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Denton PB. Sterile Neutrino Search with MicroBooNE's Electron Neutrino Disappearance Data. PHYSICAL REVIEW LETTERS 2022; 129:061801. [PMID: 36018666 DOI: 10.1103/physrevlett.129.061801] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/12/2021] [Revised: 05/17/2022] [Accepted: 07/12/2022] [Indexed: 06/15/2023]
Abstract
A sterile neutrino is a well motivated minimal new physics model that leaves an imprint in neutrino oscillations. Over the last two decades, a number of hints pointing to a sterile neutrino have emerged, many of which are pointing near m_{4}∼1 eV. Here, we show how MicroBooNE data can be used to search for electron neutrino disappearance using each of their four analysis channels. We find a hint for oscillations with the highest single channel significance of 2.4σ (using the Feldman-Cousins approach) coming from the Wire-Cell analysis and a simplified treatment of the experimental systematics. The preferred parameters are sin^{2}(2θ_{14})=0.35_{-0.16}^{+0.19} and Δm_{41}^{2}=1.25_{-0.39}^{+0.74} eV^{2}. This region of parameter space is in good agreement with existing hints from source experiments, is at a similar frequency but higher mixing than indicated by reactor antineutrinos, and is at the edge of the region allowed by solar neutrino data. Existing unanalyzed data from MicroBooNE could increase the sensitivity to the >3σ level.
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Affiliation(s)
- Peter B Denton
- High Energy Theory Group, Physics Department, Brookhaven National Laboratory, Upton, New York 11973, USA
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2
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Abstract
In this contribution, we summarise the determination of neutrino masses and mixing arising from global analysis of data from atmospheric, solar, reactor, and accelerator neutrino experiments performed in the framework of three-neutrino mixing and obtained in the context of the NuFIT collaboration. Apart from presenting the latest status as of autumn 2021, we discuss the evolution of global-fit results over the last 10 years, and mention various pending issues (and their resolution) that occurred during that period in the global analyses.
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3
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Stöcker P, Balázs C, Bloor S, Bringmann T, Gonzalo TE, Handley W, Hotinli S, Howlett C, Kahlhoefer F, Renk JJ, Scott P, Vincent AC, White M. Strengthening the bound on the mass of the lightest neutrino with terrestrial and cosmological experiments. Int J Clin Exp Med 2021. [DOI: 10.1103/physrevd.103.123508] [Citation(s) in RCA: 12] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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4
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de Gouvêa A, Martinez-Soler I, Perez-Gonzalez YF, Sen M. Fundamental physics with the diffuse supernova background neutrinos. Int J Clin Exp Med 2020. [DOI: 10.1103/physrevd.102.123012] [Citation(s) in RCA: 15] [Impact Index Per Article: 3.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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5
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Experimental evidence of neutrinos produced in the CNO fusion cycle in the Sun. Nature 2020; 587:577-582. [PMID: 33239797 DOI: 10.1038/s41586-020-2934-0] [Citation(s) in RCA: 76] [Impact Index Per Article: 19.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/26/2020] [Accepted: 10/02/2020] [Indexed: 11/08/2022]
Abstract
For most of their existence, stars are fuelled by the fusion of hydrogen into helium. Fusion proceeds via two processes that are well understood theoretically: the proton-proton (pp) chain and the carbon-nitrogen-oxygen (CNO) cycle1,2. Neutrinos that are emitted along such fusion processes in the solar core are the only direct probe of the deep interior of the Sun. A complete spectroscopic study of neutrinos from the pp chain, which produces about 99 per cent of the solar energy, has been performed previously3; however, there has been no reported experimental evidence of the CNO cycle. Here we report the direct observation, with a high statistical significance, of neutrinos produced in the CNO cycle in the Sun. This experimental evidence was obtained using the highly radiopure, large-volume, liquid-scintillator detector of Borexino, an experiment located at the underground Laboratori Nazionali del Gran Sasso in Italy. The main experimental challenge was to identify the excess signal-only a few counts per day above the background per 100 tonnes of target-that is attributed to interactions of the CNO neutrinos. Advances in the thermal stabilization of the detector over the last five years enabled us to develop a method to constrain the rate of bismuth-210 contaminating the scintillator. In the CNO cycle, the fusion of hydrogen is catalysed by carbon, nitrogen and oxygen, and so its rate-as well as the flux of emitted CNO neutrinos-depends directly on the abundance of these elements in the solar core. This result therefore paves the way towards a direct measurement of the solar metallicity using CNO neutrinos. Our findings quantify the relative contribution of CNO fusion in the Sun to be of the order of 1 per cent; however, in massive stars, this is the dominant process of energy production. This work provides experimental evidence of the primary mechanism for the stellar conversion of hydrogen into helium in the Universe.
