., Thompson, D. J., Turolla, R., Ulyanov, A., Vacchi, A., Wu, X., Zoglauer, A., and ITA

Subjects
Counterparts of gravitational wave, Multiwavelength Observations of the Universe, 01 natural sciences, Early Universe, Observatory, Jets, Nuclear Astrophysics, Nuclear astrophysics, Dark Matter, Nuclear Experiment (nucl-ex), Nuclear Astrophysic, Nuclear Experiment, 010303 astronomy & astrophysics, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::Instrumentation and Methods for Astrophysics, Counterparts of gravitational waves, Gamma-Ray Burst, Cosmic Rays, Compton and Pair Creation Telescope, Supernovae, Astrophysics - Solar and Stellar Astrophysics, High-Energy Astrophysics, Active Galactic Nuclei, Cosmic Antimatter, Fermi, Gamma-Ray Bursts, High-Energy Gamma-Ray Astronomy, Nucleosynthesis, Outflows, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Active galactic nucleus, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmic Ray, High-Energy Astrophysic, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Nucleosynthesi, 010308 nuclear & particles physics, Institut für Physik und Astronomie, Astronomy, Outflow, Astronomy and Astrophysic, Universe, Galaxy, Jet, Fermi Gamma-ray Space Telescope
Abstract

e-ASTROGAM (`enhanced ASTROGAM') is a breakthrough Observatory mission dedicated to the study of the non-thermal Universe in the photon energy range from 0.3 MeV to 3 GeV. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with polarimetric capability. In the largely unexplored MeV-GeV domain, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on Galactic ecosystems. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous generation instruments, will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LIGO-Virgo-GEO600-KAGRA, SKA, ALMA, E-ELT, TMT, LSST, JWST, Athena, CTA, IceCube, KM3NeT, and the promise of eLISA. Keywords: High-energy gamma-ray astronomy, High-energy astrophysics, Nuclear Astrophysics, Compton and Pair creation telescope, Gamma-ray bursts, Active Galactic Nuclei, Jets, Outflows, Multiwavelength observations of the Universe, Counterparts of gravitational waves, Fermi, Dark Matter, Nucleosynthesis, Early Universe, Supernovae, Cosmic Rays, Cosmic antimatter., Comment: Exp Astron (2017)

Published
2017

10. Cross-section measurements at astrophysically relevant energies: The LUNA experiment

Author

C. G. Bruno, Gianluca Imbriani, Davide Trezzi, C. Gustavino, Carlo Broggini, Gy. Gyürky, G. Gervino, Daniel Bemmerer, A. Di Leva, M. Junker, Tamás Szücs, Paolo Prati, R. Menegazzo, Antonio Caciolli, E. Somorjai, A. Formicola, M. Anders, F. Cavanna, Z. Elekes, Douglas Scott, P. Corvisiero, Rosanna Depalo, Frank Strieder, Oscar Straniero, Marialuisa Aliotta, Zs. Fülöp, A. Guglielmetti, A., Formicola, C. G., Bruno, A., Caciolli, F., Cavanna, R., Depalo, DI LEVA, Antonino, D. A., Scott, D., Trezzi, M., Aliotta, M., Ander, D., Bemmerer, C., Broggini, P., Corvisiero, Z., Eleke, F?l?p, Z. s., G., Gervino, A., Guglielmetti, C., Gustavino, Gy?rky, G. y., Imbriani, Gianluca, M., Junker, R., Menegazzo, P., Prati, E., Somorjai, O., Straniero, F., Strieder, and T., Sz?cs

Subjects
Nuclear and High Energy Physics, S-factor, Underground accelerator, Astrophysics::High Energy Astrophysical Phenomena, Measure (physics), Astrophysics::Cosmology and Extragalactic Astrophysics, Luminosity, Nuclear physics, Nucleosynthesis, Nuclear astrophysics, Astrophysics::Solar and Stellar Astrophysics, underground measurements, Nuclear Astrophysic, Nuclear Experiment, Instrumentation, Astrophysics::Galaxy Astrophysics, Experimental Nuclear Physic, Physics, COSMIC cancer database, Solar fusion, LUNA, Stars, Neutrino, Big Bang nucleosynthesis, Direct cross-section
Abstract

Accurate knowledge of thermonuclear reaction rates is important in understanding the generation of energy, the luminosity of neutrinos, and the synthesis of elements in stars. Cross-section measurements for quiescent stellar H-burning are mainly hampered by extremely low counting rate and cosmic background. The LUNA Collaboration has shown that, by going underground and by using the typical techniques of low background physics, it is possible to measure nuclear cross-sections down to the energy of the nucleosynthesis inside stars. This paper reports an overview of the experimental techniques adopted in underground nuclear astrophysics through a summary of the main recent results and achievements. The future developments of the LUNA experiment are also given. © 2013 Elsevier B.V. All rights reserved.

Published
2014
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11. S-factor of 14N(p,γ)15O at astrophysical energies⋆

Author

M. Junker, C. Rolfs, Mario R. Romano, A. Lemut, E. Somorjai, Carlo Broggini, A. Formicola, Gianluca Imbriani, J. N. Klug, Gy. Gyürky, Alberto Vomiero, A. Guglielmetti, C. Gustavino, R. Bonetti, Daniel Bemmerer, R. Menegazzo, C. Rossi Alvarez, D. Schürmann, Zs. Fülöp, Frank Strieder, A. P. Jesus, F. Confortola, P. Corvisiero, Vincenzo Roca, G. Gervino, Oscar Straniero, Filippo Terrasi, Carmen Angulo, H. Costantini, F. Schümann, Paolo Prati, Jenniffer Cruz, H. P. Trautvetter, Pierre Descouvemont, Imbriani, Gianluca, H., Costantini, A., Formicola, A., Vomiero, C., Angulo, D., Bemmerer, R., Bonetti, C., Broggini, F., Confortola, P., Corvisiero, J., Cruz, P., Descouvemont, Z., Fülöp, G., Gervino, A., Guglielmetti, C., Gustavino, Gyürky, G. y., A. P., Jesu, M., Junker, J. N., Klug, A., Lemut, R., Menegazzo, P., Prati, Roca, Vincenzo, C., Rolf, Romano, Mario, C., Rossi Alvarez, F., Schümann, D., Schürmann, E., Somorjai, O., Straniero, F., Strieder, F., Terrasi, H. P., Trautvetter, Z., Fulop, Gyurky, G. Y., C., ROSSI ALVAREZ, F., Schumann, and D., Schurmann

Subjects
Experimental Nuclear Physic, Physics, Nuclear and High Energy Physics, Work (thermodynamics), 010308 nuclear & particles physics, S-factor, FOS: Physical sciences, chemistry.chemical_element, underground laboratory, 01 natural sciences, Nuclear physics, chemistry, 0103 physical sciences, Level structure, Nuclear Experiment (nucl-ex), Nuclear Astrophysic, Tin, Nuclear Experiment, 010303 astronomy & astrophysics, Value (mathematics)
Abstract

The astrophysical S-factor of 14N(p,gamma)15O has been measured for effective center-of-mass energies between E_eff = 119 and 367 keV at the LUNA facility using TiN solid targets and Ge detectors. The data are in good agreement with previous and recent work at overlapping energies. R-matrix analysis reveals that due to the complex level structure of 15O the extrapolated S(0) value is model dependent and calls for additional experimental efforts to reduce the present uncertainty in S(0) to a level of a few percent as required by astrophysical calculations., Comment: Eur. Phys. J. A, accepted. 17 pages, 15 figures

Published
2005
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12. A new study of the 14N(p,γ)15O reaction at low energy

Author

Gianluca Imbriani, A. Formicola, H. Costantini, A., Formicola, H., Costantini, and Imbriani, Gianluca

Subjects
Experimental Nuclear Physic, Physics, Nuclear reaction, Nuclear and High Energy Physics, Particle physics, Measure (physics), Coulomb barrier, Electron, underground laboratory, Charged particle, Cosmology, Nuclear physics, Cross section (physics), Nuclear astrophysics, Nuclear Astrophysic, Nuclear Experiment
Abstract

Precise knowledge of nuclear cross sections at stellar energies is of importance for cosmology as well as for nuclear astrophysics. Measuring these cross sections at the relevant energies is quite challenging not only for the extremely low cross sections involved but also because a lot of parameters like stopping powers and electron screening are not well known at low energies. The LUNA collaboration has installed a second high current accelerator of 400kV at the underground laboratory of Gran Sasso. It is dedicated to measure the cross section of charged particle induced nuclear reactions of astrophysical interest at energies far below the respective Coulomb barrier and possibly close or within the associated Gamow energy.

