C. Gustavino - LUNA collab.

C. Gustavino
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C. Gustavino
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LUNA collab.
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Nuclear Experiment (28)
 
High Energy Physics - Experiment (15)
 
Solar and Stellar Astrophysics (11)
 
Physics - Instrumentation and Detectors (8)
 
Astrophysics (7)
 
High Energy Physics - Phenomenology (3)
 
Cosmology and Nongalactic Astrophysics (2)
 
High Energy Astrophysical Phenomena (2)
 
Astrophysics of Galaxies (1)
 
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Instrumentation and Methods for Astrophysics (1)

Publications Authored By C. Gustavino

The Extreme Energy Events Project is a synchronous sparse array of 52 tracking detectors for studying High Energy Cosmic Rays (HECR) and Cosmic Rays-related phenomena. The observatory is also meant to address Long Distance Correlation (LDC) phenomena: the network is deployed over a broad area covering 10 degrees in latitude and 11 in longitude. An overview of a set of preliminary results is given, extending from the study of local muon flux dependance on solar activity to the investigation of the upward-going component of muon flux traversing the EEE stations; from the search for anisotropies at the sub-TeV scale to the hints for observations of km-scale Extensive Air Shower (EAS). Read More

Stardust grains recovered from meteorites provide high-precision snapshots of the isotopic composition of the stellar environment in which they formed. Attributing their origin to specific types of stars, however, often proves difficult. Intermediate-mass stars of 4-8 solar masses are expected to contribute a large fraction of meteoritic stardust. Read More

2016Nov
Affiliations: 1University of Padova, Italy, 2University of Padova, Italy, 3University of Padova, Italy, 4SUPA, University of Edinburgh, United Kingdom, 5Helmholtz-Zentrum Dresden-Rossendorf, Germany, 6University of Napoli "Federico II" and INFN, Italy, 7Gran Sasso Science Institute, L'Aquila, Italy, 8SISSA, Trieste, Italy, 9INFN of Padova, Italy, 10SUPA, University of Edinburgh, United Kingdom, 11University of Padova, Italy, 12University of Genova and INFN, Italy, 13Gran Sasso Science Institute, L'Aquila, Italy, 14University of Genova and INFN, Italy, 15SUPA, University of Edinburgh, United Kingdom, 16University of Padova, Italy, 17University of Napoli "Federico II" and INFN, Italy, 18Institute for Nuclear Research, 19University of Genova and INFN, Italy, 20INFN and LNGS, Italy, 21u, 22o, 23Institute for Nuclear Research, 24University ofTorino and INFN, Italy, 25University of Milano and INFN, Italy, 26INFN, Sezione di Roma La Sapienza, Italy, 27u, 28Institute for Nuclear Research, 29University of Napoli "Federico II" and INFN, Italy, 30INFN and LNGS, Italy, 31INFN of Padova, Italy, 32University of Bari and INFN, Italy, 33University of Bari and INFN, Italy, 34University of Genova and INFN, Italy, 35INAF, Osservatorio Astronomico di Teramo, Italy, 36u, 37Institute for Nuclear Research, 38a, 39Institute for Nuclear Research, 40University ofTorino and INFN, Italy

We investigate the impact of the new LUNA rate for the nuclear reaction $^{22}$Ne$(p,\gamma)^{23}$Na on the chemical ejecta of intermediate-mass stars, with particular focus on the thermally-pulsing asymptotic giant branch (TP-AGB) stars that experience hot-bottom burning. To this aim we use the PARSEC and COLIBRI codes to compute the complete evolution, from the pre-main sequence up to the termination of the TP-AGB phase, of a set of stellar models with initial masses in the range $3.0\,M_{\odot} - 6. Read More

The $^{22}$Ne(p,$\gamma$)$^{23}$Na reaction is the most uncertain process in the neon-sodium cycle of hydrogen burning. At temperatures relevant for nucleosynthesis in asymptotic giant branch stars and classical novae, its uncertainty is mainly due to a large number of predicted but hitherto unobserved resonances at low energy. Purpose: A new direct study of low energy $^{22}$Ne(p,$\gamma$)$^{23}$Na resonances has been performed at the Laboratory for Underground Nuclear Astrophysics (LUNA), in the Gran Sasso National Laboratory, Italy. Read More

2016Oct
Affiliations: 1LUNA Collaboration, 2LUNA Collaboration, 3LUNA Collaboration, 4LUNA Collaboration, 5LUNA Collaboration, 6LUNA Collaboration, 7LUNA Collaboration, 8LUNA Collaboration, 9LUNA Collaboration, 10LUNA Collaboration, 11LUNA Collaboration, 12LUNA Collaboration, 13LUNA Collaboration, 14LUNA Collaboration, 15LUNA Collaboration, 16LUNA Collaboration, 17LUNA Collaboration, 18LUNA Collaboration, 19LUNA Collaboration, 20LUNA Collaboration, 21LUNA Collaboration, 22LUNA Collaboration, 23LUNA Collaboration, 24LUNA Collaboration, 25LUNA Collaboration, 26LUNA Collaboration, 27LUNA Collaboration, 28LUNA Collaboration, 29LUNA Collaboration, 30LUNA Collaboration, 31LUNA Collaboration, 32LUNA Collaboration, 33LUNA Collaboration, 34LUNA Collaboration, 35LUNA Collaboration

The $^{17}$O(p,$\alpha$)$^{14}$N reaction plays a key role in various astrophysical scenarios, from asymptotic giant branch stars to classical novae. It affects the synthesis of rare isotopes such as $^{17}$O and $^{18}$F, which can provide constraints on astrophysical models. A new direct determination of the $E_{\rm R}~=~64. Read More

The $^{22}$Ne(p,$\gamma$)$^{23}$Na reaction takes part in the neon-sodium cycle of hydrogen burning. This cycle affects the synthesis of the elements between $^{20}$Ne and $^{27}$Al in asymptotic giant branch stars and novae. The $^{22}$Ne(p,$\gamma$)$^{23}$Na reaction rate is very uncertain because of a large number of unobserved resonances lying in the Gamow window. Read More

2015Jul
Authors: OPERA Collaboration, N. Agafonova, A. Aleksandrov, A. Anokhina, S. Aoki, A. Ariga, T. Ariga, D. Bender, A. Bertolin, I. Bodnarchuk, C. Bozza, R. Brugnera, A. Buonaura, S. Buontempo, B. Büttner, M. Chernyavsky, A. Chukanov, L. Consiglio, N. D'Ambrosio, G. De Lellis, M. De Serio, P. Del Amo Sanchez, A. Di Crescenzo, D. Di Ferdinando, N. Di Marco, S. Dmitrievski, M. Dracos, D. Duchesneau, S. Dusini, T. Dzhatdoev, J. Ebert, A. Ereditato, R. A. Fini, F. Fornari, T. Fukuda, G. Galati, A. Garfagnini, J. Goldberg, Y. Gornushkin, G. Grella, A. M. Guler, C. Gustavino, C. Hagner, T. Hara, H. Hayakawa, A. Hollnagel, B. Hosseini, K. Ishiguro, K. Jakovcic, C. Jollet, C. Kamiscioglu, M. Kamiscioglu, J. H. Kim, S. H. Kim, N. Kitagawa, B. Klicek, K. Kodama, M. Komatsu, U. Kose, I. Kreslo, F. Laudisio, A. Lauria, A. Ljubicic, A. Longhin, P. F. Loverre, A. Malgin, M. Malenica, G. Mandrioli, T. Matsuo, T. Matsushita, V. Matveev, N. Mauri, E. Medinaceli, A. Meregaglia, S. Mikado, M. Miyanishi, F. Mizutani, P. Monacelli, M. C. Montesi, K. Morishima, M. T. Muciaccia, N. Naganawa, T. Naka, M. Nakamura, T. Nakano, Y. Nakatsuka, K. Niwa, S. Ogawa, A. Olchevsky, T. Omura, K. Ozaki, A. Paoloni, L. Paparella, B. D. Park, I. G. Park, L. Pasqualini, A. Pastore, L. Patrizii, H. Pessard, C. Pistillo, D. Podgrudkov, N. Polukhina, M. Pozzato, F. Pupilli, M. Roda, T. Roganova, H. Rokujo, G. Rosa, O. Ryazhskaya, O. Sato, A. Schembri, W. Schmidt-Parzefall, I. Shakirianova, T. Shchedrina, A. Sheshukov, H. Shibuya, T. Shiraishi, G. Shoziyoev, S. Simone, M. Sioli, C. Sirignano, G. Sirri, A. Sotnikov, M. Spinetti, L. Stanco, N. Starkov, S. M. Stellacci, M. Stipcevic, P. Strolin, S. Takahashi, M. Tenti, F. Terranova, V. Tioukov, S. Tufanli, P. Vilain, M. Vladymyrov, L. Votano, J. L. Vuilleumier, G. Wilquet, B. Wonsak, C. S. Yoon, S. Zemskova

