Browsing by Author "Bellini, G."
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- Borexino’s search for low-energy neutrinos associated with gravitational wave events from GWTC-3 databaseBasilico, D.; Bellini, G.; Benziger, J.; Biondi, R.; Caccianiga, B.; Calaprice, F.; Caminata, A.; Chepurnov, A.; D’Angelo, D.; Derbin, A.; Di Giacinto, A.; Di Marcello, V.; Ding, X. F.; Di Ludovico, A.; Di Noto, L.; Drachnev, I.; Franco, D.; Galbiati, C.; Ghiano, C.; Giammarchi, M.; Goretti, A.; Gromov, M.; Guffanti, D.; Ianni, Aldo; Ianni, Andrea; Jany, A.; Kobychev, V.; Korga, G.; Kumaran, S.; Laubenstein, M.; Litvinovich, E.; Lombardi, P.; Lomskaya, I.; Ludhova, L.; Machulin, I.; Martyn, J.; Meroni, E.; Miramonti, L.; Misiaszek, M.; Muratova, V.; Nugmanov, R.; Oberauer, L.; Orekhov, V.; Ortica, F.; Pallavicini, M.; Pelicci, L.; Penek, Ö.; Pietrofaccia, L.; Pilipenko, N.; Pocar, A.; Raikov, G.; Ranalli, M. T.; Ranucci, G.; Re, A.; Rossi, N.; Schönert, S.; Semenov, D.; Settanta, G.; Skorokhvatov, M.; Singhal, A.; Smirnov, O.; Sotnikov, A.; Tartaglia, R.; Testera, G.; Unzhakov, E.; Vishneva, A.; Vogelaar, R. Bruce; von Feilitzsch, F.; Wojcik, M.; Wurm, M.; Zavatarelli, S.; Zuber, K.; Zuzel, G. (2023-06-26)The search for neutrino events in correlation with gravitational wave (GW) events for three observing runs (O1, O2 and O3) from 09/2015 to 03/2020 has been performed using the Borexino data-set of the same period. We have searched for signals of neutrino-electron scattering and inverse beta-decay (IBD) within a time window of ±1000 s centered at the detection moment of a particular GW event. The search was done with three visible energy thresholds of 0.25, 0.8 and 3.0 MeV. Two types of incoming neutrino spectra were considered: the mono-energetic line and the supernova-like spectrum. GW candidates originated by merging binaries of black holes (BHBH), neutron stars (NSNS) and neutron star and black hole (NSBH) were analyzed separately. Additionally, the subset of most intensive BHBH mergers at closer distances and with larger radiative mass than the rest was considered. In total, follow-ups of 74 out of 93 gravitational waves reported in the GWTC-3 catalog were analyzed and no statistically significant excess over the background was observed. As a result, the strongest upper limits on GW-associated neutrino and antineutrino fluences for all flavors (𝜈𝑒,𝜈𝜇,𝜈𝜏) at the level 109−1015 cm−2GW−1 have been obtained in the 0.5–5 MeV neutrino energy range.
- Constraints on flavor-diagonal non-standard neutrino interactions from Borexino Phase-IIAgarwalla, S. K.; Agostini, Matteo; Altenmueller, Konrad; Appel, S.; Atroshchenko, Victor; Bagdasarian, Zara; Basilico, D.; Bellini, G.; Benziger, Jay; Bick, D.; Bonfini, G.; Bravo, D.; Caccianiga, B.; Calaprice, F.; Caminata, A.; Cappelli, L.; Cavalcante, P.; Cavanna, F.; Chepurnov, A.; Choi, K.; D'Angelo, D.; Davini, S.; Derbin, A. V.; Di Giacinto, A.; Di Marcello, V.; Ding, X. F.; Di Ludovico, Antonio; Di Noto, Lea; Drachnev, I.; Fomenko, K.; Formozov, A.; Franco, D.; Gabriele, Federico; Galbiati, C.; Gschwender, M.; Ghiano, C.; Giammarchi, Marco; Goretti, A.; Gromov, M.; Guffanti, D.; Hagner, C.; Hungerford, Ed V.; Ianni, Aldo; Ianni, Andrea; Jany, A.; Jeschke, D.; Kumaran, S.; Kobychev, V.; Korga, G.; Lachenmaier, Tobias; Laubenstein, Matthias; Litvinovich, E.; Lombardi, Paolo; Ludhova, L.; Lukyanchenko, G.; Lukyanchenko, L.; Machulin, I. N.; Manuzio; Marcocci, S.; Maricic, Jelena; Martyn, J.; Meroni, E.; Meyer, M.; Miramonti, L.; Misiaszek, M.; Muratova, V. N.; Neumair, B.; Nieslony, M.; Oberauer, L.; Orekhov, V.; Ortica, F.; Pallavicini, M.; Papp, L.; Penek, O.; Pietrofaccia, L.; Pilipenko, N.; Pocar, A.; Raikov, G.; Ranucci, G.; Razeto, A.; Re, A.; Redchuk, M.; Romani, A.; Rossi, Nicola; Rottenanger, Sebastian; Schoenert, S.; Semenov, D. A.; Skorokhvatov, Mikhail D.; Smirnov, O. Y.; Sotnikov, A.; Sun, C.; Suvorov, Yura; Takeuchi, Tatsu; Tartaglia, R.; Testera, G.; Thurn, J.; Unzhakov, E. V.; Vishneva, A.; Vogelaar, R. Bruce; von Feilitzsch, F.; Wojcik, M. M.; Wurm, M.; Zaimidoroga, O.; Zavatarelli, S.; Zuber, Kai; Zuzel, G. (2020-02-05)The Borexino detector measures solar neutrino fluxes via neutrino-electron elastic scattering. Observed spectra are determined by the solar-nu(e) survival probability P-ee(E), and the chiral couplings of the neutrino and electron. Some theories of physics beyond the Standard Model postulate the existence of Non-Standard Interactions (NSI's) which modify the chiral couplings and P-ee(E). In this paper, we search for such NSI's, in particular, flavor-diagonal neutral current interactions that modify the nu(e)e and nu(tau)e couplings using Borexino Phase II data. Standard Solar Model predictions of the solar neutrino fluxes for both high- and low-metallicity assumptions are considered. No indication of new physics is found at the level of sensitivity of the detector and constraints on the parameters of the NSI's are placed. In addition, with the same dataset the value of sin(2)theta(W) is obtained with a precision comparable to that achieved in reactor antineutrino experiments .