Published
2003
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13. Underground study of the O17(p,g)F18 reaction relevant for explosive hydrogen burning

Author

DI LEVA, ANTONINO, D. A. Scott, A. Caciolli, A. Formicola, F. Strieder, M. Aliotta, M. Anders, D. Bemmerer, C. Broggini, P. Corvisiero, Z. Elekes, Z.s. F?l?p, G. Gervino, A. Guglielmetti, C. Gustavino, G.y. Gy?rky, IMBRIANI, GIANLUCA, J. Jos?, M. Junker, M. Laubenstein, R. Menegazzo, E. Napolitani, P. Prati, V. Rigato, ROCA, VINCENZO, E. Somorjai, C. Salvo, O. Straniero, T. Sz?cs, F. Terrasi, D. Trezzi, DI LEVA, Antonino, D. A., Scott, A., Caciolli, A., Formicola, F., Strieder, M., Aliotta, M., Ander, D., Bemmerer, C., Broggini, P., Corvisiero, Z., Eleke, F?l?p, Z. s., G., Gervino, A., Guglielmetti, C., Gustavino, Gy?rky, G. y., Imbriani, Gianluca, J., Jos?, M., Junker, M., Laubenstein, R., Menegazzo, E., Napolitani, P., Prati, V., Rigato, Roca, Vincenzo, E., Somorjai, C., Salvo, O., Straniero, T., Sz?c, F., Terrasi, and D., Trezzi

Subjects
Nuclear Astrophysic, underground measurement, Experimental Nuclear Physics
Abstract

Background: The O17(p,γ)F18 reaction affects the production of key isotopes (e.g., F18 and O18) in the explosive hydrogen burning that powers classical novae. Under these explosive conditions, the reaction rate is dominated by contributions from a narrow resonance at Ec.m.=183keV and by the combined contributions of direct capture and low-energy tails of broad resonances. At present, the astrophysical reaction rate is not well constrained because of the lack of data in the energy region appropriate to classical novae. Purpose: This study aims at the measurement of the O17(p,γ)F18 reaction cross section in order to determine its reaction rate in the temperature region appropriate to explosive hydrogen burning in novae. Method: The O17(p,γ)F18 reaction cross section was measured using both the prompt detection of the emitted γ rays and an activation technique. Measurements were carried out at the Laboratory for Underground Nuclear Astrophysics (Gran Sasso, Italy) where the strongly reduced cosmic-ray-induced background allows for improved sensitivity compared to previous studies. Results: The O17(p,γ)F18 reaction cross section was measured in the range Ec.m.=160 to 370keV. The strength of the Ec.m.=183keV resonance, ωγ=1. 67±0.12μeV, was determined with unprecedented precision. The total S factor was obtained through a combined fit of prompt γ-ray and activation results. An overall global fit including other existing data sets was also carried out and a recommended astrophysical reaction rate is presented. Conclusions: The reaction rate uncertainty attained in this work 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.

Published
2014

14. Absolute cross section of 7Be(p,γ)8B

Author

Uwe Greife, Zs. Fülöp, F. Schümann, L. Campajola, Antonio D'Onofrio, Gianluca Imbriani, C. Rolfs, Lucio Gialanella, Vincenzo Roca, P. Corvisiero, Paolo Prati, Frank Strieder, Sandra Zavatarelli, G. Gervino, Oscar Straniero, H. Costantini, A. Ordine, Filippo Terrasi, A. Formicola, E. Somorjai, Carlo Broggini, C. Gustavino, P. G. Prada Moroni, A. Guglielmetti, R. Bonetti, Gy. Gyürky, H. P. Trautvetter, M. Junker, Mario R. Romano, Detlef Rogalla, F., Strieder, L., Gialanella, G., Gyürky, F., Schümann, R., Bonetti, C., Broggini, L., Campajola, P., Corvisiero, H., Costantini, A., D'Onofrio, A., Formicola, Z., Fülöp, G., Gervino, U., Greife, A., Guglielmetti, C., Gustavino, Imbriani, Gianluca, M., Junker, P. G. P., Moroni, A., Ordine, P., Prati, Roca, Vincenzo, D., Rogalla, C., Rolf, Romano, Mario, E., Somorjai, O., Straniero, F., Terrasi, H. P., Trautvetter, and S., Zavatarelli

Subjects
Experimental Nuclear Physic, Physics, Nuclear reaction, Nuclear and High Energy Physics, Cross section (physics), Radiative capture, Zero-point energy, Nuclide, Atomic physics, Experimental Nuclear Astrophysic, Solar neutrino, Stellar hydrogen burning
Abstract

The absolute cross section σ ( E ) for the radiative capture reaction 7 Be(p, γ ) 8 B at the center-of-mass energies E =0.32 to 2.61 MeV has been measured using a 7 Be target deposited on a Cu backing and observing the β -delayed α -particles from 8 B. The backing causes a loss of less than 1% of the 8 B residual nuclides. The resulting astrophysical S ( E ) factor at zero energy, S (0)=18.4±1.6 eV b, is consistent only with a restricted data set from previous work.

Published
2001
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15. The E1 capture amplitude in 12C(α,γ0) 16O

Author

F. Strieder, Antonio D'Onofrio, A. Ordine, Marialuisa Aliotta, Filippo Terrasi, C. Agodi, Detlef Rogalla, G. Gyürki, L. Gialanella, E. Somorjai, Vincenzo Roca, L. Campajola, Gianluca Imbriani, P. Figuera, Mario R. Romano, H. P. Trautvetter, S. Theis, Uwe Greife, A. Del Zoppo, C. Rolfs, R. Alba, F. Schümann, Paolo Sapienza, Carlo Sabbarese, Gialanella, L., Rogalla, D., Strieder, F., Theis, S., Gyurki, G., Agodi, C., Alba, R., Aliotta, M., Campajola, L., Del Zoppo, A., D'Onofrio, A., Figuera, P., Greife, U., Imbriani, G., Ordine, A., Roca, V., Rolfs, C., Romano, M., Sabbarese, C., Sapienza, P., Schumann, F., Somorjai, E., Terrasi, F., Trautvetter, H. P., L., Gialanella, D., Rogalla, F., Strieder, S., Thei, G., Gyürki, C., Agodi, R., Alba, M., Aliotta, L., Campajola, A., Del Zoppo, A., D'Onofrio, P., Figuera, U., Greife, Imbriani, Gianluca, A., Ordine, Roca, Vincenzo, C., Rolf, Romano, Mario, C., Sabbarese, P., Sapienza, F., Schümann, E., Somorjai, F., Terrasi, and H. P., Trautvetter

Subjects
Physics, Excitation function, Nuclear and High Energy Physics, S-factor, Monte Carlo method, Detector, Hadron, Extrapolation, Nuclear physics, Helium burining, Amplitude, Nuclear fusion, Experimental nuclear physic, Nuclear Astrophysic
Abstract

An excitation function of the ground-state gamma (0)-ray capture transition in C-12(alpha, gamma)O-16 at theta (gamma) = 90 degrees was obtained in far geometry using six Ge detectors, where the study of the reaction was initiated in inverse kinematics involving a windowless gas target. The detectors observed predominantly the El capture amplitude. The data at E = 1.32 to 2.99 MeV lead to an extrapolated astrophysical S factor S-E1(E-0) = 90 +/- 15 keV b at E-0 = 0.3 MeV (for the case of constructive interference between the two lowest E1 sources), in good agreement with previous works. However, a novel Monte Carlo approach in the data extrapolation reveals systematic differences between the various data sets such that a combined analysis of all available data sets could produce a biased estimate of the S-E1(E-0) value. As a consequence, the case of destructive interference between the two lowest E1 sources with S-E1(E-0) = 8 +/- 3 keV b cannot be ruled out rigorously.

Published
2001
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16. A new measurement of the E1 amplitude in 12C(α,γ0)16O

Author

L. Gialanella, Antonio D'Onofrio, E. Somorjai, Paolo Sapienza, Detlef Rogalla, C. Spitaleri, Vincenzo Roca, Frank Strieder, S. Theis, Gianluca Imbriani, L. Campajola, H. P. Trautvetter, Gyuri Gyürky, Mario R. Romano, Uwe Greife, Marialuisa Aliotta, Filippo Terrasi, C. Agodi, F. Schümann, Carlo Sabbarese, C. Rolfs, R. Alba, P. Figuera, A. Del Zoppo, L., Gialanella, M., Aliotta, D., Rogalla, C., Rolf, F., Schümann, F., Strieder, S., Thei, H. P., Trautvetter, L., Campajola, Imbriani, Gianluca, Roca, Vincenzo, Romano, Mario, A., D'Onofrio, C., Sabbarese, F., Terrasi, C., Agodi, R., Alba, A., Del Zoppo, P., Figuera, P., Sapienza, C., Spitaleri, G., Gyurky, E., Somorjai, and U., Greife

Subjects
Experimental Nuclear Physic, Physics, Nuclear and High Energy Physics, Amplitude, Quantum electrodynamics, Helium burning in Stars, Nuclear Astrophysic
Abstract

The El amplitude of the transition to the ground state in the C-12(alpha, gamma)O-16 capture reaction was measured in the energy range E-cm=1.3 to 3.0 MeV using an intense C-12 beam in combination with a windowless He-4 gas target and an array of six 70% HPGe detectors. The detectors were placed in a ring-shaped geometry around the target at a distance of 17 cm on a plane perpendicular to the beam axis. A target length of 5.3 cm was defined by a 12.5 cm thick lead shielding. Passive and active shielding was used to achieve the necessary suppression of the beam induced and cosmic background. The results of this measurement and their extrapolation to the relevant energy during the helium burning phase in massive stars are reported.