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6
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Johnson JA, Fields BD, Thompson TA. The origin of the elements: a century of progress. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2020; 378:20190301. [PMID: 32811358 DOI: 10.1098/rsta.2019.0301] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 06/02/2020] [Indexed: 06/11/2023]
Abstract
This review assesses the current state of knowledge of how the elements were produced in the Big Bang, in stellar lives and deaths, and by interactions in interstellar gas. We begin with statements of fact and discuss the evidence that convinced astronomers that the Sun is fusing hydrogen, that low-mass stars produce heavy elements through neutron capture, that massive stars can explode as supernovae and that supernovae of all types produce new elements. Nucleosynthesis in the Big Bang, through cosmic ray spallation, and in exploding white dwarfs is only ranked below the above facts in certainty because the evidence, while overwhelming, is so far circumstantial. Next, we highlight the flaws in our current understanding of the predictions for lithium production in the Big Bang and/or its destruction in stars and for the production of the elements with atomic number [Formula: see text]. While the theory that neutron star mergers produce elements through neutron-capture has powerful circumstantial evidence, we are unconvinced that they produce all of the elements past nickel. Also in dispute is the exact mechanism or mechanisms that cause the white dwarfs to explode. It is difficult to determine the origin of rare isotopes because signatures of their production are weak. We are uncertain about the production sites of some lithium and nitrogen isotopes and proton-rich heavy nuclei. Finally, Betelgeuse is probably not the next star to become a supernovae in the Milky Way, in part because Betelgeuse may collapse directly to a black hole instead. The accumulated evidence in this review shows that we understand the major production sites for the elements, but islands of uncertainty in the periodic table exist. Resolving these uncertainties requires in particular understanding explosive events with compact objects and understanding the nature of the first stars and is therefore primed for new discoveries in the next decades. This article is part of the theme issue 'Mendeleev and the periodic table'.
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Affiliation(s)
- Jennifer A Johnson
- Department of Astronomy and Center for Cosmology and AstroParticle Physics, Ohio State University, Columbus, OH 43210, USA
| | - Brian D Fields
- Departments of Astronomy and of Physics, University of Illinois, Urbana, IL 61801, USA
| | - Todd A Thompson
- Department of Astronomy and Center for Cosmology and AstroParticle Physics, Ohio State University, Columbus, OH 43210, USA
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7
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Neutrinos reveal final secret of Sun’s nuclear fusion. Nature 2020; 583:20-21. [DOI: 10.1038/d41586-020-01908-2] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/08/2022]
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8
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Present and Future Contributions of Reactor Experiments to Mass Ordering and Neutrino Oscillation Studies. UNIVERSE 2020. [DOI: 10.3390/universe6040052] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
Abstract
After a long a glorious history, marked by the first direct proofs of neutrino existence and of the mixing between the first and third neutrino generations, the reactor antineutrino experiments are still well alive and will continue to give important contributions to the development of elementary particle physics and astrophysics. In parallel to the SBL (short baseline) experiments, that will be dedicated mainly to the search for sterile neutrinos, a new kind of experiments will start playing an important role: reactor experiments with a “medium” value, around 50 km, of the baseline, somehow in the middle between the SBL and the LBL (long baselines), like KamLAND, which in the recent past gave essential contributions to the developments of neutrino physics. These new medium baseline reactor experiments can be very important, mainly for the study of neutrino mass ordering. The first example of this kind, the liquid scintillator JUNO experiment, characterized by a very high mass and an unprecedented energy resolution, will soon start data collecting in China. Its main aspects are discussed here, together with its potentialities for what concerns the mass ordering investigation and also the other issues that can be studied with this detector, spanning from the accurate oscillation parameter determination to the study of solar neutrinos, geoneutrinos, atmospheric neutrinos and neutrinos emitted by supernovas and to the search for signals of potential Lorentz invariance violation.
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10
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Agostini M, Altenmüller K, Appel S, Atroshchenko V, Bagdasarian Z, Basilico D, Bellini G, Benziger J, Bick D, Bravo D, Caccianiga B, Calaprice F, Caminata A, Cavalcante P, Chepurnov A, D’Angelo D, Davini S, Derbin A, Di Giacinto A, Di Marcello V, Ding X, Di Ludovico A, Di Noto L, Drachnev I, Formozov A, Franco D, Galbiati C, Gschwender M, Ghiano C, Giammarchi M, Goretti A, Gromov M, Guffanti D, Hagner C, Houdy T, Hungerford E, Ianni A, Ianni A, Jany A, Jeschke D, Kobychev V, Korga G, Kumaran S, Lachenmaier T, Laubenstein M, Litvinovich E, Lombardi P, Lomskaya I, Ludhova L, Lukyanchenko G, Lukyanchenko L, Machulin I, Marcocci S, Martyn J, Meroni E, Meyer M, Miramonti L, Misiaszek M, Muratova V, Neumair B, Nieslony M, Nugmanov R, Oberauer L, Orekhov V, Ortica F, Pallavicini M, Papp L, Penek Ö, Pietrofaccia L, Pilipenko N, Pocar A, Raikov G, Ranalli M, Ranucci G, Razeto A, Re A, Redchuk M, Romani A, Rossi N, Rottenanger S, Schönert S, Semenov D, Skorokhvatov M, Smirnov O, Sotnikov A, Suvorov Y, Tartaglia R, Testera G, Thurn J, Unzhakov E, Vishneva A, Vogelaar R, von Feilitzsch F, Wojcik M, Wurm M, Zavatarelli S, Zuber K, Zuzel G. Improved measurement of
B8
solar neutrinos with
1.5 kt·y
of Borexino exposure. Int J Clin Exp Med 2020. [DOI: 10.1103/physrevd.101.062001] [Citation(s) in RCA: 17] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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11
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Abstract
This work explores the possibility of resorting to neutrino phenomenology to detect evidence of new physics, caused by the residual signals of the supposed quantum structure of spacetime. In particular, this work investigates the effects on neutrino oscillations and mass hierarchy detection, predicted by models that violate Lorentz invariance, preserving the spacetime isotropy and homogeneity. Neutrino physics is the ideal environment where conducting the search for new “exotic” physics, since the oscillation phenomenon is not included in the original formulation of the minimal Standard Model (SM) of particles. The confirmed observation of the neutrino oscillation phenomenon is, therefore, the first example of physics beyond the SM and can indicate the necessity to resort to new theoretical models. In this work, the hypothesis that the supposed Lorentz Invariance Violation (LIV) perturbations can influence the oscillation pattern is investigated. LIV theories are indeed constructed assuming modified kinematics, caused by the interaction of massive particles with the spacetime background. This means that the dispersion relations are modified, so it appears natural to search for effects caused by LIV in physical phenomena governed by masses, as in the case of neutrino oscillations. In addition, the neutrino oscillation phenomenon is interesting since there are three different mass eigenstates and in a LIV scenario, which preserves isotropy, at least two different species of particle must interact.