The OPERA experiment was designed to search for $\nu_{\mu} \rightarrow \nu_{\tau}$ oscillations in appearance mode, i.e. by detecting the $\tau$-leptons produced in charged current $\nu_{\tau}$ interactions. Read More

2015Mar
Authors: OPERA Collaboration, N. Agafonova, A. Aleksandrov, A. Anokhina, S. Aoki, A. Ariga, T. Ariga, D. Bender, A. Bertolin, I. Bodnarchuk, C. Bozza, R. Brugnera, A. Buonaura, S. Buontempo, B. Büttner, M. Chernyavsky, A. Chukanov, L. Consiglio, N. D'Ambrosio, G. De Lellis, M. De Serio, P. Del Amo Sanchez, A. Di Crescenzo, D. Di Ferdinando, N. Di Marco, S. Dmitrievski, M. Dracos, D. Duchesneau, S. Dusini, T. Dzhatdoev, J. Ebert, A. Ereditato, R. A. Fini, T. Fukuda, G. Galati, A. Garfagnini, J. Goldberg, Y. Gornushkin, G. Grella, A. M. Guler, C. Gustavino, C. Hagner, T. Hara, A. Hollnagel, B. Hosseini, K. Ishiguro, K. Jakovcic, C. Jollet, C. Kamiscioglu, M. Kamiscioglu, J. H. Kim, S. H. Kim, N. Kitagawa, B. Klicek, K. Kodama, M. Komatsu, U. Kose, I. Kreslo, A. Lauria, A. Ljubicic, A. Longhin, A. Malgin, M. Malenica, G. Mandrioli, T. Matsuo, V. Matveev, N. Mauri, E. Medinaceli, A. Meregaglia, S. Mikado, P. Monacelli, M. C. Montesi, K. Morishima, M. T. Muciaccia, N. Naganawa, T. Naka, M. Nakamura, T. Nakano, Y. Nakatsuka, K. Niwa, S. Ogawa, T. Omura, K. Ozaki, A. Paoloni, L. Paparella, B. D. Park, I. G. Park, L. Pasqualini, A. Pastore, L. Patrizii, H. Pessard, D. Podgrudkov, N. Polukhina, M. Pozzato, F. Pupilli, M. Roda, T. Roganova, H. Rokujo, G. Rosa, O. Ryazhskaya, O. Sato, A. Schembri, I. Shakirianova, T. Shchedrina, A. Sheshukov, H. Shibuya, T. Shiraishi, G. Shoziyoev, S. Simone, M. Sioli, C. Sirignano, G. Sirri, M. Spinetti, L. Stanco, N. Starkov, S. M. Stellacci, M. Stipcevic, P. Strolin, S. Takahashi, M. Tenti, F. Terranova, V. Tioukov, S. Tufanli, P. Vilain, M. Vladymyrov, L. Votano, J. L. Vuilleumier, G. Wilquet, B. Wonsak, C. S. Yoon, S. Zemskova

The OPERA experiment, exposed to the CERN to Gran Sasso $\nu_\mu$ beam, collected data from 2008 to 2012. Four oscillated $\nu_\tau$ Charged Current interaction candidates have been detected in appearance mode, which are consistent with $\nu_\mu \to \nu_\tau$ oscillations at the atmospheric $\Delta m^2$ within the "standard" three-neutrino framework. In this paper, the OPERA $\nu_\tau$ appearance results are used to derive limits on the mixing parameters of a massive sterile neutrino. Read More

2014Nov
Affiliations: 1LUNA collab., 2LUNA collab., 3LUNA collab., 4LUNA collab., 5LUNA collab., 6LUNA collab., 7LUNA collab., 8LUNA collab., 9LUNA collab., 10LUNA collab., 11LUNA collab., 12LUNA collab., 13LUNA collab., 14LUNA collab., 15LUNA collab., 16LUNA collab., 17LUNA collab., 18LUNA collab., 19LUNA collab., 20LUNA collab., 21LUNA collab., 22LUNA collab., 23LUNA collab., 24LUNA collab., 25LUNA collab., 26LUNA collab., 27LUNA collab., 28LUNA collab., 29LUNA collab., 30LUNA collab., 31LUNA collab.

The $^{22}$Ne(p,$\gamma$)$^{23}$Na reaction takes part in the neon-sodium cycle of hydrogen burning. This cycle is active in asymptotic giant branch stars as well as in novae and contributes to the nucleosythesis of neon and sodium isotopes. In order to reduce the uncertainties in the predicted nucleosynthesis yields, new experimental efforts to measure the $^{22}$Ne(p,$\gamma$)$^{23}$Na cross section directly at the astrophysically relevant energies are needed. Read More

2014Jul
Authors: OPERA Collaboration, N. Agafonova, A. Aleksandrov, A. Anokhina, S. Aoki, A. Ariga, T. Ariga, T. Asada, D. Bender, A. Bertolin, C. Bozza, R. Brugnera, A. Buonaura, S. Buontempo, B. Buttne, M. Chernyavsky, A. Chukanov, L. Consiglio, N. D'Ambrosio, G. De Lellis, M. De Serio, P. Del Amo Sanchez, A. Di Crescenzo, D. Di Ferdinando, N. Di Marco, S. Dmitrievski, M. Dracos, D. Duchesneau, S. Dusini, T. Dzhatdoev, J. Ebert, A. Ereditato, R. A. Fini, T. Fukuda, G. Galati, A. Garfagnini, G. Giacomelli, C. Goellnitz, J. Goldberg, Y. Gornushkin, G. Grella, M. Guler, C. Gustavino, C. Hagner, T. Hara, T. Hayakawa, A. Hollnagel, B. Hosseini, H. Ishida, K. Ishiguro, K. Jakovcic, C. Jollet, C. Kamiscioglu, M. Kamiscioglu, T. Katsuragawa, J. Kawada, H. Kawahara, J. H. Kim, S. H. Kim, N. Kitagawa, B. Klicek, K. Kodama, M. Komatsu, U. Kose, I. Kreslo, A. Lauria, J. Lenkeit, A. Ljubicic, A. Longhin, P. Loverre, M. Malenica, A. Malgin, G. Mandrioli, T. Matsuo, V. Matveev, N. Mauri, E. Medinaceli, A. Meregaglia, M. Meyer, S. Mikado, M. Miyanishi, P. Monacelli, M. C. Montesi, K. Morishima, M. T. Muciaccia, N. Naganawa, T. Naka, M. Nakamura, T. Nakano, Y. Nakatsuka, K. Niwa, S. Ogawa, N. Okateva, A. Olshevsky, T. Omura, K. Ozaki, A. Paoloni, B. D. Park, I. G. Park, L. Pasqualini, A. Pastore, L. Patrizii, H. Pessard, C. Pistillo, D. Podgrudkov, N. Polukhina, M. Pozzato, F. Pupilli, M. Roda, T. Roganova, H. Rokujo, G. Rosa, O. Ryazhskaya, O. Sato, A. Schembri, I. Shakiryanova, T. Shchedrina, A. Sheshukov, H. Shibuya, T. Shiraishi, G. Shoziyoev, S. Simone, M. Sioli, C. Sirignano, G. Sirri, M. Spinetti, L. Stanco, N. Starkov, S. M. Stellacci, M. Stipcevic, P. Strolin, S. Takahashi, M. Tenti, F. Terranova, V. Tioukov, S. Tufanli, A. Umemoto, P. Vilain, M. Vladimirov, L. Votano, J. L. Vuilleumier, G. Wilquet, B. Wonsak, C. S. Yoon, I. Yaguchi, M. Yoshimoto, S. Zemskova, A. Zghiche