Published
2001
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17. First Direct Measurement of the ^{17}O(p,\gamma)^{18}F Reaction Cross-Section at Gamow Energies for Classical Novae

Author

D. A. Scott, A. Caciolli, A. Formicola, M. Aliotta, M. Anders, D. Bemmerer, C. Broggini, M. Campeggio, P. Corvisiero, Z. Elekes, Z.s. Fulop, G. Gervino, A. Guglielmetti, C. Gustavino, G.y. Gyurky, M. Junker, M. Laubenstein, R. Menegazzo, M. Marta, E. Napolitani, P. Prati, V. Rigato, E. Somorjai, C. Salvo, O. Straniero, F. Strieder, T. Szus, F. Terrasi, D. Trezzi, DI LEVA, ANTONINO, IMBRIANI, GIANLUCA, ROCA, VINCENZO, D. A., Scott, A., Caciolli, DI LEVA, Antonino, A., Formicola, M., Aliotta, M., Ander, D., Bemmerer, C., Broggini, M., Campeggio, P., Corvisiero, Z., Eleke, Fulop, Z. s., G., Gervino, A., Guglielmetti, C., Gustavino, Gyurky, G. y., Imbriani, Gianluca, M., Junker, M., Laubenstein, R., Menegazzo, M., Marta, E., Napolitani, P., Prati, V., Rigato, Roca, Vincenzo, E., Somorjai, C., Salvo, O., Straniero, F., Strieder, T., Szu, F., Terrasi, and D., Trezzi

Subjects
Nuclear astrophysic, Proton-capture reaction, Astrophysics - Solar and Stellar Astrophysics, Reaction rate, CNO cycle, Nuclear Experiment
Abstract

Classical novae are important contributors to the abundances of key isotopes, such as the radioactive ^{18}F, whose observation by satellite missions could provide constraints on nucleosynthesis models in novae. The ^{17}O(p,\gamma)^{18}F reaction plays a critical role in the synthesis of both oxygen and fluorine isotopes but its reaction rate is not well determined because of the lack of experimental data at energies relevant to novae explosions. In this study, the reaction cross section has been measured directly for the first time in a wide energy range Ecm = 200 - 370 keV appropriate to hydrogen burning in classical novae. In addition, the E=183 keV resonance strength, \omega \gamma=1.67\pm0.12 \mueV, has been measured with the highest precision to date. The uncertainty on the ^{17}O(p,\gamma)^{18}F reaction rate has been reduced by a factor of 4, thus leading to firmer constraints on accurate models of novae nucleosynthesis., Comment: accepted by Phys. Rev. Lett

Published
2012

18. Proton capture on 17O and its astrophysical implications

Author

Manoel Couder, Ethan Uberseder, Joachim Görres, D. Schürmann, Q. Li, Edward Stech, G. Imbriani, Donald Robertson, A. Best, Richard deBoer, A. Kontos, Michael Wiescher, A., Konto, J., Görre, Best, Andrea, M., Couder, R., Deboer, Imbriani, Gianluca, Q., Li, D., Robertson, D., Schürmann, E., Stech, E., Uberseder, and M., Wiescher

Subjects
Physics, Experimental Nuclear Physic, Nuclear and High Energy Physics, Work (thermodynamics), Range (particle radiation), Proton, 010308 nuclear & particles physics, Resonance, FOS: Physical sciences, 7. Clean energy, 01 natural sciences, Lower energy, Nuclear physics, Reaction rate, Cross section (physics), 13. Climate action, Nucleosynthesis, 0103 physical sciences, Shell Hydrogen burning in stars, Nuclear Experiment (nucl-ex), 010306 general physics, Nuclear Astrophysic, Nuclear Experiment
Abstract

The reaction $^{17}$O$(p,\gamma)^{18}$F influences hydrogen-burning nucleosynthesis in several stellar sites, such as red giants, asymptotic giant branch (AGB) stars, massive stars and classical novae. In the relevant temperature range for these environments ($T_{9}=0.01-0.4), the main contributions to the rate of this reaction are the direct capture process, two low lying narrow resonances ($E_{r}=65.1$ and 183 keV) and the low-energy tails of two broad resonances ($E_{r}=557$ and 677 keV). Previous measurements and calculations give contradictory results for the direct capture contribution which in turn increases the uncertainty of the reaction rate. In addition, very few published cross section data exist for the high energy region that might affect the interpretation of the direct capture and the contributions of the broad resonances in the lower energy range. This work aims to address these issues. The reaction cross section was measured in a wide proton energy range ($E_{c.m.}=345$ - 1700 keV) and at several angles ($\theta_{lab}=0^{\circ},45^{\circ},90^{\circ},135^{\circ}$). The observed primary $\gamma$-transitions were used as input in an $R$-matrix code in order to obtain the contribution of the direct capture and the two broad resonances to the low-energy region. The extrapolated S-factor from the present data is in good agreement with the existing literature data in the low-energy region. A new reaction rate was calculated from the combined results of this work and literature S-factor determinations. Resonance strengths and branchings are reported for several $^{18}$F states. We were able to extrapolate the astrophysical S-factor of the reaction $^{17}$O$(p,\gamma)^{18}$F at low energies from cross section data taken at higher energies. No significant changes in the nucleosynthesis are expected from the newly calculated reaction rate., Comment: Accepted in Physical Review C

Published
2012

19. The25Mg(p, γ)26Al reaction at low astrophysical energies

Author

A. Best, M. Junker, Antonio Caciolli, E. Somorjai, C. Rolfs, A. Lemut, Z. Elekes, P. Corvisiero, C. Gustavino, Oscar Straniero, Frank Strieder, Gianluca Imbriani, Michele Marta, Filippo Terrasi, A. Formicola, C. Rossi Alvarez, Daniel Bemmerer, H. P. Trautvetter, Vincenzo Roca, A. DiLeva, Paolo Prati, Zsolt Fülöp, B. Limata, Roberto Menegazzo, Gyuri Gyürky, G. Gervino, A. Guglielmetti, H. Costantini, Carlo Broggini, C. Mazzocchi, F., Strieder, Limata, BENEDICTA NORMANNA, A., Formicola, Imbriani, Gianluca, M., Junker, D., Bemmerer, Best, Andrea, C., Broggini, A., Caciolli, P., Corvisiero, H., Costantini, DI LEVA, Antonino, Z., Eleke, Fülöp, Z. s., G., Gervino, A., Guglielmetti, C., Gustavino, Gyürky, G. y., A., Lemut, M., Marta, C., Mazzocchi, R., Menegazzo, P., Prati, Roca, Vincenzo, C., Rolf, C., Rossi Alvarez, E., Somorjai, O., Straniero, F., Terrasi, and H. P., Trautvetter

Subjects
Physics, Nuclear and High Energy Physics, Nuclear astrophysic, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Resolution (electron density), Resonance, Mg-Al cycle, Nuclear astrophysics, Proton-capture reaction, Reaction rate, Resonance strength, Crystal, Nuclear physics, Underground laboratory, High Energy Physics::Experiment, Atomic physics, Hpge detector, Nuclear Experiment
Abstract

In the present work we report on a new measurement of resonance strengths in the reaction 25Mg(p,gamma)26Al at E_cm= 92 and 189 keV. This study was performed at the LUNA facility in the Gran Sasso underground laboratory using a 4pi BGO summing crystal. For the first time the 92 keV resonance was directly observed and a resonance strength omega-gamma=(2.9+/-0.6)x10E-10 eV was determined. Additionally, the gamma-ray branchings and strength of the 189 keV resonance were studied with a high resolution HPGe detector yielding an omega-gamma value in agreement with the BGO measurement, but 20% larger compared to previous works.