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12
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Abstract
Solar neutrinos have played a central role in the discovery of the neutrino oscillation mechanism. They still are proving to be a unique tool to help investigate the fusion reactions that power stars and further probe basic neutrino properties. The Borexino neutrino observatory has been operationally acquiring data at Laboratori Nazionali del Gran Sasso in Italy since 2007. Its main goal is the real-time study of low energy neutrinos (solar or originated elsewhere, such as geo-neutrinos). The latest analysis of experimental data, taken during the so-called Borexino Phase-II (2011-present), will be showcased in this talk—yielding new high-precision, simultaneous wide band flux measurements of the four main solar neutrino components belonging to the “pp” fusion chain (pp, pep, 7 Be, 8 B), as well as upper limits on the remaining two solar neutrino fluxes (CNO and hep).
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13
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Comprehensive measurement of pp-chain solar neutrinos. Nature 2018; 562:505-510. [DOI: 10.1038/s41586-018-0624-y] [Citation(s) in RCA: 108] [Impact Index Per Article: 18.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/23/2018] [Accepted: 08/23/2018] [Indexed: 11/09/2022]
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14
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Porcelli A, Agostini M, Altenmüller K, Appel S, Atroshchenko V, Bagdasarian Z, Basilico D, Bellini G, Benziger J, Bick D, Bonfini G, Bravo D, Caccianiga B, Calaprice F, Caminata A, Caprioli S, Carlini M, Cavalcante P, Chepurnov A, Choi K, Cloué O, Cribier M, D'Angelo D, Davini S, Derbin A, Ding X, Di Ludovico A, Di Noto L, Drachnev I, Durero M, Farinon S, Fischer V, Fomenko K, Formozov A, Franco D, Froborg F, Gabriele F, Gaffiot J, Galbiati C, Ghiano C, Giammarchi M, Goretti A, Gromov M, Gschwender M, Hagner C, Houdy T, Hungerford E, Ianni A, Ianni A, Jonquères N, Jany A, Jeschke D, Kobychev V, Korablev D, Korga G, Kornoukhov V, Kryn D, Lachenmaier T, Lasserre T, Laubenstein M, Litvinovich E, Lombardi F, Lombardi P, Ludhova L, Lukyanchenko G, Lukyanchenko L, Machulin I, Manuzio G, Marcocci S, Maricic J, Mention G, Martyn J, Meroni E, Meyer M, Miramonti L, Misiaszek M, Muratova V, Musenich R, Neumair B, Oberauer L, Opitz B, Ortica F, Pallavicini M, Papp L, Pilipenko N, Pocar A, Ranucci G, Razeto A, Re A, Romani A, Roncin R, Rossi N, Rottenanger S, Schönert S, Scola M, Semenov D, Skorokhvatov M, Smirnov O, Sotnikov A, Stokes L, Suvorov Y, Tartaglia R, Testera G, Thurn J, Toropova M, Unzhakov E, Veyssiére C, Vishneva A, Vivier M, Vogelaar R, von Feilitzsch F, Wang H, Weinz S, Wojcik M, Wurm M, Yokley Z, Zaimidoroga O, Zavatarelli S, Zuber K, Zuzel G. Recent Borexino results and perspectives of the SOX measurement. EPJ WEB OF CONFERENCES 2018. [DOI: 10.1051/epjconf/201818202099] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
Borexino is a liquid scintillator detector sited underground in the Laboratori Nazionali del Gran Sasso (Italy). Its physics program, until the end of this year, is focussed on the study of solar neutrinos, in particular from the Beryllium, pp, pep and CNO fusion reactions. Knowing the reaction chains in the sun provides insights towards physics disciplines such as astrophysics (star physics, star formation, etc.), astroparticle and particle physics. Phase II started in 2011 and its aim is to improve the phase I results, in particular the measurements of the neutrino fluxes from the pep and CNO processes. By the end of this year, data taking from the sun will be over and a new project is scheduled to launch: Short distance Oscillation with boreXino (SOX), which uses a Cerium source for neutrinos (100÷150 kCi of activity) and aims to confirm or rule out the presence of sterile neutrinos. This particle is hypothesised to justify the reactor, Gallium and LSND anomalies found and can reject extensions to the standard model. The work presented is a summary of the solar neutrino results achieved so far, which lead not only to a precise study of the processes in the sun, but also to more Standard Model oriented measurements (such as the stability of the charge, i.e. the life time of the electron). Furthermore, the perspectives of the SOX program are discussed showing the experiment sensitivity to a fourth neutrino state covering almost entirely 3σ of the preferred region of the anomalous neutrino experiments, and additional applications of the detector such as the study of geo-neutrinos.
