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Neutrino Physics & Energy

Neutrino physics, detection, and emerging energy applications. From neutrino oscillations (Nobel Prize 2015) and coherent elastic neutrino-nucleus scattering (C…

Physics / Energy
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Results for "neutrino oscillation detection energy"

1,000,317 total results — showing 20 from PubMed + NASA ADS + arXiv + OpenAlex
PubMed 2021 Nov

Electron-beam energy reconstruction for neutrino oscillation measurements.

Khachatryan M, Papadopoulou A, Ashkenazi A, Hauenstein F, Nambrath A, Hrnjic A, Weinstein L B, Hen O, Piasetzky E, Betancourt M, Dytman S, Mahn K, Coloma P

Nature

Show Abstract

Neutrinos exist in one of three types or 'flavours'-electron, muon and tau neutrinos-and oscillate from one flavour to another when propagating through space. This phenomena is one of the few that cannot be described using the standard model of particle physics (reviewed in ref. 1), and so its experimental study can provide new insight into the nature of our Universe (reviewed in ref. 2). Neutrinos oscillate as a function of their propagation distance (L) divided by their energy (E). Therefore, experiments extract oscillation parameters by measuring their energy distribution at different locations. As accelerator-based oscillation experiments cannot directly measure E, the interpretation of these experiments relies heavily on phenomenological models of neutrino-nucleus interactions to infer E. Here we exploit the similarity of electron-nucleus and neutrino-nucleus interactions, and use electron scattering data with known beam energies to test energy reconstruction methods and interaction models. We find that even in simple interactions where no pions are detected, only a small fraction of events reconstruct to the correct incident energy. More importantly, widely used interaction models reproduce the reconstructed energy distribution only qualitatively and the quality of the reproduction varies strongly with beam energy. This shows both the need and the pathway to improve current models to meet the requirements of next-generation, high-precision experiments such as Hyper-Kamiokande (Japan)3 and DUNE (USA)4.

PubMed 2013 Nov

Measurement of neutrino oscillation parameters from muon neutrino disappearance with an off-axis beam.

Abe K, Adam J, Aihara H, Akiri T, Andreopoulos C, Aoki S, Ariga A, Ariga T, Assylbekov S, Autiero D, Barbi M, Barker G J, Barr G, Bass M, Batkiewicz M, Bay F, Bentham S W, Berardi V, Berger B E, Berkman S, Bertram I, Bhadra S, Blaszczyk F D M, Blondel A, Bojechko C, Bordoni S, Boyd S B, Brailsford D, Bravar A, Bronner C, Buchanan N, Calland R G, Caravaca Rodríguez J, Cartwright S L, Castillo R, Catanesi M G, Cervera A, Cherdack D, Christodoulou G, Clifton A, Coleman J, Coleman S J, Collazuol G, Connolly K, Cremonesi L, Curioni A, Dabrowska A, Danko I, Das R, Davis S, de Perio P, De Rosa G, Dealtry T, Dennis S R, Densham C, Di Lodovico F, Di Luise S, Drapier O, Duboyski T, Duffy K, Dufour F, Dumarchez J, Dytman S, Dziewiecki M, Emery S, Ereditato A, Escudero L, Finch A J, Frank E, Friend M, Fujii Y, Fukuda Y, Furmanski A P, Galymov V, Gaudin A, Giffin S, Giganti C, Gilje K, Golan T, Gomez-Cadenas J J, Gonin M, Grant N, Gudin D, Hadley D R, Haesler A, Haigh M D, Hamilton P, Hansen D, Hara T, Hartz M, Hasegawa T, Hastings N C, Hayato Y, Hearty C, Helmer R L, Hierholzer M, Hignight J, Hillairet A, Himmel A, Hiraki T, Hirota S, Holeczek J, Horikawa S, Huang K, Ichikawa A K, Ieki K, Ieva M, Ikeda M, Imber J, Insler J, Irvine T J, Ishida T, Ishii T, Ives S J, Iyogi K, Izmaylov A, Jacob A, Jamieson B, Johnson R A, Jo J H, Jonsson P, Joo K K, Jung C K, Kaboth A C, Kajita T, Kakuno H, Kameda J, Kanazawa Y, Karlen D, Karpikov I, Kearns E, Khabibullin M, Khotjantsev A, Kielczewska D, Kikawa T, Kilinski A, Kim J, Kim S B, Kisiel J, Kitching P, Kobayashi T, Kogan G, Kolaceke A, Konaka A, Kormos L L, Korzenev A, Koseki K, Koshio Y, Kreslo I, Kropp W, Kubo H, Kudenko Y, Kumaratunga S, Kurjata R, Kutter T, Lagoda J, Laihem K, Laveder M, Lawe M, Lazos M, Lee K P, Licciardi C, Lim I T, Lindner T, Lister C, Litchfield R P, Longhin A, Lopez G D, Ludovici L, Macaire M, Magaletti L, Mahn K, Malek M, Manly S, Marino A D, Marteau J, Martin J F, Maruyama T, Marzec J, Masliah P, Mathie E L, Matveev V, Mavrokoridis K, Mazzucato E, McCarthy M, McCauley N, McFarland K S, McGrew C, Metelko C, Mijakowski P, Miller C A, Minamino A, Mineev O, Mine S, Missert A, Miura M, Monfregola L, Moriyama S, Mueller Th A, Murakami A, Murdoch M, Murphy S, Myslik J, Nagasaki T, Nakadaira T, Nakahata M, Nakai T, Nakamura K, Nakayama S, Nakaya T, Nakayoshi K, Naples D, Nielsen C, Nirkko M, Nishikawa K, Nishimura Y, O'Keeffe H M, Ohta R, Okumura K, Okusawa T, Oryszczak W, Oser S M, Otani M, Owen R A, Oyama Y, Pac M Y, Palladino V, Paolone V, Payne D, Pearce G F, Perevozchikov O, Perkin J D, Petrov Y, Pinzon Guerra E S, Pistillo C, Plonski P, Poplawska E, Popov B, Posiadala M, Poutissou J-M, Poutissou R, Przewlocki P, Quilain B, Radicioni E, Ratoff P N, Ravonel M, Rayner M A M, Redij A, Reeves M, Reinherz-Aronis E, Retiere F, Robert A, Rodrigues P A, Rondio E, Roth S, Rubbia A, Ruterbories D, Sacco R, Sakashita K, Sánchez F, Sato F, Scantamburlo E, Scholberg K, Schwehr J, Scott M, Seiya Y, Sekiguchi T, Sekiya H, Sgalaberna D, Shiozawa M, Short S, Shustrov Y, Sinclair P, Smith B, Smith R J, Smy M, Sobczyk J T, Sobel H, Sorel M, Southwell L, Stamoulis P, Steinmann J, Still B, Suda Y, Suzuki A, Suzuki K, Suzuki S Y, Suzuki Y, Szeglowski T, Tacik R, Tada M, Takahashi S, Takeda A, Takeuchi Y, Tanaka H K, Tanaka H A, Tanaka M M, Taylor I J, Terhorst D, Terri R, Thompson L F, Thorley A, Tobayama S, Toki W, Tomura T, Totsuka Y, Touramanis C, Tsukamoto T, Tzanov M, Uchida Y, Ueno K, Vacheret A, Vagins M, Vasseur G, Wachala T, Waldron A V, Walter C W, Wark D, Wascko M O, Weber A, Wendell R, Wilkes R J, Wilking M J, Wilkinson C, Williamson Z, Wilson J R, Wilson R J, Wongjirad T, Yamada Y, Yamamoto K, Yanagisawa C, Yen S, Yershov N, Yokoyama M, Yuan T, Zalewska A, Zalipska J, Zambelli L, Zaremba K, Ziembicki M, Zimmerman E D, Zito M, Zmuda J