The OPERA experiment is searching for nu_mu -> nu_tau oscillations in appearance mode i.e. via the direct detection of tau leptons in nu_tau charged current interactions. Read More

Big Bang Nucleosynthesis (BBN) relates key cosmological parameters to the primordial abundance of light elements. In this paper, we point out that the recent observations of Cosmic Microwave Background anisotropies by the Planck satellite and by the BICEP2 experiment constrain these parameters with such a high level of accuracy that the primordial deuterium abundance can be inferred with remarkable precision. For a given cosmological model, one can obtain independent information on nuclear processes in the energy range relevant for BBN, which determine the eventual ^2H/H yield. Read More

2014Apr
Authors: OPERA Collaboration, N. Agafonova, A. Aleksandrov, A. Anokhina, S. Aoki, A. Ariga, T. Ariga, D. Bender, A. Bertolin, C. Bozza, R. Brugnera, A. Buonaura, S. Buontempo, B. Büttner, M. Chernyavsky, A. Chukanov, L. Consiglio, N. D'Ambrosio, G. De Lellis, M. De Serio, P. Del Amo Sanchez, A. Di Crescenzo, D. Di Ferdinando, N. Di Marco, S. Dmitrievski, M. Dracos, D. Duchesneau, S. Dusini, T. Dzhatdoev, J. Ebert, A. Ereditato, R. A. Fini, T. Fukuda, G. Galati, A. Garfagnini, G. Giacomelli, C. Goellnitz, J. Goldberg, D. Goloubkov, Y. Gornushkin, G. Grella, M. Guler, C. Gustavino, C. Hagner, T. Hara, A. Hollnagel, B. Hosseini, H. Ishida, K. Ishiguro, K. Jakovcic, C. Jollet, C. Kamiscioglu, M. Kamiscioglu, J. Kawada, J. H. Kim, S. H. Kim, N. Kitagawa, B. Klicek, K. Kodama, M. Komatsu, U. Kose, I. Kreslo, A. Lauria, J. Lenkeit, A. Ljubicic, A. Longhin, P. Loverre, A. Malgin, M. Malenica, G. Mandrioli, T. Matsuo, V. Matveev, N. Mauri, E. Medinaceli, A. Meregaglia, M. Meyer, S. Mikado, P. Monacelli, M. C. Montesi, K. Morishima, M. T. Muciaccia, N. Naganawa, T. Naka, M. Nakamura, T. Nakano, Y. Nakatsuka, K. Niwa, S. Ogawa, N. Okateva, A. Olshevsky, T. Omura, K. Ozaki, A. Paoloni, B. D. Park, I. G. Park, L. Pasqualini, A. Pastore, L. Patrizii, H. Pessard, C. Pistillo, D. Podgrudkov, N. Polukhina, M. Pozzato, F. Pupilli, M. Roda, H. Rokujo, T. Roganova, G. Rosa, I. Rostovtseva, O. Ryazhskaya, O. Sato, Y. Sato, A. Schembri, I. Shakiryanova, T. Shchedrina, A. Sheshukov, H. Shibuya, T. Shiraishi, G. Shoziyoev, S. Simone, M. Sioli, C. Sirignano, G. Sirri, M. Spinetti, L. Stanco, N. Starkov, S. M. Stellacci, M. Stipcevic, P. Strolin, S. Takahashi, M. Tenti, F. Terranova, V. Tioukov, S. Tufanli, P. Vilain, M. Vladimirov, L. Votano, J. L. Vuilleumier, G. Wilquet, B. Wonsak, C. S. Yoon, Y. Zaitsev, S. Zemskova, A. Zghiche

The OPERA long-baseline neutrino-oscillation experiment has observed the direct appearance of $\nu_\tau$ in the CNGS $\nu_\mu$ beam. Two large muon magnetic spectrometers are used to identify muons produced in the $\tau$ leptonic decay and in $\nu_\mu^{CC}$ interactions by measuring their charge and momentum. Besides the kinematic analysis of the $\tau$ decays, background resulting from the decay of charmed particles produced in $\nu_\mu^{CC}$ interactions is reduced by efficiently identifying the muon track. Read More

2014Apr
Authors: N. Agafonova, A. Anokhina, S. Aoki, A. Ariga, T. Ariga, D. Bender, A. Bertolin, C. Bozza, R. Brugnera, A. Buonaura, S. Buontempo, B. Buttner, M. Chernyavsky, A. Chukanov, L. Consiglio, N. D'Ambrosio, G. De Lellis, M. De Serio, P. Del Amo Sanchez, A. Di Crescenzo, D. Di Ferdinando, N. Di Marco, S. Dmitrievski, M. Dracos, D. Duchesneau, S. Dusini, T. Dzhatdoev, J. Ebert, A. Ereditato, R. A. Fini, T. Fukuda, G. Galati, A. Garfagnini, G. Giacomelli, C. Gollnitz, J. Goldberg, Y. Gornushkin, G. Grella, M. Guler, C. Gustavino, C. Hagner, T. Hara, A. Hollnagel, B. Hosseini, H. Ishida, K. Ishiguro, K. Jakovcic, C. Jollet, C. Kamiscioglu, M. Kamiscioglu, J. Kawada, J. H. Kim, S. H. Kim, N. Kitagawa, B. Klicek, K. Kodama, M. Komatsu, U. Kose, I. Kreslo, A. Lauria, J. Lenkeit, A. Ljubicic, A. Longhin, P. Loverre, A. Malgin, M. Malenica, G. Mandrioli, T. Matsuo, V. Matveev, N. Mauri, E. Medinaceli, A. Meregaglia, S. Mikado, P. Monacelli, M. C. Montesi, K. Morishima, M. T. Muciaccia, N. Naganawa, T. Naka, M. Nakamura, T. Nakano, Y. Nakatsuka, K. Niwa, S. Ogawa, N. Okateva, A. Olshevsky, T. Omura, K. Ozaki, A. Paoloni, B. D. Park, I. G. Park, L. Pasqualini, A. Pastore, L. Patrizii, H. Pessard, C. Pistillo, D. Podgrudkov, N. Polukhina, M. Pozzato, F. Pupilli, M. Roda, H. Rokujo, T. Roganova, G. Rosa, O. Ryazhskaya, O. Sato, A. Schembri, I. Shakiryanova, T. Shchedrina, A. Sheshukov, H. Shibuya, T. Shiraishi, G. Shoziyoev, S. Simone, M. Sioli, C. Sirignano, G. Sirri, M. Spinetti, L. Stanco, N. Starkov, S. M. Stellacci, M. Stipcevic, T. Strauss, P. Strolin, S. Takahashi, M. Tenti, F. Terranova, V. Tioukov, S. Tufanli, P. Vilain, M. Vladimirov, L. Votano, J. L. Vuilleumier, G. Wilquet, B. Wonsak, C. S. Yoon, S. Zemskova, A. Zghiche

The OPERA experiment, designed to perform the first observation of $\nu_\mu \rightarrow \nu_\tau$ oscillations in appearance mode through the detection of the $\tau$ leptons produced in $\nu_\tau$ charged current interactions, has collected data from 2008 to 2012. In the present paper, the procedure developed to detect $\tau$ particle decays, occurring over distances of the order of 1 mm from the neutrino interaction point, is described in detail. The results of its application to the search for charmed hadrons are then presented as a validation of the methods for $\nu_\tau$ appearance detection. Read More