Published
2012

20. Measurement of γ rays from 15N(p,γ)16O cascade and 15N(p,α1γ)12C reactions

Author

IMBRIANI, GIANLUCA, R. deBoer, BEST, ANDREAS, M. Couder, G. Gervino, J. Görres, P. Le Blanc, H. Leiste, A. Lemut, E. Stech, F. Strieder, E. Uberseder, M. Wiescher, Imbriani, Gianluca, R., Deboer, Best, Andrea, M., Couder, G., Gervino, J., Görre, P., Le Blanc, H., Leiste, A., Lemut, E., Stech, F., Strieder, E., Uberseder, and M., Wiescher

Subjects
CNO cycle, Nuclear Astrophysic, Experimental nuclear physic
Abstract

Background The main energy production mechanism for massive stars during hydrogen burning is the CNO cycle. The reactions 15N(p, γ)16O and 15N(p, α0)12C form a branch point in this cycle. The ratio of the corresponding reaction rates determines the CNO abundances evolving during this early stage of the star's life which affects the subsequent nucleosynthesis in later phases of stellar evolution. Determining the cross sections for these reactions at stellar energies is often very difficult. Measurements of other reactions that populate the same compound nucleus can often be used to indirectly determine the cross section of interest. Purpose The nuclear level properties of broad resonances in 16O which characterize the cross section of the reactions 15N(p, γ)16O and 15N(p, α0)12C must be well known in order to accurately extrapolate the measured cross sections to the stellar energy range. The R-matrix formalism is a powerful technique for interpreting these cross sections and is greatly enhanced by additional data in other reaction channels. In a previous publication, measurements were reported for the cross section of the reaction 15N(p, γ)16O for the ground state transition only. Concurrently, γ-ray measurements were recorded for the cascade transitions to the Ex = 6.050, 6.130, and 7.117 MeV bound states of 16O as well as from the reaction 15N(p, α1γ)12C. Excitation curves for the cascade transitions have never been measured and the excitation curve data for the 15N(p, α1γ)12C reaction found in the literature may suffer from substantial errors due to target contamination. Methods Angle integrated cross sections are measured over the proton energy range from Ep = 0.14 to 1.80 MeV for the γ-ray cascade transitions and for the reaction 15N(p, α1γ)12C. Results De-excitations associated with several compound nucleus states in 16O are observed in both the γ-ray and α1 channels. An R-matrix analysis is performed and partial decay widths are deduced for several previously unobserved decay branchings from these states. Conclusion For the first time, excitation curves for the cascade transitions to the 16O bound states at Ex = 6.050, 6.130, and 7.117 MeV are reported over the energy range from Ep = 0.14 to 1.80 MeV. In addition, an improved measurement of the 15N(p, α1γ)12C excitation curve has been made over a similar energy range.

Published
2012

21. Constraining the S-factor of 15N(p,g)16O at Astrophysical Energies

Author

Leblanc, P. J., Imbriani, G., Gorres, G., Junker, M., Azuma, R., Beard, M., Bemmerer, D., Best, A., Broggini, C., Caciolli, A., Corvisiero, P., Costantini, H., Couder, M., Deboer, R., Elekes, Z., Falahat, S., Formicola, A., Fulop, Z. s., Gervino, Gianpiero, Guglielmetti, A., Gustavino, C., Gyurky, G. y., Kappeler, F., Kontos, A., Kuntz, R., Leiste, H., Lemut, A., Li, Q., Limata, B., Marta, M., Mazzocchi, C., Menegazzo, R., O'Brien, S., Palumbo, A., Prati, P., Roca, V., Rolfs, C., Rossi Alvarez, C., Samorjai, E., Stech, E., Straniero, O., Strieder, F., Tan, W., Terrasi, F., Trautvetter, H. P., Uberseder, E., Wiescher, M., Leblanc, P. J., Imbriani, Gianluca, Görres, J, Junker, M., Azuma, R., Beard, M., Bemmerer, D., Best, Andrea, Broggini, C, Caciolli, A, Corvisiero, P., Costantini, H., Couder, M., Deboer, R., 1 Elekes, Z., Falahat, S., Formicola, A., Fülp, Z, Gervino, G., Guglielmetti, A., Gustavino, C., Gyürky, G. y., Käppeler, K., Kontos, A., Kuntz, R., Leiste, H., Lemut, A., Li, Q., Limata, B., Marta, M., Mazzocchi, C., Menegazzo, R., O'Brien, S., Palumbo, A., Prati, P., Roca, Vincenzo, Rolfs, C., Rossi Alvarez, C., Somorjai, E., Stech, E., Straniero, O., Strieder, F., Tan, W., Terrasi, F., Trautvetter, H. P., Uberseder, E., and Wiescher, M.

Subjects
Experimental Nuclear Physic, Astrophysics::High Energy Astrophysical Phenomena, Radiative capture, FOS: Physical sciences, Nuclear Experiment (nucl-ex), Nuclear Astrophysic, Nuclear Experiment, Stellar hydrogen burning
Abstract

The 15N(p,g)16O reaction represents a break out reaction linking the first and second cycle of the CNO cycles redistributing the carbon and nitrogen abundances into the oxygen range. The reaction is dominated by two broad resonances at Ep = 338 keV and 1028 keV and a Direct Capture contribution to the ground state of 16O. Interference effects between these contributions in both the low energy region (Ep < 338 keV) and in between the two resonances (338, Comment: 15 pages, 9 figures

Published
2010

22. An actively vetoed Clover γ-detector for nuclear astrophysicsat LUNA

Author

Luna, Collaboration, Szucs, T., Bemmerer, D., Broggini, C., Caciolli, A., Confortola, F., Corvisiero, P., Elekes, Z., Formicola, A., Fulop, Zs, Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy, Imbriani, G., Junker, M., Lemut, A., Marta, M., Mazzocchi, C., Menegazzo, R., Prati, P., Roca, V., Rolfs, C., Rossi Alvarez, C., Somorjai, E., Oscar Straniero, Strieder, F., Terrasi, F., Trautvetter, H. P., T., Szuc, D., Bemmerer, C., Broggini, A., Caciolli, F., Confortola, P., Corvisiero, Z., Eleke, A., Formicola, F¨ul¨op, Z. s., G., Gervino, A., Guglielmetti, C., Gustavino, Gy¨urky, G. y., Imbriani, Gianluca, M., Junker, A., Lemut, M., Marta, C., Mazzocchi, R., Menegazzo, P., Prati, Roca, Vincenzo, C., Rolf, C., Rossi Alvarez, E., Somorjai, O., Straniero, F., Strieder, F., Terrasi, and H. P., Trautvetter

Subjects
Physics, Nuclear and High Energy Physics, Clover type HP Germaniun detector, Physics::Instrumentation and Detectors, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Underground Laboratories, Semiconductor detector, Nuclear physics, Nuclear astrophysics, High Energy Physics::Experiment, Nuclear Experiment (nucl-ex), Nuclear Experiment, Nuclear Astrophysic
Abstract

An escape-suppressed, composite high-purity germanium detector of the Clover type has been installed at the Laboratory for Underground Nuclear Astrophysics (LUNA) facility, deep underground in the Gran Sasso Laboratory, Italy. The laboratory gamma-ray background of the Clover detector has been studied underground at LUNA and, for comparison, also in an overground laboratory. Spectra have been recorded both for the single segments and for the virtual detector formed by online addition of all four segments. The effect of the escape-suppression shield has been studied as well. Despite their generally higher intrinsic background, escape-suppressed detectors are found to be well suited for underground nuclear astrophysics studies. As an example for the advantage of using a composite detector deep underground, the weak ground state branching of the Ep = 223 keV resonance in the 24Mg(p,gamma)25Al reaction is determined with improved precision., 8 pages, 6 figures, 3 tables; as accepted by Eur. Phys. J. A

Published
2010

23. Stellar and Primordial Nucleosynthesis of 7Be: Measurement of 3He(α,γ)7Be

Author

DI LEVA, ANTONINO, IMBRIANI, GIANLUCA, ROCA, VINCENZO, ROMANO, MARIO, Gialanella L., Kunz R., Rogalla D., Schuermann D., Strieder F., de Cesare M., de Cesare N., D'Onofrio A., Fulop Z., Gyurky G., Mangano G., Ordine A., Rolfs C., Somorjai E., Terrasi F., DI LEVA, Antonino, Gialanella, L., Kunz, R., Rogalla, D., Schuermann, D., Strieder, F., de Cesare, M., de Cesare, N., D'Onofrio, A., Fulop, Z., Gyurky, G., Imbriani, Gianluca, Mangano, G., Ordine, A., Roca, Vincenzo, Rolfs, C., Romano, Mario, Somorjai, E., and Terrasi, F.

Subjects
Nuclear astrophysic, stellar evolution, experimental nuclear physic
Abstract

The 3He(α,γ)7Be reaction presently represents the largest nuclear uncertainty in the predicted solar neutrino flux and has important implications on the big bang nucleosynthesis, i.e., the production of primordial 7Li. We present here the results of an experiment using the recoil separator ERNA (European Recoil separator for Nuclear Astrophysics) to detect directly the 7Be ejectiles. In addition, off-beam activation and coincidence γ-ray measurements were performed at selected energies. At energies above 1 MeV a large discrepancy compared to previous results is observed both in the absolute value and in the energy dependence of the cross section. Based on the available data and models, a robust estimate of the cross section at the astrophysical relevant energies is proposed.