Physical review letters

Show Abstract

The T2K Collaboration reports a precision measurement of muon neutrino disappearance with an off-axis neutrino beam with a peak energy of 0.6 GeV. Near detector measurements are used to constrain the neutrino flux and cross section parameters. The Super-Kamiokande far detector, which is 295 km downstream of the neutrino production target, collected data corresponding to 3.01×10(20) protons on target. In the absence of neutrino oscillations, 205±17 (syst) events are expected to be detected while only 58 muon neutrino event candidates are observed. A fit to the neutrino rate and energy spectrum, assuming three neutrino flavors and normal mass hierarchy yields a best-fit mixing angle sin2(θ23)=0.514±0.082 and mass splitting |Δm(32)(2)|=2.44(-0.15)(+0.17)×10(-3) eV2/c4. Our result corresponds to the maximal oscillation disappearance probability.

PubMed Review 2007 Mar

Antineutrino science by KamLAND.

Suzuki Atsuto

Proceedings of the Japan Academy. Series B, Physical and biological sciences

Show Abstract

KamLAND measured the ν̄ e's flux from distant nuclear reactors, and found fewer events than expected from standard assumptions about ν̄ e propagation at the 99.998% confidence level (C.L.). The observed energy spectrum disagrees with the expected spectral shape at 99.6% C.L., and prefers the distortion from neutrino oscillation effects. A two-flavor oscillation analysis of the data from KamLAND and solar neutrino experiments with CPT invariance, yields [Formula: see text] eV(2) and [Formula: see text]. All solutions to the solar neutrino problem except for the large mixing angle (LMA) region are excluded. KamLAND succeeded in detecting geoneutrinos produced by the decays of (238)U and (232)Th within the Earth. The total observed number of 4.5 to 54.2, assuming a Th/U mass concentration ratio of 3.9 is consistent with 19 predicted by geophysical models. This detection allows better estimation of the abundances and distributions of radioactive elements in the Earth, and of the Earth's overall heat budget.

PubMed 2022 Sep

QED radiative corrections for accelerator neutrinos.

Tomalak Oleksandr, Chen Qing, Hill Richard J, McFarland Kevin S

Nature communications

Show Abstract

Neutrino oscillation experiments at accelerator energies aim to establish charge-parity violation in the neutrino sector by measuring the energy-dependent rate of νe appearance and νμ disappearance in a νμ beam. These experiments can precisely measure νμ cross sections at near detectors, but νe cross sections are poorly constrained and require theoretical inputs. In particular, quantum electrodynamics radiative corrections are different for electrons and muons. These corrections are proportional to the small quantum electrodynamics coupling α ≈ 1/137; however, the large separation of scales between the neutrino energy and the proton mass (~GeV), and the electron mass and soft-photon detection thresholds (~MeV) introduces large logarithms in the perturbative expansion. The resulting flavor differences exceed the percent-level experimental precision and depend on nonperturbative hadronic structure. We establish a factorization theorem for exclusive charged-current (anti)neutrino scattering cross sections representing them as a product of two factors. The first factor is flavor universal; it depends on hadronic and nuclear structure and can be constrained by high-statistics νμ data. The second factor is non-universal and contains logarithmic enhancements, but can be calculated exactly in perturbation theory. For charged-current elastic scattering, we demonstrate the cancellation of uncertainties in the predicted ratio of νe and νμ cross sections. We point out the potential impact of non-collinear energetic photons and the distortion of the visible lepton spectra, and provide precise predictions for inclusive observables.

PubMed 2013 Aug

Measurement of atmospheric neutrino oscillations with IceCube.