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15
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Exploring the hidden interior of the Earth with directional neutrino measurements. Nat Commun 2017; 8:15989. [PMID: 28691700 PMCID: PMC5508127 DOI: 10.1038/ncomms15989] [Citation(s) in RCA: 15] [Impact Index Per Article: 2.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/28/2016] [Accepted: 05/16/2017] [Indexed: 11/09/2022] Open
Abstract
Roughly 40% of the Earth's total heat flow is powered by radioactive decays in the crust and mantle. Geo-neutrinos produced by these decays provide important clues about the origin, formation and thermal evolution of our planet, as well as the composition of its interior. Previous measurements of geo-neutrinos have all relied on the detection of inverse beta decay reactions, which are insensitive to the contribution from potassium and do not provide model-independent information about the spatial distribution of geo-neutrino sources within the Earth. Here we present a method for measuring previously unresolved components of Earth's radiogenic heating using neutrino-electron elastic scattering and low-background, direction-sensitive tracking detectors. We calculate the exposures needed to probe various contributions to the total geo-neutrino flux, specifically those associated to potassium, the mantle and the core. The measurements proposed here chart a course for pioneering exploration of the veiled inner workings of the Earth.
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16
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Zuzel G, Pelczar K, Wójcik M. Studies of surface and bulk 210Po in metals using an ultra-low background large surface alpha spectrometer. Appl Radiat Isot 2017; 126:165-167. [PMID: 28161104 DOI: 10.1016/j.apradiso.2017.01.030] [Citation(s) in RCA: 9] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/14/2016] [Revised: 12/30/2016] [Accepted: 01/23/2017] [Indexed: 11/17/2022]
Abstract
First measurements of natural surface and bulk 210Po specific activities for metals are reported. If covered with protective foils, the surfaces did not show indications of 210Po and the obtained upper limits are in the range of single mBqm-2. Weak bulk activities, in the range of 50 - 280mBqkg-1, were registered for Stainless Steel and Copper, while significant amounts of 210Po, ∼1.5Bqkg-1, were detected in Titanium. One special Teflon sample was investigated with respect to its bulk 210Po.
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Affiliation(s)
- G Zuzel
- M. Smoluchowski Institute of Physics, Jagiellonian University, Lojasiewicza 11, 30-348 Kraków, Poland.
| | - K Pelczar
- M. Smoluchowski Institute of Physics, Jagiellonian University, Lojasiewicza 11, 30-348 Kraków, Poland
| | - M Wójcik
- M. Smoluchowski Institute of Physics, Jagiellonian University, Lojasiewicza 11, 30-348 Kraków, Poland
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17
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18
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D’Angelo D, Agostini M, Altenmüller K, Appel S, Bellini G, Benziger J, Bick D, Bonfini G, Bravo D, Caccianiga B, Calaprice F, Caminata A, Cavalcante P, Chepurnov A, Davini S, Derbin A, Di Noto L, Drachnev I, Etenko A, Fomenko K, Franco D, Gabriele F, Galbiati C, Ghiano C, Giammarchi M, Goeger-Neff M, Goretti A, Gromov M, Hagner C, Hungerford E, Ianni A, Ianni A, Jedrzejczak K, Kaiser M, Kobychev V, Korablev D, Korga G, Kryn D, Laubenstein M, Lehnert B, Litvinovich E, Lombardi F, Lombardi P, Ludhova L, Lukyanchenko G, Machulin I, Manecki S, Maneschg W, Marcocci S, Meroni E, Meyer M, Miramonti L, Misiaszek M, Montuschi M, Mosteiro P, Muratova V, Neumair B, Oberauer L, Obolensky M, Ortica F, Pallavicini M, Papp L, Perasso L, Pocar A, Ranucci G, Razeto A, Re A, Romani A, Roncin R, Rossi N, Schönert S, Semenov D, Simgen H, Skorokhvatov M, Smirnov O, Sotnikov A, Sukhotin S, Suvorov Y, Tartaglia R, Testera G, Thurn J, Toropova M, Unzhakov E, Vishneva A, Vogelaar R, von Feilitzsch F, Wang H, Weinz S, Winter J, Wojcik M, Wurm M, Yokley Z, Zaimidoroga O, Zavatarelli S, Zuber K, Zuzel G. Recent Borexino results and prospects for the near future. EPJ WEB OF CONFERENCES 2016. [DOI: 10.1051/epjconf/201612602008] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/15/2022] Open
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19
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Kerman S, Sharma V, Deniz M, Wong H, Chen JW, Li H, Lin S, Liu CP, Yue Q. Coherency in neutrino-nucleus elastic scattering. Int J Clin Exp Med 2016. [DOI: 10.1103/physrevd.93.113006] [Citation(s) in RCA: 38] [Impact Index Per Article: 4.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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20