Published
2009

24. The He3(α,γ)Be7 S-factor at solar energies: The prompt γ experiment at LUNA

Author

Costantini H., Bemmerer D., Confortola F., Formicola A., Gyürky G.y., Bezzon P., Bonetti R., Broggini C., Corvisiero P., Elekes Z., Fülöp Z.s., Gervino G., Guglielmetti A., Gustavino C., Junker M., Laubenstein M., Lemut A., Limata B., Lozza V., Marta M., Menegazzo R., Prati P., Rolfs C., Alvarez C. Rossi, Somorjai E., Straniero O., Strieder F., Terrasi F., Trautvetter H. P., IMBRIANI, GIANLUCA, ROCA, VINCENZO, Costantini, H., Bemmerer, D., Confortola, F., Formicola, A., Gyürky, G. y., Bezzon, P., Bonetti, R., Broggini, C., Corvisiero, P., Elekes, Z., Fülöp, Z. s., Gervino, G., Guglielmetti, A., Gustavino, C., Imbriani, Gianluca, Junker, M., Laubenstein, M., Lemut, A., Limata, B., Lozza, V., Marta, M., Menegazzo, R., Prati, P., Roca, Vincenzo, Rolfs, C., Alvarez C., Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., and Trautvetter, H. P.

Subjects
Experimental Nuclear Physic, Nuclear Astrophysic, underground laboratory
Abstract

The He-3(alpha, gamma)Be-7 process is a key reaction in both Big-Bang nucleosynthesis and p-p chain of Hydrogen Burning in Stars. A new measurement of the He-3(alpha, gamma)Be-7 cross section has been performed at the INFN Gran Sasso underground laboratory by both the activation and the prompt gamma detection methods. The present work reports full details of the prompt gamma detection experiment, focusing on the determination of the systematic uncertainty. The final data, including activation measurements at LUNA, are compared with the results of the last generation experiments and two different theoretical models are used to obtain the S-factor at solar energies.

Published
2008

25. Astrophysical S factor of the He3(α,γ)Be7 reaction measured at low energy via detection of prompt and delayed γ rays

Author

F. Confortola, D. Bemmerer, H. Costantini, A. Formicola, G.y. Gyürky, P. Bezzon, R. Bonetti, C. Broggini, P. Corvisiero, Z. Elekes, Z.s. Fülöp, G. Gervino, A. Guglielmetti, C. Gustavino, M. Junker, M. Laubenstein, A. Lemut, B. Limata, V. Lozza, M. Marta, R. Menegazzo, P. Prati, C. Rolfs, C. Alvarez, E. Somorjai, O. Straniero, F. Strieder, F. Terrasi, H. Trautvetter, IMBRIANI, GIANLUCA, ROCA, VINCENZO, F., Confortola, D., Bemmerer, H., Costantini, A., Formicola, Gyürky, G. y., P., Bezzon, R., Bonetti, C., Broggini, P., Corvisiero, Z., Eleke, Fülöp, Z. s., G., Gervino, A., Guglielmetti, C., Gustavino, Imbriani, Gianluca, M., Junker, M., Laubenstein, A., Lemut, B., Limata, V., Lozza, M., Marta, R., Menegazzo, P., Prati, Roca, Vincenzo, C., Rolf, C., Alvarez, E., Somorjai, O., Straniero, F., Strieder, F., Terrasi, and H., Trautvetter

Subjects
solar neutrino, Experimental nuclear physic, nuclear astrophysic
Abstract

Solar neutrino fluxes depend both on astrophysical and on nuclear physics inputs, namely on the cross sections of the reactions responsible for neutrino production inside the Solar core. While the flux of solar 8B neutrinos has been recently measured at Superkamiokande with a 3.5% uncertainty and a precise measurement of 7Be neutrino flux is foreseen in the next future, the predicted fluxes are still affected by larger errors. The largest nuclear physics uncertainty to determine the fluxes of 8B and 7Be neutrinos comes from the 3He(alpha,gamma )7Be reaction. The uncertainty on its S-factor is due to an average discrepancy in results obtained using two different experimental approaches: the detection of the delayed γ rays from 7Be decay and the measurement of the prompt-gamma emission. Here we report on a new high precision experiment performed with both techniques at the same time. Thanks to the low background conditions of the Gran Sasso LUNA accelerator facility, the cross section has been measured at Ec.m. = 170, 106, and 93 keV, the latter being the lowest interaction energy ever reached. The S-factors from the two methods do not show any discrepancy within the experimental errors. An extrapolated S(0) = 0.560 +/- 0.017 keVbarn is obtained. Moreover, branching ratios between the two prompt-gamma transitions have been measure with 5–8% accuracy.

Published
2007

26. Measurement of 25Mg(p; gamma)26Al resonance strengths via gamma spectrometry

Author

A. Formicola, BEST, ANDREAS, M. Junker, D. Bemmerer, R. Bonetti, C. Broggini, A. Caciolli, F. Confortola, P. Corvisiero, H. Costantini, Z. Elekes, Z. Fulop, G. Gervino, A. Guglielmetti, G. Gyürky, C. Gustavino, A. Lemut, M. Marta, C. Mazzocchi, R. Menegazzo, P. Prati, C. Rolfs, C. Rossi Alvarez, E. Somorjai, O. Straniero, F. Strieder, F. Terrasi, H. P. T.r.a.u.t.v.e.t.t.e.r. In: Journal of physics G. : nuclear, particle p.h.y.s.i.c.s. ISSN 0954 3.8.9.9. 3.5.:.1. p. 014013 0.1.4.0.1.3., IMBRIANI, GIANLUCA, LIMATA, BENEDICTA NORMANNA, ROCA, VINCENZO, A., Formicola, Best, Andrea, Imbriani, Gianluca, M., Junker, D., Bemmerer, R., Bonetti, C., Broggini, A., Caciolli, F., Confortola, P., Corvisiero, H., Costantini, Z., Eleke, Z., Fulop, G., Gervino, A., Guglielmetti, G., Gyürky, C., Gustavino, A., Lemut, Limata, BENEDICTA NORMANNA, M., Marta, C., Mazzocchi, R., Menegazzo, P., Prati, Roca, Vincenzo, C., Rolf, C., Rossi Alvarez, E., Somorjai, O., Straniero, F., Strieder, F., Terrasi, nuclear, H. P. T. r. a. u. t. v. e. t. t. e. r. In: Journal of physics G., and Particle, p. h. y. s. i. c. s. ISSN 0954 3. 8. 9. 9. 3. 5. :. 1. p. 014013 0. 1. 4. 0. 1. 3.

Subjects
Physics, Nuclear and High Energy Physics, COSMIC cancer database, Photon, Detector, Resonance, FOS: Physical sciences, Mass spectrometry, Galaxy, Nuclear physics, Underground laboratory, Mg abbundance, Nuclear Experiment (nucl-ex), Hpge detector, Nuclear Experiment, nuclear astrophysic
Abstract

The COMPTEL instrument performed the first mapping of the 1.809 MeV photons in the Galaxy, triggering considerable interest in determing the sources of interstellar 26Al. The predicted 26Al is too low compared to the observation, for a better understanding more accurate rates for the 25Mg(p; gamma)26Al reaction are required. The 25Mg(p;gamma)26Al reaction has been investigated at the resonances at Er= 745; 418; 374; 304 keV at Ruhr-Universitat-Bochum using a Tandem accelerator and a 4piNaI detector. In addition the resonance at Er = 189 keV has been measured deep underground laboratory at Laboratori Nazionali del Gran Sasso, exploiting the strong suppression of cosmic background. This low resonance has been studied with the 400 kV LUNA accelerator and a HPGe detector. The preliminary results of the resonance strengths will be reported., Comment: Accepted for publication in Journal of Physics G

Published
2007
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27. Low energy measurement of the 14N(p,γ)15O total cross section at the LUNA underground facility

Author

Bemmerer, D., Confortola, F., Lemut, A., Bonetti, R., Broggini, C., Corvisiero, P., Costantini, H., Cruz, J., Formicola, A., Fülöp, Z. s., Gervino, Gianpiero, Guglielmetti, A., Gustavino, C., Gyürky, G. y., Imbriani, G., Jesus, A., Junker, M., Limata, B., Menegazzo, R., Prati, P, Roca, V., Rolfs, C., Rogalla, D., Romano, M., Rossi Alvarez, C., Schümann, F., Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., D., Bemmerer, F., Confortola, A., Lemut, R., Bonetti, C., Broggini, P., Corvisiero, H., Costantini, J., Cruz, A., Formicola, Fülöp, Z. s., G., Gervino, A., Guglielmetti, C., Gustavino, Gyürky, G. y., Imbriani, Gianluca, A., Jesu, M., Junker, B., Limata, R., Menegazzo, P., Prati, Roca, Vincenzo, C., Rolf, D., Rogalla, Romano, Mario, C., Rossi Alvarez, F., Schümann, E., Somorjai, O., Straniero, F., Strieder, F., Terrasi, and H. P., Trautvetter