- Modulations of the cosmic muon signal in ten years of Borexino dataAgostini, Matteo; Altenmueller, Konrad; Appel, S.; Atroshchenko, Victor; Bagdasarian, Zara; Basilico, D.; Bellini, G.; Benziger, Jay; Bick, D.; Bolognino, Irene; Bonfini, G.; Bravo, D.; Caccianiga, B.; Calaprice, F.; Caminata, A.; Caprioli, S.; Carlini, M.; Cavalcante, P.; Cavanna, F.; Chepurnov, A.; Choi, K.; Collica, L.; D'Angelo, D.; Davini, S.; Derbin, A. V.; Ding, X. F.; Di Ludovico, Antonio; Di Noto, Lea; Drachnev, I.; Fomenko, K.; Formozov, A.; Franco, D.; Gabriele, Federico; Galbiati, C.; Gschwender, M.; Ghiano, C.; Giammarchi, Marco; Goretti, A.; Gromov, M.; Guffanti, D.; Hagner, C.; Houdy, T.; Hungerford, Ed V.; Ianni, Aldo; Ianni, Andrea; Jany, A.; Jeschke, D.; Kobychev, V.; Korablev, D.; Korga, G.; Kudryavtsev, V. A.; Kumaran, S.; Lachenmaier, Tobias; Laubenstein, Matthias; Litvinovich, E.; Lombardi, Francesco; Lombardi, Paolo; Ludhova, L.; Lukyanchenko, G.; Lukyanchenko, L.; Machulin, I. N.; Manuzio, G.; Marcocci, S.; Maricic, Jelena; Martyn, J.; Meighen-Berger, S.; Meroni, E.; Meyer, M.; Miramonti, L.; Misiaszek, M.; Muratova, V. N.; Neumair, B.; Nieslony, M.; Oberauer, L.; Opitz, B.; Orekhov, V.; Ortica, F.; Pallavicini, M.; Papp, L.; Penek, Oe; Pietrofaccia, L.; Pilipenko, N.; Pocar, A.; Porcelli, A.; Raikov, G.; Ranucci, G.; Razeto, A.; Re, A.; Redchuk, M.; Romani, A.; Rossi, Nicola; Rottenanger, Sebastian; Schoenert, S.; Semenov, D. A.; Skorokhvatov, Mikhail D.; Smirnov, O. Y.; Sotnikov, A.; Stokes, Lee F. F.; Suvorov, Yura; Tartaglia, R.; Testera, G.; Thurn, J.; Toropova, M.; Unzhakov, E. V.; Vishneva, A.; Vogelaar, R. Bruce; von Feilitzsch, F.; Weinz, S.; Wojcik, M. M.; Wurm, M.; Yokley, Z. W.; Zaimidoroga, O.; Zavatarelli, S.; Zuber, Kai; Zuzel, G. (2019-02)We have measured the flux of cosmic muons in the Laboratori Nazionali del Gran Sasso at 3800 m.w.e. to be (3.432 +/- 0.003) center dot 10(-4) m(-2) s(-1) based on ten years of Borexino data acquired between May 2007 and May 2017. A seasonal modulation with a period of (366.3 +/- 0.6) d and a relative amplitude of (1.36 +/- 0.04)% is observed. The phase is measured to be (181.7 +/- 0.4) d, corresponding to a maximum at the 1 st of July. Using data inferred from global atmospheric models, we show the muon flux to be positively correlated with the atmospheric temperature and measure the e ff ective temperature coe ffi cient alpha(T) = 0.90 +/- 0.02. The origin of cosmic muons from pion and kaon decays in the atmosphere allows to interpret the e ff ective temperature coe ffi cient as an indirect measurement of the atmospheric kaon-topion production ratio r(K/pi) = 0.11(-0.07)(+0.11) for primary energies above 18TeV. We find evidence for a long-term modulation of the muon flux with a period of similar to 3000 d and a maximum in June 2012 that is not present in the atmospheric temperature data. A possible correlation between this modulation and the solar activity is investigated. The cosmogenic neutron production rate is found to show a seasonal modulation in phase with the cosmic muon flux but with an increased amplitude of (2.6 +/- 0.4)%.