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Pallavicini M, Bellini G, Benziger J, Bick D, Bonfini G, Bravo D, Caccianiga B, Calaprice F, Caminata A, Cavalcante P, Chavarria A, Chepurnov A, D'Angelo D, Davini S, Derbin A, Empl A, Etenko A, Fomenko K, Franco D, Gabriele F, Galbiati C, Gazzana S, Ghiano C, Giammarchi M, Göger-Neff M, Goretti A, Gromov M, Hagner C, Hungerford E, Ianni A, Ianni A, Kayser M, Kobychev V, Korablëv D, Korga G, Kryn D, Laubenstein M, Lehnert B, Lewke T, Litvinovich E, Lombardi F, Lombardi P, Ludhova L, Lukyanchenko G, Machulin I, Manecki S, Maneschg W, Marcocci S, Meindl Q, Meroni E, Meyer M, Miramonti L, Misiaszek M, Montuschi M, Mosteiro P, Muratova V, Oberauer L, Obolensky M, Ortica F, Otis K, Papp L, Perasso L, Pocar A, Ranucci G, Razeto A, Re A, Romani A, Rossi N, Saldanha R, Salvo C, Schönert S, Simgen H, Skorokhvatov M, Smirnov O, Sotnikov A, Sukhotin S, Suvorov Y, Tartaglia R, Testera G, Vignaud D, Vogelaar R, Feilitzsch FV, Wang H, Winter J, Wojcik M, Wurm M, Zaimidoroga O, Zavatarelli S, Zuber K, Zuzel G. First real–time detection of solar pp neutrinos by Borexino. EPJ WEB OF CONFERENCES 2016. [DOI: 10.1051/epjconf/201612101001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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21
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Caminata A, Agostini M, Altenmüller K, Appel S, Bellini G, Benziger J, Berton N, Bick D, Bonfini G, Bravo D, Caccianiga B, Calaprice F, Cavalcante P, Chepurnov A, Cribier M, D'Angelo D, Davini S, Derbin A, Noto LD, Durero M, Empl A, Etenko A, Farinon S, Fischer V, Fomenko K, Franco D, Gabriele F, Gaffiot J, Galbiati C, Ghiano C, Giammarchi M, Göger-Neff M, Goretti A, Gromov M, Hagner C, Houdy T, Hungerford E, Ianni A, Ianni A, Jonquères N, Kaiser M, Kobychev V, Korablev D, Korga G, Kryn D, Lachenmaier T, Lasserre T, Laubenstein M, Lehnert B, Link J, Litvinovich E, Lombardi F, Lombardi P, Ludhova L, Lukyanchenko G, Machulin I, Maneschg W, Marcocci S, Maricic J, Mention G, Meroni E, Meyer M, Miramonti L, Misiaszek M, Montuschi M, Muratova V, Musenich R, Neumair B, Oberauer L, Obolensky M, Ortica F, Pallavicini M, Papp L, Perasso L, Pocar A, Ranucci G, Razeto A, Re A, Romani A, Rossi N, Schönert S, Scola L, Simgen H, Skorokhvatov M, Smirnov O, Sotnikov A, Sukhotin S, Suvorov Y, Tartaglia R, Testera G, Veyssière C, Vivier M, Vogelaar R, Feilitzsch FV, Wang H, Winter J, Wojcik M, Wurm M, Zaimidoroga O, Zavatarelli S, Zuber K, Zuzel G. Short distance neutrino oscillations with Borexino. EPJ WEB OF CONFERENCES 2016. [DOI: 10.1051/epjconf/201612101002] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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22
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Agostini M, Appel S, Bellini G, Benziger J, Bick D, Bonfini G, Bravo D, Caccianiga B, Calaprice F, Caminata A, Cavalcante P, Chepurnov A, D'Angelo D, Davini S, Derbin A, Di Noto L, Drachnev I, Empl A, Etenko A, Fomenko K, Franco D, Gabriele F, Galbiati C, Ghiano C, Giammarchi M, Goeger-Neff M, Goretti A, Gromov M, Hagner C, Hungerford E, Ianni A, Ianni A, Jedrzejczak K, Kaiser M, Kobychev V, Korablev D, Korga G, Kryn D, Laubenstein M, Lehnert B, Litvinovich E, Lombardi F, Lombardi P, Ludhova L, Lukyanchenko G, Machulin I, Manecki S, Maneschg W, Marcocci S, Meroni E, Meyer M, Miramonti L, Misiaszek M, Montuschi M, Mosteiro P, Muratova V, Neumair B, Oberauer L, Obolensky M, Ortica F, Otis K, Pallavicini M, Papp L, Perasso L, Pocar A, Ranucci G, Razeto A, Re A, Romani A, Roncin R, Rossi N, Schönert S, Semenov D, Simgen H, Skorokhvatov M, Smirnov O, Sotnikov A, Sukhotin S, Suvorov Y, Tartaglia R, Testera G, Thurn J, Toropova M, Unzhakov E, Vishneva A, Vogelaar RB, von Feilitzsch F, Wang H, Weinz S, Winter J, Wojcik M, Wurm M, Yokley Z, Zaimidoroga O, Zavatarelli S, Zuber K, Zuzel G. Test of Electric Charge Conservation with Borexino. PHYSICAL REVIEW LETTERS 2015; 115:231802. [PMID: 26684111 DOI: 10.1103/physrevlett.115.231802] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/03/2015] [Indexed: 06/05/2023]
Abstract
Borexino is a liquid scintillation detector located deep underground at the Laboratori Nazionali del Gran Sasso (LNGS, Italy). Thanks to the unmatched radio purity of the scintillator, and to the well understood detector response at low energy, a new limit on the stability of the electron for decay into a neutrino and a single monoenergetic photon was obtained. This new bound, τ≥6.6×10^{28} yr at 90% C.L., is 2 orders of magnitude better than the previous limit.