Aartsen M G, Abbasi R, Abdou Y, Ackermann M, Adams J, Aguilar J A, Ahlers M, Altmann D, Auffenberg J, Bai X, Baker M, Barwick S W, Baum V, Bay R, Beatty J J, Bechet S, Becker Tjus J, Becker K-H, Bell M, Benabderrahmane M L, Benzvi S, Berdermann J, Berghaus P, Berley D, Bernardini E, Bernhard A, Bertrand D, Besson D Z, Binder G, Bindig D, Bissok M, Blaufuss E, Blumenthal J, Boersma D J, Bohaichuk S, Bohm C, Bose D, Böser S, Botner O, Brayeur L, Bretz H-P, Brown A M, Bruijn R, Brunner J, Carson M, Casey J, Casier M, Chirkin D, Christov A, Christy B, Clark K, Clevermann F, Coenders S, Cohen S, Cowen D F, Cruz Silva A H, Danninger M, Daughhetee J, Davis J C, De Clercq C, De Ridder S, Desiati P, de With M, DeYoung T, Díaz-Vélez J C, Dunkman M, Eagan R, Eberhardt B, Eisch J, Ellsworth R W, Euler S, Evenson P A, Fadiran O, Fazely A R, Fedynitch A, Feintzeig J, Feusels T, Filimonov K, Finley C, Fischer-Wasels T, Flis S, Franckowiak A, Franke R, Frantzen K, Fuchs T, Gaisser T K, Gallagher J, Gerhardt L, Gladstone L, Glüsenkamp T, Goldschmidt A, Golup G, Gonzalez J G, Goodman J A, Góra D, Grandmont D T, Grant D, Groß A, Ha C, Haj Ismail A, Hallen P, Hallgren A, Halzen F, Hanson K, Heereman D, Heinen D, Helbing K, Hellauer R, Hickford S, Hill G C, Hoffman K D, Hoffmann R, Homeier A, Hoshina K, Huelsnitz W, Hulth P O, Hultqvist K, Hussain S, Ishihara A, Jacobi E, Jacobsen J, Jagielski K, Japaridze G S, Jero K, Jlelati O, Kaminsky B, Kappes A, Karg T, Karle A, Kelley J L, Kiryluk J, Kislat F, Kläs J, Klein S R, Köhne J-H, Kohnen G, Kolanoski H, Köpke L, Kopper C, Kopper S, Koskinen D J, Kowalski M, Krasberg M, Krings K, Kroll G, Kunnen J, Kurahashi N, Kuwabara T, Labare M, Landsman H, Larson M J, Lesiak-Bzdak M, Leuermann M, Leute J, Lünemann J, Madsen J, Maruyama R, Mase K, Matis H S, McNally F, Meagher K, Merck M, Mészáros P, Meures T, Miarecki S, Middell E, Milke N, Miller J, Mohrmann L, Montaruli T, Morse R, Nahnhauer R, Naumann U, Niederhausen H, Nowicki S C, Nygren D R, Obertacke A, Odrowski S, Olivas A, Olivo M, O'Murchadha A, Palazzo A, Paul L, Pepper J A, Pérez de los Heros C, Pfendner C, Pieloth D, Pinat E, Pirk N, Posselt J, Price P B, Przybylski G T, Rädel L, Rameez M, Rawlins K, Redl P, Reimann R, Resconi E, Rhode W, Ribordy M, Richman M, Riedel B, Rodrigues J P, Rott C, Ruhe T, Ruzybayev B, Ryckbosch D, Saba S M, Salameh T, Sander H-G, Santander M, Sarkar S, Schatto K, Scheel M, Scheriau F, Schmidt T, Schmitz M, Schoenen S, Schöneberg S, Schönwald A, Schukraft A, Schulte L, Schulz O, Seckel D, Sestayo Y, Seunarine S, Sheremata C, Smith M W E, Soldin D, Spiczak G M, Spiering C, Stamatikos M, Stanev T, Stasik A, Stezelberger T, Stokstad R G, Stößl A, Strahler E A, Ström R, Sullivan G W, Taavola H, Taboada I, Tamburro A, Tepe A, Ter-Antonyan S, Tešić G, Tilav S, Toale P A, Toscano S, Usner M, van der Drift D, van Eijndhoven N, Van Overloop A, van Santen J, Vehring M, Voge M, Vraeghe M, Walck C, Waldenmaier T, Wallraff M, Wasserman R, Weaver Ch, Wellons M, Wendt C, Westerhoff S, Whitehorn N, Wiebe K, Wiebusch C H, Williams D R, Wissing H, Wolf M, Wood T R, Woschnagg K, Xu C, Xu D L, Xu X W, Yanez J P, Yodh G, Yoshida S, Zarzhitsky P, Ziemann J, Zierke S, Zoll M

Physical review letters

Show Abstract

We present the first statistically significant detection of neutrino oscillations in the high-energy regime (>20 GeV) from an analysis of IceCube Neutrino Observatory data collected in 2010 and 2011. This measurement is made possible by the low-energy threshold of the DeepCore detector (~20 GeV) and benefits from the use of the IceCube detector as a veto against cosmic-ray-induced muon background. The oscillation signal was detected within a low-energy muon neutrino sample (20-100 GeV) extracted from data collected by DeepCore. A high-energy muon neutrino sample (100 GeV-10 TeV) was extracted from IceCube data to constrain systematic uncertainties. The disappearance of low-energy upward-going muon neutrinos was observed, and the nonoscillation hypothesis is rejected with more than 5σ significance. In a two-neutrino flavor formalism, our data are best described by the atmospheric neutrino oscillation parameters |Δm(32)(2)|=(2.3(-0.5)(+0.6))×10(-3) eV(2) and sin(2)(2θ(23))>0.93, and maximum mixing is favored.

PubMed 2022 07

Scintillation light detection in the 6-m drift-length ProtoDUNE Dual Phase liquid argon TPC.