2014Mar
Authors: N. Agafonova, A. Anokhina, S. Aoki, A. Ariga, T. Ariga, D. Bender, A. Bertolin, C. Bozza, R. Brugnera, A. Buonaura, S. Buontempo, B. Buettner, M. Chernyavsky, A. Chukanov, L. Consiglio, N. D'Ambrosio, G. De Lellis, M. De Serio, P. Del Amo Sanchez, A. Di Crescenzo, D. Di Ferdinando, N. Di Marco, S. Dmitrievski, M. Dracos, D. Duchesneau, S. Dusini, T. Dzhatdoev, J. Ebert, A. Ereditato, R. A. Fini, T. Fukuda, G. Galati, A. Garfagnini, G. Giacomelli, C. Goellnitz, J. Goldberg, Y. Gornushkin, G. Grella, M. Guler, C. Gustavino, C. Hagner, T. Hara, A. Hollnagel, B. Hosseini, H. Ishida, K. Ishiguro, K. Jakovcic, C. Jollet, C. Kamiscioglu, M. Kamiscioglu, J. Kawada, J. H. Kim, S. H. Kim, N. Kitagawa, B. Klicek, K. Kodama, M. Komatsu, U. Kose, I. Kreslo, A. Lauria, J. Lenkeit, A. Ljubicic, A. Longhin, P. Loverre, A. Malgin, M. Malenica, G. Mandrioli, T. Matsuo, V. Matveev, N. Mauri, E. Medinaceli, A. Meregaglia, S. Mikado, P. Monacelli, M. C. Montesi, K. Morishima, M. T. Muciaccia, N. Naganawa, T. Naka, M. Nakamura, T. Nakano, Y. Nakatsuka, K. Niwa, S. Ogawa, N. Okateva, A. Olshevsky, T. Omura, K. Ozaki, A. Paoloni, B. D. Park, I. G. Park, L. Pasqualini, A. Pastore, L. Patrizii, H. Pessard, C. Pistillo, D. Podgrudkov, N. Polukhina, M. Pozzato, F. Pupilli, M. Roda, H. Rokujo, T. Roganova, G. Rosa, O. Ryazhskaya, O. Sato, A. Schembri, I. Shakiryanova, T. Shchedrina, A. Sheshukov, H. Shibuya, T. Shiraishi, G. Shoziyoev, S. Simone, M. Sioli, C. Sirignano, G. Sirri, M. Spinetti, L. Stanco, N. Starkov, S. M. Stellacci, M. Stipcevic, P. Strolin, S. Takahashi, M. Tenti, F. Terranova, V. Tioukov, S. Tufanli, P. Vilain, M. Vladimirov, L. Votano, J. L. Vuilleumier, G. Wilquet, B. Wonsak, C. S. Yoon, S. Zemskova, A. Zghiche

The OPERA detector, designed to search for $\nu_{\mu} \to \nu_{\tau}$ oscillations in the CNGS beam, is located in the underground Gran Sasso laboratory, a privileged location to study TeV-scale cosmic rays. For the analysis here presented, the detector was used to measure the atmospheric muon charge ratio in the TeV region. OPERA collected charge-separated cosmic ray data between 2008 and 2012. Read More

2014Jan
Authors: N. Agafonova, A. Aleksandrov, A. Anokhina, S. Aoki, A. Ariga, T. Ariga, T. Asada, D. Autiero, A. Ben Dhahbi, A. Badertscher, D. Bender, A. Bertolin, C. Bozza, R. Brugnera, F. Brunet, G. Brunetti, A. Buonaura, S. Buontempo, B. Buettner, L. Chaussard, M. Chernyavsky, V. Chiarella, A. Chukanov, L. Consiglio, N. D'Ambrosio, G. De Lellis, M. De Serio, P. Del Amo Sanchez, A. Di Crescenzo, D. Di Ferdinando, N. Di Marco, S. Dmitrievski, M. Dracos, D. Duchesneau, S. Dusini, T. Dzhatdoev, J. Ebert, A. Ereditato, J. Favier, T. Ferber, G. Ferone, R. A. Fini, T. Fukuda, G. Galati, A. Garfagnini, G. Giacomelli, C. Goellnitz, J. Goldberg, Y. Gornushkin, G. Grella, F. Grianti, M. Guler, C. Gustavino, C. Hagner, K. Hakamata, T. Hara, T. Hayakawa, M. Hierholzer, A. Hollnagel, B. Hosseini, H. Ishida, K. Ishiguro, M. Ishikawa, K. Jakovcic, C. Jollet, C. Kamiscioglu, M. Kamiscioglu, T. Katsuragawa, J. Kawada, H. Kawahara, J. H. Kim, S. H. Kim, M. Kimura, N. Kitagawa, B. Klicek, K. Kodama, M. Komatsu, U. Kose, I. Kreslo, A. Lauria, J. Lenkeit, A. Ljubicic, A. Longhin, P. Loverre, A. Malgin, G. Mandrioli, J. Marteau, T. Matsuo, V. Matveev, N. Mauri, E. Medinaceli, A. Meregaglia, P. Migliozzi, S. Mikado, M. Miyanishi, E. Miyashita, P. Monacelli, M. C. Montesi, K. Morishima, M. T. Muciaccia, N. Naganawa, T. Naka, M. Nakamura, T. Nakano, Y. Nakatsuka, K. Niwa, S. Ogawa, N. Okateva, A. Olshevsky, T. Omura, K. Ozaki, A. Paoloni, B. D. Park, I. G. Park, A. Pastore, L. Patrizii, E. Pennacchio, H. Pessard, C. Pistillo, D. Podgrudkov, N. Polukhina, M. Pozzato, K. Pretzl, F. Pupilli, R. Rescigno, M. Roda, H. Rokujo, T. Roganova, G. Rosa, I. Rostovtseva, A. Rubbia, O. Ryazhskaya, O. Sato, Y. Sato, A. Schembri, W. Schmidt-Parzefal, I. Shakiryanova, T. Shchedrina, A. Sheshukov, H. Shibuya, T. Shiraishi, G. Shoziyoev, S. Simone, M. Sioli, C. Sirignano, G. Sirri, M. Spinetti, L. Stanco, N. Starkov, S. M. Stellacci, M. Stipcevic, T. Strauss, P. Strolin, K. Suzuki, S. Takahashi, M. Tenti, F. Terranova, V. Tioukov, S. Tufanli, P. Vilain, M. Vladimirov, L. Votano, J. L. Vuilleumier, G. Wilquet, B. Wonsak, C. S. Yoon, J. Yoshida, M. Yoshimoto, Y. Zaitsev, S. Zemskova, A. Zghiche

The OPERA experiment is designed to search for $\nu_{\mu} \rightarrow \nu_{\tau}$ oscillations in appearance mode i.e. through the direct observation of the $\tau$ lepton in $\nu_{\tau}$ charged current interactions. Read More