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Affiliation(s)
- M Agostini
- Physik-Department and Excellence Cluster Universe, Technische Universität München, 85748 Garching, Germany
- Gran Sasso Science Institute (INFN), 67100 Ł'Aquila, Italy
| | - S Appel
- Physik-Department and Excellence Cluster Universe, Technische Universität München, 85748 Garching, Germany
| | - G Bellini
- Dipartimento di Fisica, Università degli Studi e INFN, 20133 Milano, Italy
| | - J Benziger
- Chemical Engineering Department, Princeton University, Princeton, New Jersey 08544, USA
| | - D Bick
- Institut für Experimentalphysik, Universität Hamburg, 22761 Hamburg, Germany
| | - G Bonfini
- INFN Laboratori Nazionali del Gran Sasso, 67010 Assergi (AQ), Italy
| | - D Bravo
- Physics Department, Virginia Polytechnic Institute and State University, Blacksburg, Virginia 24061, USA
| | - B Caccianiga
- Dipartimento di Fisica, Università degli Studi e INFN, 20133 Milano, Italy
| | - F Calaprice
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
- Gran Sasso Science Institute (INFN), 67100 Ł'Aquila, Italy
| | - A Caminata
- Dipartimento di Fisica, Università degli Studi e INFN, 16146 Genova, Italy
| | - P Cavalcante
- INFN Laboratori Nazionali del Gran Sasso, 67010 Assergi (AQ), Italy
| | - A Chepurnov
- Lomonosov Moscow State University Skobeltsyn Institute of Nuclear Physics, 119234 Moscow, Russia
| | - D D'Angelo
- Dipartimento di Fisica, Università degli Studi e INFN, 20133 Milano, Italy
| | - S Davini
- Gran Sasso Science Institute (INFN), 67100 Ł'Aquila, Italy
| | - A Derbin
- St. Petersburg Nuclear Physics Institute NRC Kurchatov Institute, 188350 Gatchina, Russia
| | - L Di Noto
- Dipartimento di Fisica, Università degli Studi e INFN, 16146 Genova, Italy
| | - I Drachnev
- Gran Sasso Science Institute (INFN), 67100 Ł'Aquila, Italy
| | - A Empl
- Department of Physics, University of Houston, Houston, Texas 77204, USA
| | - A Etenko
- NRC Kurchatov Institute, 123182 Moscow, Russia
| | - K Fomenko
- Joint Institute for Nuclear Research, 141980 Dubna, Russia
| | - D Franco
- AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/IRFU, Observatoire de Paris, Sorbonne Paris Cité, 75205 Paris Cedex 13, France
| | - F Gabriele
- INFN Laboratori Nazionali del Gran Sasso, 67010 Assergi (AQ), Italy
| | - C Galbiati
- Dipartimento di Fisica, Università degli Studi e INFN, 20133 Milano, Italy
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - C Ghiano
- Dipartimento di Fisica, Università degli Studi e INFN, 16146 Genova, Italy
| | - M Giammarchi
- Dipartimento di Fisica, Università degli Studi e INFN, 20133 Milano, Italy
| | - M Goeger-Neff
- Physik-Department and Excellence Cluster Universe, Technische Universität München, 85748 Garching, Germany
| | - A Goretti
- INFN Laboratori Nazionali del Gran Sasso, 67010 Assergi (AQ), Italy
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - M Gromov
- Lomonosov Moscow State University Skobeltsyn Institute of Nuclear Physics, 119234 Moscow, Russia
- Lomonosov Moscow State University Faculty of Physics, 119234 Moscow, Russia
| | - C Hagner
- Institut für Experimentalphysik, Universität Hamburg, 22761 Hamburg, Germany
| | - E Hungerford
- Department of Physics, University of Houston, Houston, Texas 77204, USA
| | - Aldo Ianni
- INFN Laboratori Nazionali del Gran Sasso, 67010 Assergi (AQ), Italy
- Laboratorio Subterráneo de Canfranc, Paseo de los Ayerbe S/N, 22880 Canfranc, Estacion Huesca, Spain
| | - Andrea Ianni
- INFN Laboratori Nazionali del Gran Sasso, 67010 Assergi (AQ), Italy
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - K Jedrzejczak
- M. Smoluchowski Institute of Physics, Jagiellonian University, 30348 Krakow, Poland
| | - M Kaiser
- Institut für Experimentalphysik, Universität Hamburg, 22761 Hamburg, Germany
| | - V Kobychev
- Kiev Institute for Nuclear Research, 03680 Kiev, Ukraine
| | - D Korablev
- Joint Institute for Nuclear Research, 141980 Dubna, Russia
| | - G Korga
- INFN Laboratori Nazionali del Gran Sasso, 67010 Assergi (AQ), Italy
| | - D Kryn
- AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/IRFU, Observatoire de Paris, Sorbonne Paris Cité, 75205 Paris Cedex 13, France
| | - M Laubenstein
- INFN Laboratori Nazionali del Gran Sasso, 67010 Assergi (AQ), Italy
| | - B Lehnert
- Department of Physics, Technische Universität Dresden, 01062 Dresden, Germany
| | - E Litvinovich
- NRC Kurchatov Institute, 123182 Moscow, Russia