Abud A Abed, Abi B, Acciarri R, Acero M A, Adames M R, Adamov G, Adamowski M, Adams D, Adinolfi M, Aduszkiewicz A, Aguilar J, Ahmad Z, Ahmed J, Aimard B, Ali-Mohammadzadeh B, Alion T, Allison K, Monsalve S Alonso, AlRashed M, Alt C, Alton A, Alvarez R, Amedo P, Anderson J, Andreopoulos C, Andreotti M, Andrews M, Andrianala F, Andringa S, Anfimov N, Ankowski A, Antoniassi M, Antonova M, Antoshkin A, Antusch S, Aranda-Fernandez A, Arellano L, Arnold L O, Arroyave M A, Asaadi J, Asquith L, Aurisano A, Aushev V, Autiero D, Lara V Ayala, Ayala-Torres M, Azfar F, Back A, Back H, Back J J, Backhouse C, Bagaturia I, Bagby L, Balashov N, Balasubramanian S, Baldi P, Baller B, Bambah B, Barao F, Barenboim G, Alzas P Barham, Barker G, Barkhouse W, Barnes C, Barr G, Monarca J Barranco, Barros A, Barros N, Barrow J L, Basharina-Freshville A, Bashyal A, Basque V, Batchelor C, Chagas E Batista das, Battat J B R, Battisti F, Bay F, Bazetto M C Q, Alba J L L Bazo, Beacom J F, Bechetoille E, Behera B, Beigbeder C, Bellantoni L, Bellettini G, Bellini V, Beltramello O, Benekos N, Montiel C Benitez, Neves F Bento, Berger J, Berkman S, Bernardini P, Berner R M, Bersani A, Bertolucci S, Betancourt M, Rodríguez A Betancur, Bevan A, Bezawada Y, Bezerra T J C, Bhardwaj A, Bhatnagar V, Bhattacharjee M, Bhattarai D, Bhuller S, Bhuyan B, Biagi S, Bian J, Biassoni M, Biery K, Bilki B, Bishai M, Bitadze A, Blake A, Blaszczyk F, Blazey G C, Blucher E, Boissevain J, Bolognesi S, Bolton T, Bomben L, Bonesini M, Bongrand M, Bonilla-Diaz C, Bonini F, Booth A, Boran F, Bordoni S, Borkum A, Bostan N, Bour P, Bourgeois C, Boyden D, Bracinik J, Braga D, Brailsford D, Branca A, Brandt A, Bremer J, Breton D, Brew C, Brice S J, Brizzolari C, Bromberg C, Brooke J, Bross A, Brunetti G, Brunetti M, Buchanan N, Budd H, Butorov I, Cagnoli I, Cai T, Caiulo D, Calabrese R, Calafiura P, Calcutt J, Calin M, Calvez S, Calvo E, Caminata A, Campanelli M, Caratelli D, Carber D, Carceller J C, Carini G, Carlus B, Carneiro M F, Carniti P, Terrazas I Caro, Carranza H, Carroll T, Forero J F Castaño, Castillo A, Castromonte C, Catano-Mur E, Cattadori C, Cavalier F, Cavallaro G, Cavanna F, Centro S, Cerati G, Cervelli A, Villanueva A Cervera, Chalifour M, Chappell A, Chardonnet E, Charitonidis N, Chatterjee A, Chattopadhyay S, Neyra M S S Chavarry, Chen H, Chen M, Chen Y, Chen Z, Chen-Wishart Z, Cheon Y, Cherdack D, Chi C, Childress S, Chirco R, Chiriacescu A, Chisnall G, Cho K, Choate S, Chokheli D, Chong P S, Christensen A, Christian D, Christodoulou G, Chukanov A, Chung M, Church E, Cicero V, Clarke P, Cline G, Coan T E, Cocco A G, Coelho J A B, Colton N, Conley E, Conley R, Conrad J, Convery M, Copello S, Cova P, Cremaldi L, Cremonesi L, Crespo-Anadón J I, Crisler M, Cristaldo E, Crnkovic J, Cross R, Cudd A, Cuesta C, Cui Y, Cussans D, Dalager O, da Motta H, Da Silva Peres L, David C, David Q, Davies G S, Davini S, Dawson J, De K, De S, Debbins P, De Bonis I, Decowski M P, De Gouvêa A, De Holanda P C, De Icaza Astiz I L, Deisting A, De Jong P, Delbart A, Delepine D, Delgado M, Dell'Acqua A, Delmonte N, De Lurgio P, de Mello Neto J R T, DeMuth D M, Dennis S, Densham C, Deptuch G W, De Roeck A, De Romeri V, De Souza G, Devi R, Dharmapalan R, Dias M, Diaz F, Díaz J S, Domizio S Di, Giulio L Di, Ding P, Noto L Di, Dirkx G, Distefano C, Diurba R, Diwan M, Djurcic Z, Doering D, Dolan S, Dolek F, Dolinski M, Domine L, Donon Y, Douglas D, Douillet D, Dragone A, Drake G, Drielsma F, Duarte L, Duchesneau D, Duffy K, Dunne P, Dutta B, Duyang H, Dvornikov O, Dwyer D, Dyshkant A, Eads M, Earle A, Edmunds D, Eisch J, Emberger L, Emery S, Englezos P, Ereditato A, Erjavec T, Escobar C, Eurin G, Evans J J, Ewart E, Ezeribe A C, Fahey K, Falcone A, Fani' M, Farnese C, Farzan Y, Fedoseev D, Felix J, Feng Y, Fernandez-Martinez E, Menendez P Fernandez, Morales M Fernandez, Ferraro F, Fields L, Filip P, Filthaut F, Fiorini M, Fischer V, Fitzpatrick R S, Flanagan W, Fleming B, Flight R, Fogarty S, Foreman W, Fowler J, Fox W, Franc J, Francis K, Franco D, Freeman J, Freestone J, Fried J, Friedland A, Robayo F Fuentes, Fuess S, Furic I K, Furman K, Furmanski A P, Gabrielli A, Gago A, Gallagher H, Gallas A, Gallego-Ros A, Gallice N, Galymov V, Gamberini E, Gamble T, Ganacim F, Gandhi R, Gandrajula R, Gao F, Gao S, Garcia-Gamez D, García-Peris M Á, Gardiner S, Gastler D, Gauvreau J, Ge G, Geffroy N, Gelli B, Gendotti A, Gent S, Ghorbani-Moghaddam Z, Giammaria P, Giammaria T, Giangiacomi N, Gibin D, Gil-Botella I, Gilligan S, Girerd C, Giri A K, Gnani D, Gogota O, Gold M, Gollapinni S, Gollwitzer K, Gomes R A, Bermeo L V Gomez, Fajardo L S Gomez, Gonnella