2013Aug
Authors: OPERA Collaboration, N. Agafonova, A. Aleksandrov, A. Anokhina, S. Aoki, A. Ariga, T. Ariga, T. Asada, D. Autiero, A. Badertscher, A. Ben Dhahbi, D. Bender, A. Bertolin, C. Bozza, R. Brugnera, G. Brunetti, B. Buettner, S. Buontempo, L. Chaussard, M. Chernyavskiy, V. Chiarella, A. Chukanov, L. Consiglio, N. D'Ambrosio, P. Del Amo Sanchez, G. De Lellis, M. De Serio, A. Di Crescenzo, D. Di Ferdinando, N. Di Marco, S. Dmitrievski, M. Dracos, D. Duchesneau, S. Dusini, J. Ebert, A. Ereditato, J. Favier, T. Ferber, R. A. Fini, T. Fukuda, A. Garfagnini, G. Giacomelli, C. Goellnitz, J. Goldberg, Y. Gornushkin, G. Grella, F. Grianti, A. M. Guler, C. Gustavino, C. Hagner, K. Hakamata, T. Hara, T. Hayakawa, M. Hierholzer, A. Hollnagel, B. Hosseini, H. Ishida, K. Ishiguro, M. Ishikawa, K. Jakovcic, C. Jollet, C. Kamiscioglu, M. Kamiscioglu, T. Katsuragawa, H. Kawahara, J. Kawada, J. H. Kim, S. H. Kim, M. Kimura, N. Kitagawa, B. Klicek, K. Kodama, M. Komatsu, U. Kose, I. Kreslo, A. Lauria, J. Lenkeit, A. Ljubicic, A. Longhin, P. Loverre, A. Malgin, G. Mandrioli, J. Marteau, T. Matsuo, V. Matveev, N. Mauri, E. Medinaceli, A. Meregaglia, P. Migliozzi, S. Mikado, A. Minotti, M. Miyanishi, E. Miyashita, P. Monacelli, M. C. Montesi, K. Morishima, M. T. Muciaccia, N. Naganawa, T. Naka, M. Nakamura, T. Nakano, Y. Nakatsuka, K. Niwa, S. Ogawa, N. Okateva, A. Olshevsky, T. Omura, K. Ozaki, A. Paoloni, B. D. Park, I. G. Park, A. Pastore, L. Patrizii, E. Pennacchio, H. Pessard, C. Pistillo, D. Podgrudkov, N. Polukhina, M. Pozzato, K. Pretzl, F. Pupilli, R. Rescigno, M. Roda, T. Roganova, H. Rokujo, G. Rosa, I. Rostovtseva, A. Rubbia, A. Russo, O. Ryazhskaya, O. Sato, Y. Sato, A. Schembri, W. Schmidt-Parzefall, I. Shakiryanova, T. Schcedrina, A. Sheshukov, H. Shibuya, T. Shiraishi, G. Shoziyoev, S. Simone, M. Sioli, C. Sirignano, G. Sirri, M. Spinetti, L. Stanco, N. Starkov, S. M. Stellacci, M. Stipcevic, T. Strauss, P. Strolin, K. Suzuki, S. Takahashi, M. Tenti, F. Terranova, V. Tioukov, P. Tolun, S. Tufanli, P. Vilain, M. Vladimirov, L. Votano, J. L. Vuilleumier, G. Wilquet, B. Wonsak, C. S. Yoon, J. Yoshida, M. Yoshimoto, Y. Zaitsev, S. Zemskova, A. Zghiche

The OPERA neutrino experiment is designed to perform the first observation of neutrino oscillations in direct appearance mode in the $\nu_\mu \to \nu_\tau$ channel, via the detection of the $\tau$-leptons created in charged current $\nu_\tau$ interactions. The detector, located in the underground Gran Sasso Laboratory, consists of an emulsion/lead target with an average mass of about 1.2 kt, complemented by electronic detectors. Read More

2013Mar
Authors: OPERA collaboration, N. Agafonova, A. Aleksandrov, A. Anokhina, S. Aoki, A. Ariga, T. Ariga, D. Autiero, A. Badertscher, A. Ben Dhahbi, A. Bertolin, C. Bozza, R. Brugnera, F. Brunet, G. Brunetti, B. Buettner, S. Buontempo, L. Chaussard, M. Chernyavsky, V. Chiarella, A. Chukanov, L. Consiglio, N. D'Ambrosio, G. De Lellis, M. De Serio, P. del Amo Sanchez, A. Di Crescenzo, D. Di Ferdinando, N. Di Marco, S. Dmitrievsky, M. Dracos, D. Duchesneau, S. Dusini, T. Dzhatdoev, J. Ebert, A. Ereditato, T. Ferber, R. A. Fini, T. Fukuda, A. Garfagnini, G. Giacomelli, C. Goellnitz, J. Goldberg, Y. Gornushkin, G. Grella, F. Grianti, A. M. Guler, C. Gustavino, C. Hagner, K. Hamada, T. Hara, M. Hierholzer, A. Hollnagel, B. Hosseini, H. Ishida, K. Ishiguro, K. Jakovcic, C. Jollet, F. Juget, C. Kamiscioglu, M. Kamiscioglu, J. Kawada, J. H. Kim, S. H. Kim, M. Kimura, N. Kitagawa, B. Klicek, K. Kodama, M. Komatsu, U. Kose, I. Kreslo, A. Lauria, J. Lenkeit, A. Ljubicic, A. Longhin, P. Loverre, A. Malgin, C. Mancini-Terracciano, G. Mandrioli, J. Marteau, T. Matsuo, V. Matveev, N. Mauri, E. Medinaceli, F. W. Meisel, A. Meregaglia, P. Migliozzi, S. Mikado, A. Minotti, P. Monacelli, M. C. Montesi, K. Morishima, M. T. Muciaccia, M. Nakamura, T. Nakano, Y. Nakatsuka, D. Naumov, K. Niwa, S. Ogawa, N. Okateva, A. Olchevsky, T. Omura, K. Ozaki, A. Paoloni, B. D. Park, I. G. Park, A. Pastore, L. Patrizii, E. Pennacchio, H. Pessard, C. Pistillo, D. Podgrudkov, N. Polukhina, M. Pozzato, K. Pretzl, F. Pupilli, R. Rescigno, M. Roda, T. Roganova, H. Rokujo, G. Rosa, I. Rostovtseva, A. Rubbia, A. Russo, O. Ryazhskaya, O. Sato, Y. Sato, T. Schchedrina, A. Schembri, W. Schmidt-Parzefall, I. Shakiryanova, A. Sheshukov, H. Shibuya, T. Shiraishi, G. Shoziyoev, S. Simone, M. Sioli, C. Sirignano, G. Sirri, M. Spinetti, L. Stanco, N. Starkov, S. M. Stellacci, M. Stipcevic, T. Strauss, P. Strolin, K. Suzuki, S. Takahashi, M. Tenti, F. Terranova, V. Tioukov, P. Tolun, S. Tufanli, P. Vilain, M. Vladimirov, L. Votano, J. -L. Vuilleumier, G. Wilquet, B. Wonsak, C. S. Yoon, J. Yoshida, Y. Zaitsev, S. Zemskova, A. Zghiche

A first result of the search for \numu $\rightarrow$ \nue oscillations in the OPERA experiment, located at the Gran Sasso Underground Laboratory, is presented. The experiment looked for the appearance of \nue in the CNGS neutrino beam using the data collected in 2008 and 2009. Data are compatible with the non-oscillation hypothesis in the three-flavour mixing model. Read More

2013Jan
Affiliations: 1LUNA collaboration, 2LUNA collaboration, 3LUNA collaboration, 4LUNA collaboration, 5LUNA collaboration, 6LUNA collaboration, 7LUNA collaboration, 8LUNA collaboration, 9LUNA collaboration, 10LUNA collaboration, 11LUNA collaboration, 12LUNA collaboration, 13LUNA collaboration, 14LUNA collaboration, 15LUNA collaboration, 16LUNA collaboration, 17LUNA collaboration, 18LUNA collaboration, 19LUNA collaboration, 20LUNA collaboration, 21LUNA collaboration, 22LUNA collaboration, 23LUNA collaboration, 24LUNA collaboration, 25LUNA collaboration, 26LUNA collaboration, 27LUNA collaboration, 28LUNA collaboration, 29LUNA collaboration

The production of the stable isotope Li-6 in standard Big Bang nucleosynthesis has recently attracted much interest. Recent observations in metal-poor stars suggest that a cosmological Li-6 plateau may exist. If true, this plateau would come in addition to the well-known Spite plateau of Li-7 abundances and would point to a predominantly primordial origin of Li-6, contrary to the results of standard Big Bang nucleosynthesis calculations. Read More