Subjects
Physics, Experimental Nuclear Physic, Nuclear and High Energy Physics, CNO cycle, S-factor, Underground accelerator, 14N(p, γ)15O, Direct measurement, underground laboratory, γ)15O, Nuclear physics, Cross section (physics), Low energy, 14N(p, National laboratory, Nuclear Astrophysic
Abstract

Deep underground in Gran Sasso National Laboratory (Italy), at the LUNA facility, the cross section of the 14N(p, γ)15O, the slowest process of the CNO cycle, has been measured at energies much lower than achieved before. Using a 400 kV accelerator, a windowless gas target and a 4π BGO summing detector, direct cross section data has been obtained down to 70 keV, reaching a value of 0.24 picobarn, corresponding to an S-factor of 1.74±0.14(stat)±0.14(syst) keV barn. The Gamow peak has been covered by direct experimental data for several scenarios of stable and explosive hydrogen burning. The ωγ strength of the 259 keV resonance has been re-measured obtaining 12.8±0.3(stat)±0.4(syst) meV. The stellar reaction rate has been calculated for temperatures 0.09×109−0.3×109 K. A complete description of the experiment is here presented, including the impact of the present data on nucleosynthesis in AGB stars.

Published
2006

28. First direct measurement of the total cross-section of 12C(α,γ)16O

Author

D. Schürmann, A. Di Leva, L. Gialanella, D. Rogalla, F. Strieder, N. De Cesare, A. D'Onofrio, G. Imbriani, R. Kunz, C. Lubritto, A. Ordine, V. Roca, C. Rolfs, M. Romano, F. Schümann, F. Terrasi, H. -P. Trautvetter, D., Schürmann, DI LEVA, Antonino, L., Gialanella, D., Rogalla, F., Strieder, N., De Cesare, A., D'Onofrio, Imbriani, Gianluca, R., Kunz, C., Lubritto, A., Ordine, Roca, Vincenzo, C., Rolf, Romano, Mario, F., Schümann, F., Terrasi, and H. P., Trautvetter

Subjects
Physics, Nuclear and High Energy Physics, Range (particle radiation), Inverse kinematics, Separator (oil production), Alpha (navigation), Stellar helium burnung, Nuclear physics, Cross section (physics), Recoil, Nuclear Experiment, Experimental nuclear physic, Experimental Nuclear Astrophysic, Energy (signal processing)
Abstract

The total cross section of 12C(alpha,gamma)16O was measured for the first time by a direct and ungated detection of the 16O recoils. This measurement in inverse kinematics using the recoil mass separator ERNA in combination with a windowless He gas target allowed to collect data with high precision in the energy range E=1.9 to 4.9 MeV. The data represent new information for the determination of the astrophysical S(E) factor.

Published
2005

29. Feasibility of low energy radiative capture experiments at the LUNA underground accelerator facility

Author

Gianluca Imbriani, Mario R. Romano, Daniel Bemmerer, Matthias Junker, Gy. Gyürky, Roberto Menegazzo, F. Confortola, A. P. Jesus, C. Rossi Alvarez, E. Somorjai, Oscar Straniero, C. Gustavino, C. Rolfs, H. P. Trautvetter, Filippo Terrasi, P. Corvisiero, João Cruz, F. Schümann, A. Guglielmetti, Paolo Prati, A. Lemut, G. Gervino, Detlef Rogalla, A. Formicola, B. Limata, Zs. Fülöp, R. Bonetti, Alberto Vomiero, H. Costantini, C. Broggini, Vincenzo Roca, F. Strieder, D., Bemmerer, F., Confortola, A., Lemut, R., Bonetti, C., Broggini, P., Corvisiero, H., Costantini, J., Cruz, A., Formicola, Flp, Z. S., G., Gervino, A., Guglielmetti, C., Gustavino, Gyrky, G. Y., G., Imbriani, A. P., Jesu, M., Junker, B., Limata, R., Menegazzo, P., Prati, V., Roca, D., Rogalla, C., Rolf, M., Romano, C., ROSSI ALVAREZ, F., Schmann, E., Somorjai, O., Straniero, F., Strieder, Terrasi, Filippo, H. P., Trautvetter, A., Vomiero, Fülöp, Z. s., Gyürky, G. y., Imbriani, Gianluca, Roca, Vincenzo, Romano, Mario, C., Rossi Alvarez, F., Schümann, F., Terrasi, Fulop, Z. S., Gyurky, G. Y., F., Schumann, and AND A., Vomiero

Subjects
Nuclear reaction, Physics, Experimental Nuclear Physic, Nuclear and High Energy Physics, Proton, Gamma ray, chemistry.chemical_element, FOS: Physical sciences, Germanium, Bismuth germanate, underground laboratory, Nuclear physics, symbols.namesake, chemistry.chemical_compound, chemistry, symbols, Nuclear astrophysics, Nuclear Experiment (nucl-ex), Nuclear Astrophysic, Doppler effect, Nuclear Experiment, Beam (structure)
Abstract

The LUNA (Laboratory Underground for Nuclear Astrophysics) facility has been designed to study nuclear reactions of astrophysical interest. It is located deep underground in the Gran Sasso National Laboratory, Italy. Two electrostatic accelerators, with 50 and 400 kV maximum voltage, in combination with solid and gas target setups allowed to measure the total cross sections of the radiative capture reactions $^2$H(p,$\gamma$)3He and $^{14}$N(p,$\gamma$)$^{15}$O within their relevant Gamow peaks. We report on the gamma background in the Gran Sasso laboratory measured by germanium and bismuth germanate detectors, with and without an incident proton beam. A method to localize the sources of beam induced background using the Doppler shift of emitted gamma rays is presented. The feasibility of radiative capture studies at energies of astrophysical interest is discussed for several experimental scenarios., Comment: Submitted to Eur. Phys. J. A

Published
2005

30. Astrophysical S-factor of 14N(p,)15O

Author

Gianluca Imbriani, F. Schümann, H. Costantini, R. Menegazzo, Gy. Gyürky, Vincenzo Roca, Pierre Descouvemont, Daniel Bemmerer, C. Rolfs, A. Guglielmetti, G. Gervino, R. Bonetti, Frank Strieder, Alberto Vomiero, P. Corvisiero, Zs. Fülöp, A. P. Jesus, A. Formicola, C. Broggini, Carmen Angulo, C. Rossi Alvarez, E. Somorjai, Sandra Zavatarelli, C. Gustavino, M. Junker, Mario R. Romano, A. Lemut, H. P. Trautvetter, Oscar Straniero, Filippo Terrasi, João Cruz, Paolo Prati, Formicola, A., Imbriani, G., Costantini, H., Angulo, C., Bemmerer, D., Bonetti, R., Broggini, C., Corvisiero, P., Cruz, J., Descouvemont, P., Fulop, Z., Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, G., Jesus, A., Junker, M., Lemut, A., Menegazzo, R., Prati, P., Roca, V., Rolfs, C., Romano, M., ROSSI ALVAREZ, C., Schumann, F., Somorjai, E., Straniero, O., Strieder, F., Terrasi, Filippo, Trautvetter, H., Vomiero, A., Zavatarelli, S., Imbriani, Gianluca, Jesus, A. P., Roca, Vincenzo, Romano, Mario, Rossi Alvarez, C., Schuemann, F., Terrasi, F., and Trautvetter, H. P.