F, Gonzalez-Diaz D, Gonzalez-Lopez M, Goodman M C, Goodwin O, Goswami S, Gotti C, Goudzovski E, Grace C, Gran R, Granados E, Granger P, Grant A, Grant C, Gratieri D, Green P, Greenler L, Greer J, Grenard J, Griffith W C, Groh M, Grudzinski J, Grzelak K, Gu W, Guardincerri E, Guarino V, Guarise M, Guenette R, Guerard E, Guerzoni M, Guffanti D, Guglielmi A, Guo B, Gupta A, Gupta V, Guthikonda K K, Gutierrez R, Guzowski P, Guzzo M M, Gwon S, Ha C, Haaf K, Habig A, Hadavand H, Haenni R, Hahn A, Haiston J, Hamacher-Baumann P, Hamernik T, Hamilton P, Han J, Harris D A, Hartnell J, Hartnett T, Harton J, Hasegawa T, Hasnip C, Hatcher R, Hatfield K W, Hatzikoutelis A, Hayes C, Hayrapetyan K, Hays J, Hazen E, He M, Heavey A, Heeger K M, Heise J, Henry S, Morquecho M A Hernandez, Herner K, Hewes J, Hilgenberg C, Hill T, Hillier S J, Himmel A, Hinkle E, Hirsch L R, Ho J, Hoff J, Holin A, Hoppe E, Horton-Smith G A, Hostert M, Hourlier A, Howard B, Howell R, Hoyos J, Hristova I, Hronek M S, Huang J, Hulcher Z, Iles G, Ilic N, Iliescu A M, Illingworth R, Ingratta G, Ioannisian A, Irwin B, Isenhower L, Itay R, Jackson C M, Jain V, James E, Jang W, Jargowsky B, Jediny F, Jena D, Jeong Y S, Jesús-Valls C, Ji X, Jiang L, Jiménez S, Jipa A, Johnson R, Johnson W, Johnston N, Jones B, Jones S, Judah M, Jung C K, Junk T, Jwa Y, Kabirnezhad M, Kaboth A, Kadenko I, Kakorin I, Kalitkina A, Kalra D, Kamiya F, Kaneshige N, Kaplan D M, Karagiorgi G, Karaman G, Karcher A, Karolak M, Karyotakis Y, Kasai S, Kasetti S P, Kashur L, Kazaryan N, Kearns E, Keener P, Kelly K J, Kemp E, Kemularia O, Ketchum W, Kettell S H, Khabibullin M, Khotjantsev A, Khvedelidze A, Kim D, King B, Kirby B, Kirby M, Klein J, Klustova A, Kobilarcik T, Koehler K, Koerner L W, Koh D H, Kohn S, Koller P P, Kolupaeva L, Korablev D, Kordosky M, Kosc T, Kose U, Kostelecký V A, Kothekar K, Kralik R, Kreczko L, Krennrich F, Kreslo I, Kropp W, Kroupova T, Kubota S, Kudenko Y, Kudryavtsev V A, Kulagin S, Kumar J, Kumar P, Kunze P, Kurita N, Kuruppu C, Kus V, Kutter T, Kvasnicka J, Kwak D, Lambert A, Land B, Lane C E, Lang K, Langford T, Langstaff M, Larkin J, Lasorak P, Last D, Laundrie A, Laurenti G, Lawrence A, Lazanu I, LaZur R, Lazzaroni M, Le T, Leardini S, Learned J, LeBrun P, LeCompte T, Lee C, Lee S Y, Miotto G Lehmann, Lehnert R, de Oliveira M A Leigui, Leitner M, Lepin L M, Li S W, Li Y, Liao H, Lin C S, Lin Q, Lin S, Lineros R A, Ling J, Lister A, Littlejohn B R, Liu J, Liu Y, Lockwitz S, Loew T, Lokajicek M, Lomidze I, Long K, Lord T, LoSecco J M, Louis W C, Lu X-G, Luk K B, Lunday B, Luo X, Luppi E, Lux T, Luzio V P, Maalmi J, MacFarlane D, Machado A A, Machado P, Macias C T, Macier J R, Maddalena A, Madera A, Madigan P, Magill S, Mahn K, Maio A, Major A, Maloney J A, Mandrioli G, Mandujano R C, Maneira J, Manenti L, Manly S, Mann A, Manolopoulos K, Plata M Manrique, Manyam V N, Manzanillas L, Marchan M, Marchionni A, Marciano W, Marfatia D, Mariani C, Maricic J, Marie R, Marinho F, Marino A D, Marsden D, Marshak M, Marshall C, Marshall J, Marteau J, Martín-Albo J, Martinez N, Caicedo D A Martinez, Miravé P Martínez, Martynenko S, Mascagna V, Mason K, Mastbaum A, Matichard F, Matsuno S, Matthews J, Mauger C, Mauri N, Mavrokoridis K, Mawby I, Mazza R, Mazzacane A, Mazzucato E, McAskill T, McCluskey E, McConkey N, McFarland K S, McGrew C, McNab A, Mefodiev A, Mehta P, Melas P, Mena O, Mendez H, Mendez P, Méndez D P, Menegolli A, Meng G, Messier M D, Metcalf W, Mettler T, Mewes M, Meyer H, Miao T, Michna G, Miedema T, Mikola V, Milincic R, Miller G, Miller W, Mills J, Mineev O, Minotti A, Miranda O G, Miryala S, Mishra C S, Mishra S R, Mislivec A, Mitchell M, Mladenov D, Mocioiu I, Moffat K, Moggi N, Mohanta R, Mohayai T A, Mokhov N, Molina J, Bueno L Molina, Montagna E, Montanari A, Montanari C, Montanari D, Zetina L M Montañno, Moon S H, Mooney M, Moor A F, Moreno D, Moretti D, Morris C, Mossey C, Mote M, Motuk E, Moura C A, Mousseau J, Mouster G, Mu W, Mualem L, Mueller J, Muether M, Mufson S, Muheim F, Muir A, Mulhearn M, Munford D, Muramatsu H, Murphy S, Musser J, Nachtman J, Nagu S, Nalbandyan M, Nandakumar R, Naples D, Narita S, Nath A, Navrer-Agasson A, Nayak N, Nebot-Guinot M, Negishi K, Nelson J K, Nesbit J, Nessi M, Newbold D, Newcomer M, Newton H, Nichol R, Nicolas-Arnaldos F, Nikolica A, Niner E, Nishimura K, Norman A, Norrick A, Northrop R, Novella P, Nowak J A, Oberling M, Ochoa-Ricoux J, Olivier A, Olshevskiy A, Onel Y, Onishchuk Y, Ott J, Pagani L, Palacio G, Palamara O, Palestini S, Paley J M, Pallavicini M, Palomares C, Vazquez W Panduro, Pantic E, Paolone V, Papadimitriou V, Papaleo R, Papanestis A, Paramesvaran