2012Dec
Authors: The OPERA Collaboration, T. Adam, N. Agafonova, A. Aleksandrov, A. Anokhina, S. Aoki, A. Ariga, T. Ariga, D. Autiero, A. Badertscher, A. Ben Dhahbi, M. Beretta, A. Bertolin, C. Bozza, T. Brugière, R. Brugnera, F. Brunet, G. Brunetti, B. Buettner, S. Buontempo, B. Carlus, F. Cavanna, A. Cazes, L. Chaussard, M. Chernyavsky, V. Chiarella, A. Chukanov, N. D'Ambrosio, G. De Lellis, M. De Serio, P. del Amo Sanchez, A. Di Crescenzo, D. Di Ferdinando, N. Di Marco, S. Dmitrievsky, M. Dracos, D. Duchesneau, S. Dusini, T. Dzhatdoev, J. Ebert, A. Ereditato, L. S. Esposito, J. Favier, G. Felici, T. Ferber, R. A. Fini, T. Fukuda, A. Garfagnini, G. Giacomelli, C. Girerd, C. Goellnitz, J. Goldberg, D. Golubkov, Y. Gornushkin, G. Grella, F. Grianti, C. Guerin, A. M. Guler, C. Gustavino, C. Hagner, K. Hamada, T. Hara, M. Hierholzer, A. Hollnagel, H. Ishida, K. Ishiguro, K. Jakovcic, C. Jollet, C. Kamiscioglu, M. Kamiscioglu, J. Kawada, J. H. Kim, S. H. Kim, M. Kimura, N. Kitagawa, B. Klicek, K. Kodama, M. Komatsu, U. Kose, I. Kreslo, A. Lauria, C. Lazzaro, J. Lenkeit, A. Ljubicic, A. Longhin, C. Mancini-Terracciano, A. Malgin, G. Mandrioli, J. Marteau, T. Matsuo, V. Matveev, N. Mauri, E. Medinaceli, A. Meregaglia, P. Migliozzi, S. Mikado, P. Monacelli, M. C. Montesi, K. Morishima, U. Moser, M. T. Muciaccia, M. Nakamura, T. Nakano, Y. Nakatsuka, D. Naumov, V. Nikitina, S. Ogawa, A. Olchevsky, K. Ozaki, O. Palamara, A. Paoloni, B. D. Park, I. G. Park, A. Pastore, L. Patrizii, E. Pennacchio, H. Pessard, C. Pistillo, D. Podgrudkov, N. Polukhina, M. Pozzato, K. Pretzl, F. Pupilli, R. Rescigno, M. Roda, T. Roganova, H. Rokujo, G. Rosa, I. Rostovtseva, A. Rubbia, A. Russo, O. Ryazhskaya, O. Sato, Y. Sato, A. Schembri, W. Schmidt-Parzefall, J. Schuler, I. Shakiryanova, A. Sheshukov, H. Shibuya, G. Shoziyoev, S. Simone, M. Sioli, C. Sirignano, G. Sirri, J. S. Song, M. Spinetti, L. Stanco, N. Starkov, S. M. Stellacci, M. Stipcevic, T. Strauss, S. Takahashi, M. Tenti, F. Terranova, V. Tioukov, P. Tolun, S. Tufanli, P. Vilain, M. Vladimirov, L. Votano, J. L. Vuilleumier, G. Wilquet, B. Wonsak, J. Wurtz, C. S. Yoon, J. Yoshida, Y. Zaitsev, S. Zemskova, A. Zghiche, R. Zimmermann

In spring 2012 CERN provided two weeks of a short bunch proton beam dedicated to the neutrino velocity measurement over a distance of 730 km. The OPERA neutrino experiment at the underground Gran Sasso Laboratory used an upgraded setup compared to the 2011 measurements, improving the measurement time accuracy. An independent timing system based on the Resistive Plate Chambers was exploited providing a time accuracy of $\sim$1 ns. Read More

Proton captures on Mg isotopes play an important role in the Mg-Al cycle active in stellar H-burning regions. In particular, low-energy nuclear resonances in the $^{25}$Mg(p,$\gamma$)$^{26}$Al reaction affect the production of radioactive $^{26}$Al$^{gs}$ as well as the resulting Mg/Al abundance ratio. Reliable estimations of these quantities require precise measurements of the strengths of low-energy resonances. Read More

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. Read More

The direct measurement of reaction cross sections at astrophysical energies often requires the use of solid targets of known thickness, isotopic composition, and stoichiometry that are able to withstand high beam currents for extended periods of time. Here, we report on the production and characterisation of isotopically enriched Ta$_2$O$_5$ targets for the study of proton-induced reactions at the Laboratory for Underground Nuclear Astrophysics facility of the Laboratori Nazionali del Gran Sasso. The targets were prepared by anodisation of tantalum backings in enriched water (up to 66% in $^{17}$O and up to 96% in $^{18}$O). Read More

2012Jun
Affiliations: 1the LVD Collaboration, 2the LVD Collaboration, 3the LVD Collaboration, 4the LVD Collaboration, 5the LVD Collaboration, 6the LVD Collaboration, 7the LVD Collaboration, 8the LVD Collaboration, 9the LVD Collaboration, 10the LVD Collaboration, 11the LVD Collaboration, 12the LVD Collaboration, 13the LVD Collaboration, 14the LVD Collaboration, 15the LVD Collaboration, 16the LVD Collaboration, 17the LVD Collaboration, 18the LVD Collaboration, 19the LVD Collaboration, 20the LVD Collaboration, 21the OPERA Collaboration, 22the OPERA Collaboration, 23the OPERA Collaboration, 24the OPERA Collaboration, 25the OPERA Collaboration, 26the OPERA Collaboration, 27the OPERA Collaboration, 28the OPERA Collaboration, 29the OPERA Collaboration, 30the OPERA Collaboration, 31the OPERA Collaboration, 32the OPERA Collaboration, 33the OPERA Collaboration, 34the OPERA Collaboration, 35the OPERA Collaboration, 36the OPERA Collaboration, 37the OPERA Collaboration, 38the OPERA Collaboration, 39the OPERA Collaboration, 40the OPERA Collaboration, 41the OPERA Collaboration, 42the OPERA Collaboration, 43the OPERA Collaboration, 44the OPERA Collaboration, 45the OPERA Collaboration, 46the OPERA Collaboration, 47the OPERA Collaboration, 48the OPERA Collaboration, 49the OPERA Collaboration, 50the OPERA Collaboration, 51the OPERA Collaboration, 52the OPERA Collaboration, 53the OPERA Collaboration, 54the OPERA Collaboration, 55the OPERA Collaboration, 56the OPERA Collaboration, 57the OPERA Collaboration, 58the OPERA Collaboration, 59the OPERA Collaboration, 60the OPERA Collaboration, 61the OPERA Collaboration, 62the OPERA Collaboration, 63the OPERA Collaboration, 64the OPERA Collaboration, 65the OPERA Collaboration, 66the OPERA Collaboration, 67the OPERA Collaboration, 68the OPERA Collaboration, 69the OPERA Collaboration, 70the OPERA Collaboration, 71the OPERA Collaboration, 72the OPERA Collaboration, 73the OPERA Collaboration, 74the OPERA Collaboration, 75the OPERA Collaboration, 76the OPERA Collaboration, 77the OPERA Collaboration, 78the OPERA Collaboration, 79the OPERA Collaboration, 80the OPERA Collaboration, 81the OPERA Collaboration, 82the OPERA Collaboration, 83the OPERA Collaboration, 84the OPERA Collaboration, 85the OPERA Collaboration, 86the OPERA Collaboration, 87the OPERA Collaboration, 88the OPERA Collaboration, 89the OPERA Collaboration, 90the OPERA Collaboration, 91the OPERA Collaboration

The purpose of this work is to report the measurement of a time-shift in the OPERA set-up in a totally independent way from Time Of Flight (TOF) measurements of CNGS neutrino events. The LVD and OPERA experiments are both installed in the same laboratory: LNGS. The relative position of the two detectors, separated by an average distance of ~ 160 m, allows the use of very high energy horizontal muons to cross-calibrate the timing systems of the two detectors, using a TOF technique which is totally independent from TOF of CNGS neutrino events. Read More