- National Research Nuclear University MEPhI (Moscow Engineering Physics Institute), 115409 Moscow, Russia
| | - F Lombardi
- INFN Laboratori Nazionali del Gran Sasso, 67010 Assergi (AQ), Italy
| | - P Lombardi
- Dipartimento di Fisica, Università degli Studi e INFN, 20133 Milano, Italy
| | - L Ludhova
- Dipartimento di Fisica, Università degli Studi e INFN, 20133 Milano, Italy
| | | | - I Machulin
- NRC Kurchatov Institute, 123182 Moscow, Russia
- National Research Nuclear University MEPhI (Moscow Engineering Physics Institute), 115409 Moscow, Russia
| | - S Manecki
- Physics Department, Virginia Polytechnic Institute and State University, Blacksburg, Virginia 24061, USA
| | - W Maneschg
- Max-Planck-Institut für Kernphysik, 69117 Heidelberg, Germany
| | - S Marcocci
- Gran Sasso Science Institute (INFN), 67100 Ł'Aquila, Italy
| | - E Meroni
- Dipartimento di Fisica, Università degli Studi e INFN, 20133 Milano, Italy
| | - M Meyer
- Institut für Experimentalphysik, Universität Hamburg, 22761 Hamburg, Germany
| | - L Miramonti
- Dipartimento di Fisica, Università degli Studi e INFN, 20133 Milano, Italy
| | - M Misiaszek
- M. Smoluchowski Institute of Physics, Jagiellonian University, 30348 Krakow, Poland
- INFN Laboratori Nazionali del Gran Sasso, 67010 Assergi (AQ), Italy
| | - M Montuschi
- Dipartimento di Fisica e Scienze della Terra Università degli Studi di Ferrara e INFN, 44122 Ferrara, Italy
| | - P Mosteiro
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - V Muratova
- St. Petersburg Nuclear Physics Institute NRC Kurchatov Institute, 188350 Gatchina, Russia
| | - B Neumair
- Physik-Department and Excellence Cluster Universe, Technische Universität München, 85748 Garching, Germany
| | - L Oberauer
- Physik-Department and Excellence Cluster Universe, Technische Universität München, 85748 Garching, Germany
| | - M Obolensky
- AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/IRFU, Observatoire de Paris, Sorbonne Paris Cité, 75205 Paris Cedex 13, France
| | - F Ortica
- Dipartimento di Chimica, Biologia e Biotecnologie, Università e INFN, 06123 Perugia, Italy
| | - K Otis
- Amherst Center for Fundamental Interactions and Physics Department, University of Massachusetts, Amherst, Massachusetts 01003, USA
| | - M Pallavicini
- Dipartimento di Fisica, Università degli Studi e INFN, 16146 Genova, Italy
| | - L Papp
- Physik-Department and Excellence Cluster Universe, Technische Universität München, 85748 Garching, Germany
| | - L Perasso
- Dipartimento di Fisica, Università degli Studi e INFN, 16146 Genova, Italy
| | - A Pocar
- Amherst Center for Fundamental Interactions and Physics Department, University of Massachusetts, Amherst, Massachusetts 01003, USA
| | - G Ranucci
- Dipartimento di Fisica, Università degli Studi e INFN, 20133 Milano, Italy
| | - A Razeto
- INFN Laboratori Nazionali del Gran Sasso, 67010 Assergi (AQ), Italy
| | - A Re
- Dipartimento di Fisica, Università degli Studi e INFN, 20133 Milano, Italy
| | - A Romani
- Dipartimento di Chimica, Biologia e Biotecnologie, Università e INFN, 06123 Perugia, Italy
| | - R Roncin
- AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/IRFU, Observatoire de Paris, Sorbonne Paris Cité, 75205 Paris Cedex 13, France
- INFN Laboratori Nazionali del Gran Sasso, 67010 Assergi (AQ), Italy
| | - N Rossi
- INFN Laboratori Nazionali del Gran Sasso, 67010 Assergi (AQ), Italy
| | - S Schönert
- Physik-Department and Excellence Cluster Universe, Technische Universität München, 85748 Garching, Germany
| | - D Semenov
- St. Petersburg Nuclear Physics Institute NRC Kurchatov Institute, 188350 Gatchina, Russia
| | - H Simgen
- Max-Planck-Institut für Kernphysik, 69117 Heidelberg, Germany
| | - M Skorokhvatov
- NRC Kurchatov Institute, 123182 Moscow, Russia
- National Research Nuclear University MEPhI (Moscow Engineering Physics Institute), 115409 Moscow, Russia
| | - O Smirnov
- Joint Institute for Nuclear Research, 141980 Dubna, Russia
| | - A Sotnikov
- Joint Institute for Nuclear Research, 141980 Dubna, Russia
| | - S Sukhotin
- NRC Kurchatov Institute, 123182 Moscow, Russia
| | - Y Suvorov
- Physics and Astronomy Department, University of California Los Angeles (UCLA), Los Angeles, California 90095, USA
| | - R Tartaglia
- INFN Laboratori Nazionali del Gran Sasso, 67010 Assergi (AQ), Italy
| | - G Testera
- Dipartimento di Fisica, Università degli Studi e INFN, 16146 Genova, Italy
| | - J Thurn