S, Parke S, Parozzi E, Parsa Z, Parvu M, Pascoli S, Pasqualini L, Pasternak J, Pater J, Patrick C, Patrizii L, Patterson R B, Patton S J, Patzak T, Paudel A, Paulos B, Paulucci L, Pavlovic Z, Pawloski G, Payne D, Pec V, Peeters S J M, Perez A Pena, Pennacchio E, Penzo A, Peres O L G, Perry J, Pershey D, Pessina G, Petrillo G, Petta C, Petti R, Pia V, Piastra F, Pickering L, Pietropaolo F, Pimentel V L, Pinaroli G, Plows K, Plunkett R, Poling R, Pompa F, Pons X, Poonthottathil N, Poppi F, Pordes S, Porter J, Potekhin M, Potenza R, Potukuchi B V K S, Pozimski J, Pozzato M, Prakash S, Prakash T, Prest M, Prince S, Psihas F, Pugnere D, Qian X, Raaf J L, Radeka V, Rademacker J, Radics B, Rafique A, Raguzin E, Rai M, Rajaoalisoa M, Rakhno I, Rakotonandrasana A, Rakotondravohitra L, Rameika R, Delgado M A Ramirez, Ramson B, Rappoldi A, Raselli G, Ratoff P, Raut S, Razakamiandra R F, Rea E M, Real J S, Rebel B, Rechenmacher R, Reggiani-Guzzo M, Reichenbacher J, Reitzner S D, Sfar H Rejeb, Renshaw A, Rescia S, Resnati F, Ribas M, Riboldi S, Riccio C, Riccobene G, Rice L C J, Ricol J S, Rigamonti A, Rigaut Y, Rincón E V, Ritchie-Yates H, Rivera D, Robert A, Rochester L, Roda M, Rodrigues P, Alonso M J Rodriguez, Bonilla E Rodriguez, Rondon J Rodriguez, Rosauro-Alcaraz S, Rosenberg M, Rosier P, Roskovec B, Rossella M, Rossi M, Rout J, Roy P, Rubbia A, Rubbia C, Russell B, Ruterbories D, Rybnikov A, Saa-Hernandez A, Saakyan R, Sacerdoti S, Safford T, Sahu N, Sakashita K, Sala P, Samios N, Samoylov O, Sanchez M C, Sandberg V, Sanders D A, Sankey D, Santana S, Santos-Maldonado M, Saoulidou N, Sapienza P, Sarasty C, Sarcevic I, Savage G, Savinov V, Scaramelli A, Scarff A, Scarpelli A, Schefke T, Schellman H, Schifano S, Schlabach P, Schmitz D, Schneider A W, Scholberg K, Schukraft A, Segreto E, Selyunin A, Senise C R, Sensenig J, Sergi A, Sgalaberna D, Shaevitz M H, Shafaq S, Shaker F, Shamma M, Sharankova R, Sharma H R, Sharma R, Sharma R K, Shaw T, Shchablo K, Shepherd-Themistocleous C, Sheshukov A, Shin S, Shoemaker I, Shooltz D, Shrock R, Siegel H, Simard L, Sinclair J, Sinev G, Singh J, Singh J, Singh L, Singh P, Singh V, Sipos R, Sippach F W, Sirri G, Sitraka A, Siyeon K, Skarpaas K, Smith A, Smith E, Smith P, Smolik J, Smy M, Snider E, Snopok P, Snowden-Ifft D, Nunes M Soares, Sobel H, Soderberg M, Sokolov S, Salinas C J Solano, Söldner-Rembold S, Soleti S R, Solomey N, Solovov V, Sondheim W E, Sorel M, Sotnikov A, Soto-Oton J, Ugaldi F A Soto, Sousa A, Soustruznik K, Spagliardi F, Spanu M, Spitz J, Spooner N J C, Spurgeon K, Stancari M, Stanco L, Stanford C, Stein R, Steiner H M, Lisbôa A F Steklain, Stewart J, Stillwell B, Stock J, Stocker F, Stokes T, Strait M, Strauss T, Strigari L, Stuart A, Suarez J G, Sunción J M Suárez, Sullivan H, Summers D, Surdo A, Susic V, Suter L, Sutera C M, Svoboda R, Szczerbinska B, Szelc A M, Tanaka H, Tang S, Tapia A, Oregui B Tapia, Tapper A, Tariq S, Tarpara E, Tata N, Tatar E, Tayloe R, Teklu A M, Tennessen P, Tenti M, Terao K, Ternes C A, Terranova F, Testera G, Thakore T, Thea A, Thompson J L, Thorn C, Timm S C, Tishchenko V, Tomassetti L, Tonazzo A, Torbunov D, Torti M, Tortola M, Tortorici F, Tosi N, Totani D, Toups M, Touramanis C, Travaglini R, Trevor J, Trilov S, Trzaska W H, Tsai Y, Tsai Y-T, Tsamalaidze Z, Tsang K V, Tsverava N, Tufanli S, Tull C, Tyley E, Tzanov M, Uboldi L, Uchida M A, Urheim J, Usher T, Uzunyan S, Vagins M R, Vahle P, Valder S, Valdiviesso G D A, Valencia E, Valentim R, Vallari Z, Vallazza E, Valle J W F, Vallecorsa S, Berg R Van, de Water R G Van, Forero D Vanegas, Vannerom D, Varanini F, Oliva D Vargas, Varner G, Vasel J, Vasina S, Vasseur G, Vaughan N, Vaziri K, Ventura S, Verdugo A, Vergani S, Vermeulen M A, Verzocchi M, Vicenzi M, de Souza H Vieira, Vignoli C, Vilela C, Viren B, Vrba T, Wachala T, Waldron A V, Wallbank M, Wallis C, Wang H, Wang J, Wang L, Wang M H L S, Wang X, Wang Y, Wang Y, Warburton K, Warner D, Wascko M O, Waters D, Watson A, Wawrowska K, Weatherly P, Weber A, Weber M, Wei H, Weinstein A, Wenman D, Wetstein M, White A, Whitehead L H, Whittington D, Wilking M J, Wilkinson A, Wilkinson C, Williams Z, Wilson F, Wilson R J, Wisniewski W, Wolcott J, Wongjirad T, Wood A, Wood K, Worcester E, Worcester M, Wresilo K, Wret C, Wu W, Wu W, Xiao Y, Xie F, Yaeggy B, Yandel E, Yang G, Yang K, Yang T, Yankelevich A, Yershov N, Yonehara K, Yoon Y S, Young T, Yu B, Yu H, Yu H, Yu J, Yu Y, Yuan W, Zaki R, Zalesak J, Zambelli L, Zamorano B, Zani A, Zazueta L, Zeller G P, Zennamo J, Zeug K, Zhang C, Zhang S, Zhang Y, Zhao M, Zhivun E, Zhu G, Zimmerman E D, Zucchelli S, Zuklin J, Zutshi V, Zwaska R