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. Read More

2011Sep
Authors: The OPERA Collaboration, T. Adam, N. Agafonova, A. Aleksandrov, O. Altinok, P. Alvarez Sanchez, A. Anokhina, S. Aoki, A. Ariga, T. Ariga, D. Autiero, A. Badertscher, A. Ben Dhahbi, A. Bertolin, C. Bozza, T. Brugiere, R. Brugnera, F. Brunet, G. Brunetti, S. Buontempo, B. Carlus, F. Cavanna, A. Cazes, L. Chaussard, M. Chernyavsky, V. Chiarella, A. Chukanov, G. Colosimo, M. Crespi, N. D'Ambrosio, G. De Lellis, M. De Serio, Y. Declais, P. del Amo Sanchez, F. Di Capua, A. Di Crescenzo, D. Di Ferdinando, N. Di Marco, S. Dmitrievsky, M. Dracos, D. Duchesneau, S. Dusini, T. Dzhatdoev, J. Ebert, I. Efthymiopoulos, O. Egorov, A. Ereditato, L. S. Esposito, J. Favier, T. Ferber, R. A. Fini, T. Fukuda, A. Garfagnini, G. Giacomelli, M. Giorgini, M. Giovannozzi, C. Girerd, J. Goldberg, C. Gollnitz, D. Golubkov, L. Goncharova, Y. Gornushkin, G. Grella, F. Grianti, E. Gschwendtner, C. Guerin, A. M. Guler, C. Gustavino, C. Hagner, K. Hamada, T. Hara, R. Enikeev, M. Hierholzer, A. Hollnagel, M. Ieva, H. Ishida, K. Ishiguro, K. Jakovcic, C. Jollet, M. Jones, F. Juget, M. Kamiscioglu, J. Kawada, S. H. Kim, M. Kimura, E. Kiritsis, N. Kitagawa, B. Klicek, J. Knuesel, K. Kodama, M. Komatsu, U. Kose, I. Kreslo, C. Lazzaro, J. Lenkeit, A. Ljubicic, A. Longhin, A. Malgin, G. Mandrioli, J. Marteau, T. Matsuo, V. Matveev, N. Mauri, A. Mazzoni, E. Medinaceli, F. Meisel, A. Meregaglia, P. Migliozzi, S. Mikado, D. Missiaen, P. Monacelli, K. Morishima, U. Moser, M. T. Muciaccia, N. Naganawa, T. Naka, M. Nakamura, T. Nakano, Y. Nakatsuka, D. Naumov, V. Nikitina, F. Nitti, S. Ogawa, N. Okateva, A. Olchevsky, O. Palamara, A. Paoloni, B. D. Park, I. G. Park, A. Pastore, L. Patrizii, E. Pennacchio, H. Pessard, C. Pistillo, N. Polukhina, M. Pozzato, K. Pretzl, F. Pupilli, R. Rescigno, F. Riguzzi, T. Roganova, H. Rokujo, G. Rosa, I. Rostovtseva, A. Rubbia, A. Russo, V. Ryasny, O. Ryazhskaya, O. Sato, Y. Sato, Z. Sahnoun, A. Schembri, J. Schuler, L. Scotto Lavina, J. Serrano, I. Shakiryanova, A. Sheshukov, H. Shibuya, G. Shoziyoev, S. Simone, M. Sioli, C. Sirignano, G. Sirri, J. S. Song, M. Spinetti, L. Stanco, N. Starkov, S. Stellacci, M. Stipcevic, T. Strauss, S. Takahashi, M. Tenti, F. Terranova, I. Tezuka, V. Tioukov, P. Tolun, N. T. Tran, S. Tufanli, P. Vilain, M. Vladimirov, L. Votano, J. -L. Vuilleumier, G. Wilquet, B. Wonsak, J. Wurtz, V. Yakushev, C. S. Yoon, J. Yoshida, Y. Zaitsev, S. Zemskova, A. Zghiche

The OPERA neutrino experiment at the underground Gran Sasso Laboratory has measured the velocity of neutrinos from the CERN CNGS beam over a baseline of about 730 km. The measurement is based on data taken by OPERA in the years 2009, 2010 and 2011. Dedicated upgrades of the CNGS timing system and of the OPERA detector, as well as a high precision geodesy campaign for the measurement of the neutrino baseline, allowed reaching comparable systematic and statistical accuracies. Read More

The NO cycle takes place in the deepest layer of a H-burning core or shell, when the temperature exceeds T {\simeq} 30 {\cdot} 106 K. The O depletion observed in some globular cluster giant stars, always associated with a Na enhancement, may be due to either a deep mixing during the RGB (red giant branch) phase of the star or to the pollution of the primordial gas by an early population of massive AGB (asymptotic giant branch) stars, whose chemical composition was modified by the hot bottom burning. In both cases, the NO cycle is responsible for the O depletion. Read More

2011Mar
Affiliations: 1LUNA collaboration, 2LUNA collaboration, 3LUNA collaboration, 4LUNA collaboration, 5LUNA collaboration, 6LUNA collaboration, 7LUNA collaboration, 8LUNA collaboration, 9LUNA collaboration, 10LUNA collaboration, 11LUNA collaboration, 12LUNA collaboration, 13LUNA collaboration, 14LUNA collaboration, 15LUNA collaboration, 16LUNA collaboration, 17LUNA collaboration, 18LUNA collaboration, 19LUNA collaboration, 20LUNA collaboration, 21LUNA collaboration, 22LUNA collaboration, 23LUNA collaboration, 24LUNA collaboration, 25LUNA collaboration, 26LUNA collaboration, 27LUNA collaboration, 28LUNA collaboration, 29LUNA collaboration

The rate of the carbon-nitrogen-oxygen (CNO) cycle of hydrogen burning is controlled by the 14N(p,gamma)15O reaction. The reaction proceeds by capture to the ground states and several excited states in O-15. In order to obtain a reliable extrapolation of the excitation curve to astrophysical energy, fits in the R-matrix framework are needed. Read More

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 Read More

Proton captures on Mg isotopes play an important role in the Mg-Al cycle active in stellar H shell burning. In particular, the strengths of low-energy resonances with E < 200 keV in 25Mg(p,gamma)26Al determine the production of 26Al and a precise knowledge of these nuclear data is highly desirable. Absolute measurements at such low-energies are often very difficult and hampered by gamma-ray background as well as changing target stoichiometry during the measurements. Read More

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. Read More

2010Mar
Authors: OPERA Collaboration, N. Agafonova, A. Anokhina, S. Aoki, A. Ariga, T. Ariga, D. Autiero, A. Badertscher, A. Bagulya, A. Bertolin, M. Besnier, D. Bick, V. Boyarkin, C. Bozza, T. Brugière, R. Brugnera, G. Brunetti, S. Buontempo, A. Cazes, L. Chaussard, M. Chernyavsky, V. Chiarella, N. Chon-Sen, A. Chukanov, M. Cozzi, G. D'Amato, F. Dal Corso, N. D'Ambrosio, G. De Lellis, Y. D'eclais, M. De Serio, F. Di Capua, D. Di Ferdinando, A. Di Giovanni, N. Di Marco, S. Dmitrievski, M. Dracos, D. Duchesneau, S. Dusini, J. Ebert, O. Egorov, R. Enikeev, A. Ereditato, L. S. Esposito, J. Favier, G. Felici, T. Ferber, R. Fini, D. Frekers, T. Fukuda, C. Fukushima, V. I. Galkin, A. Garfagnini, G. Giacomelli, M. Giorgini, C. Goellnitz, J. Goldberg, D. Golubkov, L. Goncharova, Y. Gornushkin, G. Grella, F. Grianti, M. Guler, C. Gustavino, C. Hagner, K. Hamada, T. Hara, M. Hierholzer, K. Hoshino, M. Ieva, K. Jakovcic, C. Jollet, F. Juget, M. Kazuyama, S. H. Kim, M. Kimura, B. Klicek, J. Knuesel, K. Kodama, M. Komatsu, U. Kose, I. Kreslo, H. Kubota, C. Lazzaro, J. Lenkeit, A. Ljubicic, A. Longhin, G. Lutter, A. Malgin, G. Mandrioli, A. Marotta, J. Marteau, T. Matsuo, V. Matveev, N. Mauri, E. Medinaceli, F. Meisel, A. Meregaglia, P. Migliozzi, S. Mikado, S. Miyamoto, P. Monacelli, K. Morishima, U. Moser, M. T. Muciaccia, N. Naganawa, T. Naka, M. Nakamura, T. Nakano, D. Naumov, V. Nikitina, K. Niwa, Y. Nonoyama, S. Ogawa, A. Olchevski, C. Oldorf, G. Orlova, V. Osedlo, M. Paniccia, A. Paoloni, B. D. Park, I. G. Park, A. Pastore, L. Patrizii, E. Pennacchio, H. Pessard, V. Pilipenko, C. Pistillo, G. Policastro, N. Polukhina, M. Pozzato, K. Pretzl, P. Publichenko, F. Pupilli, R. Rescigno, T. Roganova, H. Rokujo, G. Romano, G. Rosa, I. Rostovtseva, A. Rubbia, A. Russo, V. Ryasny, O. Ryazhskaya, O. Sato, Y. Sato, A. Schembri, W. Schmidt Parzefall, H. Schroeder, L. Scotto Lavina, A. Sheshukov, H. Shibuya, S. Simone, M. Sioli, C. Sirignano, G. Sirri, J. S. Song, M. Spinetti, L. Stanco, N. Starkov, M. Stipcevic, T. Strauss, P. Strolin, S. Takahashi, M. Tenti, F. Terranova, I. Tezuka, V. Tioukov, P. Tolun, T. Tran, S. Tufanli, P. Vilain, M. Vladimirov, L. Votano, J. L. Vuilleumier, G. Wilquet, B. Wonsak, V. Yakushev, C. S. Yoon, T. Yoshioka, J. Yoshida, Y. Zaitsev, S. Zemskova, A. Zghiche, R. Zimmermann