Subjects
Physics, Nuclear and High Energy Physics, 24.30.-v, Solar spectra, S-factor, Physique, Solar neutrino, Direct reaction, Resonance reaction, CNO cycle, Hydrostatic stellar nucleosynthesis, Experimental physics, Nuclear physics, Cross section (physics), Globular cluster, 26.20.+f, 24.50.+g, nuclear astrophysic, Matrix method, R-matrix
Abstract

We report on a new measurement of the 14N(p,γ) 15O capture cross section at Ep=140 to 400 keV using the 400 kV LUNA accelerator facility at the Laboratori Nazionali del Gran Sasso (LNGS). The uncertainties have been reduced with respect to previous measurements and their analysis. We have analyzed the data using the R-matrix method and we find that the ground state transition accounts for about 15% of the total S-factor. The main contribution to the S-factor is given by the transition to the 6.79 MeV state. We find a total S(0)=1.7±0.2 keVb, in agreement with recent extrapolations. The result has important consequences for the solar neutrino spectrum as well as for the age of globular clusters. © 2004 Elsevier B.V. All rights reserved., info:eu-repo/semantics/published

Published
2004

31. THE LUNA II 400KV ACCELERATOR

Author

A. Formicola, M. Junker, D. Bemmerer, R. Bonetti, G. Broggini, C. Casella, P. Corvsiero, H. Costantini, G. Gervino, C. Gustavino, A. Lemut, P. Prati, C. Rolfs, D. Shurmann, F. Strieder, F. Terrasi, H. P. Trautvetter, S. Zavatarelli, IMBRIANI, GIANLUCA, ROCA, VINCENZO, ROMANO, MARIO, A., Formicola, Imbriani, Gianluca, M., Junker, D., Bemmerer, R., Bonetti, G., Broggini, C., Casella, P., Corvsiero, H., Costantini, G., Gervino, C., Gustavino, A., Lemut, P., Prati, Roca, Vincenzo, C., Rolf, Romano, Mario, D., Shurmann, F., Strieder, F., Terrasi, H. P., Trautvetter, and S., Zavatarelli

Subjects
electrostatic accelerator, calibration, underground laboratory, nuclear astrophysic
Abstract

A second high current accelerator of 400 kV has been installed at the underground laboratory of Gran Sasso, called LUNA II. We describe this new facility as well as measurements of the proton beam characteristics: absolute energy, energy spread, and long-term energy stability. The absolute energy was determined to a precision of 7300 eV at Ep ¼ 130–400 keV using the energy of the capture g-ray transition of 12Cðp; gÞ13N as well as resonance energies at Ep ¼ 309–389 keV of 23Naðp; gÞ24Mg; 26Mgðp; gÞ27Al; and 25Mgðp; gÞ26Al: The resonance studies led to a proton energy spread of better than 100 eV and a long-term energy stability of 5 eV per hour

Published
2003

32. The LUNA II accelerator

Author

C. Gustavino, Gianluca Imbriani, D. Schürmann, A. Formicola, R. Bonetti, G. Gervino, C. Casella, H. Costantini, Sandra Zavatarelli, Vincenzo Roca, Paolo Prati, Filippo Terrasi, F. Strieder, C. Rolfs, P. Corvisiero, Carlo Broggini, Daniel Bemmerer, H. P. Trautvetter, M. Junker, Mario R. Romano, A. Lemut, A., Formicola, Imbriani, Gianluca, M., Junker, D., Bemmerer, R., Bonetti, C., Broggini, C., Casella, P., Corvisiero, H., Costantini, G., Gervino, C., Gustavino, A., Lemut, P., Prati, Roca, Vincenzo, C., Rolf, Romano, Mario, D., Schürmann, F., Strieder, F., Terrasi, H. P., Trautvetter, and S., Zavatarelli

Subjects
Nuclear reaction, Physics, Nuclear and High Energy Physics, Proton, Carbon-12, Resonance, Isotopes of sodium, Nuclear physics, Nuclear astrophysics, Nuclear Reactions, Atomic physics, Experimental nuclear physic, Experimental Nuclear Astrophysic, Instrumentation, Isotopes of magnesium, Beam (structure)
Abstract

A second high current accelerator of 400 kV has been installed at the underground laboratory of Gran Sasso, called LUNA II. We describe this new facility as well as measurements of the proton beam characteristics: absolute energy, energy spread, and long-term energy stability. The absolute energy was determined to a precision of +/-300 eV at E-p = 130-400 keV using the energy of the capture gamma-ray transition of C-12(p,gamma)N-13 as well as resonance energies at E-p = 309-389 keV of Na-23(p, gamma)Mg-24, Mg-26(p, gamma)Al-27, and Mg-25(p, gamma)Al-26. The resonance studies led to a proton energy spread of better than 100 eV and a long-term energy stability of 5 eV per hour.

Published
2003

33. Direct measurement of the absolute cross section of p(7Be,γ)8B

Author

Vincenzo Roca, Antonio D'Onofrio, Frank Strieder, E. Somorjai, Gianluca Imbriani, C. Rolfs, Filippo Terrasi, Carmine Lubritto, Carlo Sabbarese, H. P. Trautvetter, A. Ordine, Mario R. Romano, L. Gialanella, Detlef Rogalla, L. Campajola, Uwe Greife, Gyuri Gyürky, Terrasi, F., Gialanella, L., Imbriani, G., Strieder, F., Campajola, L., D'Onofrio, A., Greife, U., Gyurky, G., Lubritto, C., Ordine, A., Roca, V., Rolfs, C., Romano, M., Rogalla, D., Sabbarese, C., Somorjai, E., Trautvetter, H. P., F., Terrasi, L., Gialanella, Imbriani, Gianluca, F., Strieder, L., Campajola, A., D'Onofrio, U., Greife, G., Gyurky, C., Lubritto, A., Ordine, Roca, Vincenzo, C., Rolf, Romano, Mario, D., Rogalla, C., Sabbarese, E., Somorjai, and H. P., Trautvetter

Subjects
Nuclear physics, Physics, Nuclear and High Energy Physics, Cross section (physics), Solar Hydrogen Burining, Absolute (philosophy), Experimantal nuclear physic, Nuclear Astrophysic
Abstract

A new direct measurement of the absolute cross section of the 1H(7Be,γ)8B reaction has been performed in inverse kinematics at Ecm = 990 keV. A radioactive 7Be beam (Elab, = 8 MeV) and a windowless H2 gas target were used; 8B recoils were identified and counted by a recoil mass separator. The reaction cross section was derived by normalization to the elastic scattering cross section, measured in a separate run. The resulting value σr = 0.40 ± 0.12 μb yielded an astrophysical S-factor at zero energy So = 15.3 ± 4.5 eV b, in fair agreement with recommended values. © 2001 Elsevier Science B.V. All rights reserved.

Published
2001

34. The D(He-3, p)He-4 fusion reaction: electron screening effect and astrophysical S(E) factor at low energies

Author

C. Rolfs, R. Bonetti, F. Strieder, Antonio D'Onofrio, P. G. Prada Moroni, Gianluca Imbriani, F. Schümann, Sandra Zavatarelli, A. Ordine, H. Costantini, M. Junker, G. Gervino, Filippo Terrasi, Mario R. Romano, Detlef Rogalla, H. P. Trautvetter, L. Campajola, Vincenzo Roca, C. Gustavino, Paolo Prati, P. Corvisiero, A. Formicola, Lucio Gialanella, Carlo Broggini, A. Guglielmetti, S., Zavatarelli, P., Corvisiero, H., Costantini, P. G., Prada Moroni, P., Prati, R., Bonetti, A., Guglielmetti, C., Broggini, L., Campajola, A., Formicola, L., Gialanella, Imbriani, Gianluca, A., Ordine, Roca, Vincenzo, Romano, Mario, A., D'Onofrio, F., Terrasi, G., Gervino, C., Gustavino, M., Junker, D., Rogalla, C., Rolf, F., Schumann, F., Strieder, and H. P., Trautvetter

Subjects
Nuclear physics, Physics, Experimental Nuclear Physic, Nuclear and High Energy Physics, Screening effect, Nuclear Astrophysics, Nuclear fusion, Electron, Atomic physics, E factor, Nuclear Astrophysic, underground laboratory
Abstract

The D(He-3,p)He-4 cross section has been measured at E = 4.2 to 13.8 keV using the LUNA accelerator facility installed in the Gran Sasso National Laboratory (LNGS). The experimental setup and the interpretation of results in terms of electron screening potential are described. In the same experiment an estimate of the observed stopping power of the He-3 ions in D-2 target has been obtained and it turned out to be in good agreement with the standard compilation.

Published
2001

35. First measurement of the 3He(3He,2p)4He cross section down to the lower edge of the Solar Gamow peak

Author

Bonetti, R., Broggini, C., Campajola, L., Corvisiero, P., D Alessandro, A., Dessalvi, M., D Onofrio, A., Fubini, A., Gervino, G., Gialanella, L., Greife, U., Guglielmetti, A., Gustavino, C., Imbriani, G., Junker, M., Prati, P., Roca, V., Rolfs, C., Romano, M., Schuemann, F., Strieder, F., Filippo Terrasi, Trautvetter, H. P., Zavatarelli, S., Bonetti, R., Broggini, C., Campajola, L., Corvisiero, P., Dalessandro, A., Dessalvi, M., D'Onofrio, Antonio, Fubini, A., Gervino, G., Gialanella, L., Greife, U., Guglielmetti, A., Gustavino, C., Imbriani, G., Junker, M., Prati, P., Roca, V., Rolfs, C., Romano, M., Schuemann, F., Strieder, F., Terrasi, Filippo, Trautvetter, H. P., Zavatarelli, S., R., Bonetti, C., Broggini, Campajola, Luigi, P., Corvisiero, A., D’Alessandro, M., Dessalvi, A., D'Onofrio, A., Fubini, G., Gervino, L., Gialanella, U., Greife, A., Guglielmetti, C., Gustavino, Imbriani, Gianluca, M., Junker, P., Prati, Roca, Vincenzo, C., Rolf, Romano, Mario, F., Schuemann, F., Strieder, F., Terrasi, H. P., Trautvetter, and S., Zavatarelli

Subjects
Experimental Nuclear Physic, Nuclear Astrophysic, underground laboratory
Abstract

We give the LUNA results on the sigma(E) cross section measurement of a key reaction of the proton-proton chain strongly affecting the calculated neutrino luminosity from the Sun: He-3(He-3, 2p)He-4. Because of the cosmic ray suppression provided by the Gran Sasso underground laboratory, it has been possible to measure sigma(E) throughout the energy range in which this reaction occurs in the Sun, i.e., down to 16.5 keV center of mass energy. The data clearly show the cross section increase due to the electron screening effect but they do not exhibit any evidence for a narrow resonance suggested to explain the B-8 and Be-7 solar neutrino flux reduction.