The European physical journal. C, Particles and fields

Show Abstract

DUNE is a dual-site experiment for long-baseline neutrino oscillation studies, neutrino astrophysics and nucleon decay searches. ProtoDUNE Dual Phase (DP) is a 6  ×  6  ×  6 m 3 liquid argon time-projection-chamber (LArTPC) that recorded cosmic-muon data at the CERN Neutrino Platform in 2019-2020 as a prototype of the DUNE Far Detector. Charged particles propagating through the LArTPC produce ionization and scintillation light. The scintillation light signal in these detectors can provide the trigger for non-beam events. In addition, it adds precise timing capabilities and improves the calorimetry measurements. In ProtoDUNE-DP, scintillation and electroluminescence light produced by cosmic muons in the LArTPC is collected by photomultiplier tubes placed up to 7 m away from the ionizing track. In this paper, the ProtoDUNE-DP photon detection system performance is evaluated with a particular focus on the different wavelength shifters, such as PEN and TPB, and the use of Xe-doped LAr, considering its future use in giant LArTPCs. The scintillation light production and propagation processes are analyzed and a comparison of simulation to data is performed, improving understanding of the liquid argon properties.

PubMed 2018 Aug

Probing high-momentum protons and neutrons in neutron-rich nuclei.

Nature

Show Abstract

The atomic nucleus is one of the densest and most complex quantum-mechanical systems in nature. Nuclei account for nearly all the mass of the visible Universe. The properties of individual nucleons (protons and neutrons) in nuclei can be probed by scattering a high-energy particle from the nucleus and detecting this particle after it scatters, often also detecting an additional knocked-out proton. Analysis of electron- and proton-scattering experiments suggests that some nucleons in nuclei form close-proximity neutron-proton pairs1-12 with high nucleon momentum, greater than the nuclear Fermi momentum. However, how excess neutrons in neutron-rich nuclei form such close-proximity pairs remains unclear. Here we measure protons and, for the first time, neutrons knocked out of medium-to-heavy nuclei by high-energy electrons and show that the fraction of high-momentum protons increases markedly with the neutron excess in the nucleus, whereas the fraction of high-momentum neutrons decreases slightly. This effect is surprising because in the classical nuclear shell model, protons and neutrons obey Fermi statistics, have little correlation and mostly fill independent energy shells. These high-momentum nucleons in neutron-rich nuclei are important for understanding nuclear parton distribution functions (the partial momentum distribution of the constituents of the nucleon) and changes in the quark distributions of nucleons bound in nuclei (the EMC effect)1,13,14. They are also relevant for the interpretation of neutrino-oscillation measurements15 and understanding of neutron-rich systems such as neutron stars3,16.

PubMed 2014 Aug

Neutrinos from the primary proton-proton fusion process in the Sun.