The OPERA detector at the Gran Sasso underground laboratory (LNGS) was used to measure the atmospheric muon charge ratio in the TeV energy region. We analyzed 403069 atmospheric muons corresponding to 113.4 days of livetime during the 2008 CNGS run. Read More

The 15N(p,gamma)16O reaction controls the passage of nucleosynthetic material from the first to the second carbon-nitrogen-oxygen (CNO) cycle. A direct measurement of the total 15N(p,gamma)16O cross section at energies corresponding to hydrogen burning in novae is presented here. Data have been taken at 90-230 keV center-of-mass energy using a windowless gas target filled with nitrogen of natural isotopic composition and a bismuth germanate summing detector. Read More

2008Dec
Affiliations: 1LUNA collaboration, 2LUNA collaboration, 3LUNA collaboration, 4LUNA collaboration, 5LUNA collaboration, 6LUNA collaboration, 7LUNA collaboration, 8LUNA collaboration, 9LUNA collaboration, 10LUNA collaboration, 11LUNA collaboration, 12LUNA collaboration, 13LUNA collaboration, 14LUNA collaboration, 15LUNA collaboration, 16LUNA collaboration, 17LUNA collaboration, 18LUNA collaboration, 19LUNA collaboration, 20LUNA collaboration, 21LUNA collaboration, 22LUNA collaboration, 23LUNA collaboration, 24LUNA collaboration, 25LUNA collaboration, 26LUNA collaboration, 27LUNA collaboration, 28LUNA collaboration, 29LUNA collaboration, 30LUNA collaboration, 31LUNA collaboration, 32LUNA collaboration

Ultra-sensitive in-beam gamma-ray spectroscopy studies for nuclear astrophysics are performed at the LUNA (Laboratory for Underground Nuclear Astrophysics) 400 kV accelerator, deep underground in Italy's Gran Sasso laboratory. By virtue of a specially constructed passive shield, the laboratory gamma-ray background for E_\gamma < 3 MeV at LUNA has been reduced to levels comparable to those experienced in dedicated offline underground gamma-counting setups. The gamma-ray background induced by an incident alpha-beam has been studied. Read More

The 3He(alpha,gamma)7Be process is a key reaction in both Big-Bang nucleosynthesis and p-p chain of Hydrogen Burning in Stars. A new measurement of the 3He(alpha,gamma)7Be 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. Read More

The rate of the hydrogen-burning carbon-nitrogen-oxygen (CNO) cycle is controlled by the slowest process, 14N(p,gamma)15O, which proceeds by capture to the ground and several excited states in 15O. Previous extrapolations for the ground state contribution disagreed by a factor 2, corresponding to 15% uncertainty in the total astrophysical S-factor. At the Laboratory for Underground Nuclear Astrophysics (LUNA) 400 kV accelerator placed deep underground in the Gran Sasso facility in Italy, a new experiment on ground state capture has been carried out at 317. Read More

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. Read More

We report on a new measurement of $^{14}$N(p,$\gamma$)$^{15}$O for the ground state capture transition at $E_p$ = 360, 380 and 400 keV, using the 400 kV LUNA accelerator. The true coincidence summing effect --the major source of error in the ground state capture determination-- has been significantly reduced by using a Clover--type gamma detector. Read More

Recently, the LUNA collaboration has carried out a high precision measurement on the 3He(alpha,gamma)7Be reaction cross section with both activation and on-line gamma-detection methods at unprecedented low energies. In this paper the results obtained with the activation method are summarized. The results are compared with previous activation experiments and the zero energy extrapolated astrophysical S factor is determined using different theoretical models. Read More

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. Read More

The flux of 7Be and 8B neutrinos from the Sun and the production of 7Li via primordial nucleosynthesis depend on the rate of the 3He(alpha,gamma)7Be reaction. In extension of a previous study showing cross section data at 127 - 167 keV center of mass energy, the present work reports on a measurement of the 3He(alpha,gamma)7Be cross section at 106 keV performed at Italy's Gran Sasso underground laboratory by the activation method. This energy is closer to the solar Gamow energy than ever reached before. Read More

The nuclear physics input from the 3He(alpha,gamma)7Be cross section is a major uncertainty in the fluxes of 7Be and 8B neutrinos from the Sun predicted by solar models and in the 7Li abundance obtained in big-bang nucleosynthesis calculations. The present work reports on a new precision experiment using the activation technique at energies directly relevant to big-bang nucleosynthesis. Previously such low energies had been reached experimentally only by the prompt-gamma technique and with inferior precision. Read More

The new experiment ``Extreme Energy Events'' (EEE) to detect extensive air showers through muon detection is starting in Italy. The use of particle detectors based on Multigap Resistive Plate Chambers (MRPC) will allow to determine with a very high accuracy the direction of the axis of cosmic ray showers initiated by primaries of ultra-high energy, together with a high temporal resolution. The installation of many of such 'telescopes' in numerous High Schools scattered all over the Italian territory will also allow to investigate coincidences between multiple primaries producing distant showers. Read More

In stars with temperatures above 20*10^6 K, hydrogen burning is dominated by the CNO cycle. Its rate is determined by the slowest process, the 14N(p,gamma)15O reaction. Deep underground in Italy's Gran Sasso laboratory, at the LUNA 400 kV accelerator, the cross section of this reaction has been measured at energies much lower than ever achieved before. Read More

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. Read More

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. Read More

The OPERA neutrino oscillation experiment foresees the construction of two magnetized iron spectrometers located after the lead-nuclear emulsion targets. The magnet is made up of two vertical walls of rectangular cross section connected by return yokes. The particle trajectories are measured by high precision drift tubes located before and after the arms of the magnet. Read More

The transition between the Main Sequence and the Red Giant Branch in low mass stars is powered by the onset of the CNO burning, whose bottleneck is the $^{14}$N(p,$\gamma)^{15}$O. The LUNA collaboration has recently improved the low energy measurements of the cross section of this key reaction. We analyse the impact of the revised reaction rate on the estimate of the Globular Clusters ages, as derived from the turnoff luminosity. Read More

A high-density calorimeter, consisting of magnetized iron planes interleaved by RPCs, as tracking and timing devices, is a good candidate for a next generation experiment on atmospheric neutrinos. With 34 kt of mass and in four years of data taking, this experiment will be sensitive to $\nu_\mu \to \nu_x$ oscillation with $\Delta m^2 > 6 \times 10^{-5}$ and mixing near to maximal and fully cover the region of oscillation parameters suggested by Super-Kamiokande results. Moreover, the experimental method will enable to measure the oscillation parameters from the modulation of the L/E spectrum ($\nu_\mu$ disappearance). Read More

We give the LUNA results on the cross section measurement of a key reaction of the proton-proton chain strongly affecting the calculated neutrino luminosity from the Sun: He3+He3-->He4+2p. Due to the cosmic ray suppression provided by the Gran Sasso underground laboratory it has been possible to measure the cross section down to the lower edge of the solar Gamow peak, i.e. Read More