Published
1999

36. LUNA: a laboratory for underground nuclear astrophysics

Author

F. Strieder, A. Formicola, Gianluca Imbriani, H. Costantini, M. Junker, C. Rolfs, Costantini, H., Formicola, A., Imbriani, Gianluca, Junker, M., Rolfs, C., and Strieder, F.

Subjects
Experimental Nuclear Physic, Physics, Luminosity (scattering theory), FOS: Physical sciences, General Physics and Astronomy, Astronomy, Nucleosynthesis, Nuclear astrophysics, Nuclear fusion, Nuclear Experiment (nucl-ex), Neutrino, Nuclear Astrophysic, Stellar Evolution, Nuclear Experiment, Stellar evolution
Abstract

It is in the nature of astrophysics that many of the processes and objects one tries to understand are physically inaccessible. Thus, it is important that those aspects that can be studied in the laboratory be rather well understood. One such aspect are the nuclear fusion reactions, which are at the heart of nuclear astrophysics. They influence sensitively the nucleosynthesis of the elements in the earliest stages of the universe and in all the objects formed thereafter, and control the associated energy generation, neutrino luminosity, and evolution of stars. We review an experimental approach for the study of nuclear fusion reactions based on an underground accelerator laboratory, named LUNA., Invited Review; accepted for publication in Reports on Progress in Physics; 26 pages; 27 figures

Published
2009
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37. Production of heavy and superheavy neutron-rich nuclei in transfer reactions.

Author

Zagrebaev, V. I. and Greiner, Walter

Subjects
*HEAVY nuclei, *NUCLEAR reactions, *NUCLEOSYNTHESIS, *ASTROPHYSICS, *NUCLEAR physics
Abstract

The problem of production and study of heavy neutron-rich nuclei has been intensively discussed during recent years. Many reasons arouse a great interest in this problem. The present limits of the upper part of the nuclear map are very close to the β stability line while the unexplored area of heavy neutron-rich nuclides (also those located along the neutron closed shell N = 126 to the right-hand side of the stability line) is extremely important for nuclear astrophysic investigations and, in particular, for the understanding of the r process of astrophysical nucleogenesis. For elements with Z > 100 only neutron deficient isotopes (located to the left of the stability line) have been synthesized so far. The "northeast" area of the nuclear map can be reached neither in fusion-fission reactions nor in fragmentation processes widely used nowadays for the production of new nuclei. Multinucleon transfer processes in near barrier collisions of heavy (and very heavy, U-like) ions seem to be the only reaction mechanism allowing us to produce and explore neutron-rich heavy nuclei including those located at the superheavy island of stability. In this paper several transfer reactions for different projectile-target combinations are studied in detail. Besides the predictions for the cross sections of such processes, we also analyze the angular and energy distributions of primary and survived reaction products in the laboratory frame. These results, as well as predicted excitation functions for the yields of neutron-rich superheavy isotopes, might be useful for the design of appropriate experimental equipment and for carrying out experiments of such kind. [ABSTRACT FROM AUTHOR]

Published
2011
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38. Preliminary studies for three experiments at Treiman-Yang criterion.

Author

KRES, I. V., KONDRATYEV, V. N., CHERUBINI, S., and SPITALERI, C.

Subjects
NUCLEAR reactions, FEYNMAN diagrams, QUASI-free reactions, COLLISIONS (Nuclear physics), NUCLEAR energy
Abstract

Nuclear reactions with three bodies in their final state may proceed through different reaction mechanisms. The Feynman graph technique has been widely used to describe such reactions. However, it is very difficult in general to select the graphs that dominate in given process. The Treiman-Yang criterion is one of the most powerful experimental tests for verifying the pole approximation prediction when describing a quasi-free reaction mechanism. We propose the theoretical study of the H²(B10, α Be7)ns, H¹(B11,α1 α2)αs, He³(Be9, α1α2)αs reactions at different energies. The preliminary study helps to check the existence of a QF channel by using the TY creterion. [ABSTRACT FROM AUTHOR]

Published
2016
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42. Science with radioactive beams: the alchemist's dream.

Author

Gelletly, W.

Subjects
RADIOACTIVE nuclear beams, NUCLEAR physics
Abstract

Nuclear science is being transformed by a new capacity to create beams of radioactive nuclei. Until now all of our knowledge of nuclear physics and the applications which flow from it has been derived from studies of radioactive decay and nuclear reactions induced by beams of the 283 stable or long-lived nuclear species we can find on Earth. Here we describe first how beams of radioactive nuclei can be created. The present status of nuclear physics is then reviewed before potential applications to nuclear physics, nuclear astrophysics, materials science, bio-medical, and environmental studies are described. [ABSTRACT FROM AUTHOR]

Published
2001
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43. What We Would Like Lhc To Give Us - Proceedings Of The International School Of Subnuclear Physics

Author

Antonino Zichichi and Antonino Zichichi

Subjects
Colliders (Nuclear physics)--Congresses, Nuclear physics--Congresses, Particles (Nuclear physics)--Congresses
Abstract

This book is the proceedings of the International School of Subnuclear Physics, ISSP 2012, 50th Course — ERICE, 23 June 2013 - 2 July 2012. This course was devoted to the celebrations of the 50th Anniversary of the Subnuclear Physics School which was started in 1961 by Antonino Zichichi with John Bell at CERN and formally established in 1962 by Bell, Blackett, Weisskopf, Rabi and Zichichi in Geneva (CERN). The lectures covered the latest and most significant achievements in theoretical and in experimental subnuclear physics.

Published
2014

44. Progress in Cosmology : Proceedings of the Oxford International Symposium Held in Christ Church, Oxford, September 14-18, 1981

Author

A.W. Wolfendale and A.W. Wolfendale

Subjects
Cosmology--Congresses, Nuclear astrophysics--Congresses
Abstract

When my colleague Dr. Paul Kent asked me which branch of Physics was most lively and which would lend itself best to a small high quality Symposium, I had no hesitation in answering'Cosmology'. It seemed very timely that a meeting should take place which would bring together scientists interested in all branches of Astronomy, including Cosmic Rays, and Elementary Particles too and endeavour to put at least some of the pieces of the jigsaw together. The vast majority of the papers presented were later produced ~n appropriate camera-ready form and are published in this volume. I am very grateful to the authors for their ready cooperation. Grateful thanks are also extended to the Board of Management of the Foster-Wills and Theodor Heuss Scholarships, Oxford University and the Deutscher Akademischer Austauschdienst (German Academic Exchange Service) who funded the Symposium. The Director of the German Academic Exchange Service, Frau M.E. Schmitz and her colleague Mrs. Susan Putt, organized the whole meeting in a most exemplary fashion. Finally, on behalf of all participants and guests, s~ncere thanks are offered to Paul Kent as Convenor for initiating the Symposium, arranging the social events and organizing accommodation in such magnificent surroundings. Christ Church was the horne of Lewis Carrol and we were ever mindful - and appropriately so - of Alice. A. W. Wolfendale Durham, February 10th, 1982 vii A. W. Wolfendale (ed.), Progress in Cosmology, vii.

Published
2012

45. Heavy Ion Collisions - Proceedings Of The Third In2p3-riken Symposium

Author

Tohru Motobayashi, Masayasu Ishihara, N Frascaria, Tohru Motobayashi, Masayasu Ishihara, and N Frascaria

Subjects
Heavy ion collisions--Congresses, Exotic nuclei--Congresses
Abstract

This book covers recent topics on studies of heavy ion collisions in the energy domain from several MeV/nucleon to several GeV/nucleon: exotic nuclei and radiactive beams; hot nuclei; hot and cold giant resonances; high spin and some applications; and panel for future collaboration.

Published
1995

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