- Department of Physics, Technische Universität Dresden, 01062 Dresden, Germany
| | - M Toropova
- NRC Kurchatov Institute, 123182 Moscow, Russia
| | - E Unzhakov
- St. Petersburg Nuclear Physics Institute NRC Kurchatov Institute, 188350 Gatchina, Russia
| | - A Vishneva
- Joint Institute for Nuclear Research, 141980 Dubna, Russia
| | - R B Vogelaar
- Physics Department, Virginia Polytechnic Institute and State University, Blacksburg, Virginia 24061, USA
| | - F von Feilitzsch
- Physik-Department and Excellence Cluster Universe, Technische Universität München, 85748 Garching, Germany
| | - H Wang
- Physics and Astronomy Department, University of California Los Angeles (UCLA), Los Angeles, California 90095, USA
| | - S Weinz
- Institute of Physics and Excellence Cluster PRISMA, Johannes Gutenberg-Universität Mainz, 55099 Mainz, Germany
| | - J Winter
- Institute of Physics and Excellence Cluster PRISMA, Johannes Gutenberg-Universität Mainz, 55099 Mainz, Germany
| | - M Wojcik
- M. Smoluchowski Institute of Physics, Jagiellonian University, 30348 Krakow, Poland
| | - M Wurm
- Institute of Physics and Excellence Cluster PRISMA, Johannes Gutenberg-Universität Mainz, 55099 Mainz, Germany
| | - Z Yokley
- Physics Department, Virginia Polytechnic Institute and State University, Blacksburg, Virginia 24061, USA
| | - O Zaimidoroga
- Joint Institute for Nuclear Research, 141980 Dubna, Russia
| | - S Zavatarelli
- Dipartimento di Fisica, Università degli Studi e INFN, 16146 Genova, Italy
| | - K Zuber
- Department of Physics, Technische Universität Dresden, 01062 Dresden, Germany
| | - G Zuzel
- M. Smoluchowski Institute of Physics, Jagiellonian University, 30348 Krakow, Poland
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O’Hare CA, Green AM, Billard J, Figueroa-Feliciano E, Strigari LE. Readout strategies for directional dark matter detection beyond the neutrino background. Int J Clin Exp Med 2015. [DOI: 10.1103/physrevd.92.063518] [Citation(s) in RCA: 52] [Impact Index Per Article: 5.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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24
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Vincent AC, Scott P, Serenelli A. Possible indication of momentum-dependent asymmetric dark matter in the sun. PHYSICAL REVIEW LETTERS 2015; 114:081302. [PMID: 25768751 DOI: 10.1103/physrevlett.114.081302] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/05/2014] [Indexed: 06/04/2023]
Abstract
Broad disagreement persists between helioseismological observables and predictions of solar models computed with the latest surface abundances. Here we show that most of these problems can be solved by the presence of asymmetric dark matter coupling to nucleons as the square of the momentum q exchanged in the collision. We compute neutrino fluxes, small frequency separations, surface helium abundances, sound speed profiles, and convective zone depths for a number of models, showing more than a 6σ preference for q^{2} models over others, and over the standard solar model. The preferred mass (3 GeV) and reference dark matter-nucleon cross section (10^{-37} cm^{2} at q_{0}=40 MeV) are within the region of parameter space allowed by both direct detection and collider searches.
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Affiliation(s)
- Aaron C Vincent
- Institute for Particle Physics Phenomenology (IPPP), Department of Physics, Durham University, Durham DH1 3LE, United Kingdom
| | - Pat Scott
- Department of Physics, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, United Kingdom
| | - Aldo Serenelli
- Institut de Ciències de l'Espai (CSIC-IEEC), Campus UAB, Carrer de Can Magrans, s/n 08193 Cerdanyola del Vallés, Spain
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25
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Pallavicini M. Short review on solar neutrinos experiments and search for sterile neutrinos with solar neutrino detectors. EPJ WEB OF CONFERENCES 2015. [DOI: 10.1051/epjconf/20159503028] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/15/2022] Open
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26
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27
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Cowen R. Long-sought neutrinos answer burning question about the Sun. Nature 2014. [DOI: 10.1038/nature.2014.15779] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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