Nature

Show Abstract

In the core of the Sun, energy is released through sequences of nuclear reactions that convert hydrogen into helium. The primary reaction is thought to be the fusion of two protons with the emission of a low-energy neutrino. These so-called pp neutrinos constitute nearly the entirety of the solar neutrino flux, vastly outnumbering those emitted in the reactions that follow. Although solar neutrinos from secondary processes have been observed, proving the nuclear origin of the Sun's energy and contributing to the discovery of neutrino oscillations, those from proton-proton fusion have hitherto eluded direct detection. Here we report spectral observations of pp neutrinos, demonstrating that about 99 per cent of the power of the Sun, 3.84 × 10(33) ergs per second, is generated by the proton-proton fusion process.

NASA ADS 2016-02-00
542 citations

Supernova neutrinos: production, oscillations and detection

Mirizzi, A., Tamborra, I., Janka, H.-Th., Saviano, N., Scholberg, K., Bollig, R., Hüdepohl, L., Chakraborty, S.

Nuovo Cimento Rivista Serie

Show Abstract

Neutrinos play a crucial role in the collapse and explosion of massive stars, governing the infall dynamics of the stellar core, triggering and fueling the explosion and driving the cooling and deleptonization of the newly formed neutron star. Due to their role neutrinos carry information from the heart of the explosion and, due to their weakly interacting nature, offer the only direct probe of the dynamics and thermodynamics at the center of a supernova. In this paper, we review the present status of modelling the neutrino physics and signal formation in collapsing and exploding stars. We assess the capability of current and planned large underground neutrino detectors to yield faithful information of the time and flavor-dependent neutrino signal from a future Galactic supernova. We show how the observable neutrino burst would provide a benchmark for fundamental supernova physics with unprecedented richness of detail. Exploiting the treasure of the measured neutrino events requires a careful discrimination of source-generated properties from signal features that originate on the way to the detector. As for the latter, we discuss self-induced flavor conversions associated with neutrino-neutrino interactions that occur in the deepest stellar regions; matter effects that modify the pattern of flavor conversions in the dynamical stellar envelope; neutrino-oscillation signatures that result from structural features associated with the shock-wave propagation as well as turbulent mass motions in post-shock layers. Finally, we highlight our current understanding of the formation of the diffuse supernova neutrino background and we analyse the perspectives for a detection of this relic signal that integrates the contributions from all past core-collapse supernovae in the Universe.

NASA ADS 2018-04-00
150 citations

What can be learned from a future supernova neutrino detection?

Horiuchi, Shunsaku, Kneller, James P.

Journal of Physics G Nuclear Physics

Show Abstract

This year marks the 30th anniversary of the only supernova from which we have detected neutrinos—SN 1987A. The 20 or so neutrinos that were detected were mined to great depth in order to determine the events that occurred in the explosion and to place limits upon all manner of neutrino properties. Since 1987 the scale and sensitivity of the detectors capable of identifying neutrinos from a Galactic supernova have grown considerably so that current generation detectors are capable of detecting of order 10 000 neutrinos for a supernova at the Galactic Center. Next generation detectors will increase that yield by another order of magnitude. Simultaneous with the growth of neutrino detection capability, our understanding of how massive stars explode and how the neutrino interacts with hot and dense matter has also increased by a tremendous degree. The neutrino signal will contain much information on all manner of physics of interest to a wide community. In this review we describe the expected features of the neutrino signal, the detectors which will detect it, and the signatures one might try to look for in order to get at this physics.

NASA ADS 2025-06-00
107 citations

Cosmology in Extended Parameter Space with DESI Data Release 2 Baryon Acoustic Oscillations: A 2σ+ Detection of Nonzero Neutrino Masses with an Update on Dynamical Dark Energy and Lensing Anomaly

Roy Choudhury, Shouvik

The Astrophysical Journal

Show Abstract

We obtain constraints in a 12 parameter cosmological model using the recent Dark Energy Spectroscopic Instrument Data Release (DR) 2 Baryon Acoustic Oscillations (BAO) data, combined with cosmic microwave background (CMB) power spectra (Planck Public Release, PR, 4) and lensing (Planck PR4 + Atacama Cosmology Telescope DR 6) data, uncalibrated Type Ia supernovae (SNe) data from Pantheon+ and Dark Energy Survey (DES) Year 5 (DESY5) samples, and Weak Lensing (WL; DES Year 1) data. The cosmological model consists of six Λ cold dark matter parameters and additionally, the dynamical dark energy parameters (w<SUB>0</SUB>, w<SUB>a</SUB>), the sum of neutrino masses (∑m<SUB>ν</SUB>), the effective number of non-photon radiation species (N<SUB>eff</SUB>), the scaling of the lensing amplitude (A<SUB>lens</SUB>), and the running of the scalar spectral index (α<SUB>s</SUB>). Our major findings are the following: (i) With CMB+BAO+DESY5+WL, we obtain the first 2σ+ detection of a non-zero <inline-formula> <mml:math><mml:mrow><mml:mo>∑</mml:mo></mml:mrow><mml:msub><mml:mrow><mml:mi>m</mml:mi></mml:mrow><mml:mrow><mml:mi>ν</mml:mi></mml:mrow></mml:msub><mml:mo>=</mml:mo><mml:mn>0.1</mml:mn><mml:msubsup><mml:mrow><mml:mn>9</mml:mn></mml:mrow><mml:mrow><mml:mo>−</mml:mo><mml:mn>0.18</mml:mn></mml:mrow><mml:mrow><mml:mo>+</mml:mo><mml:mn>0.15</mml:mn></mml:mrow></mml:msubsup></mml:math> </inline-formula> eV (95%). Replacing DESY5 with Pantheon+ still yields a ∼1.9σ detection. (ii) The cosmological constant lies at the edge of the 95% contour with CMB+BAO+Pantheon+ but is excluded at 2σ+ with DESY5, leaving evidence for dynamical dark energy data-set dependent and inconclusive. (iii) With CMB+BAO+SNe+WL, A<SUB>lens</SUB> = 1 is excluded at &gt;2σ, while it remains consistent with unity without WL data—suggesting that the existence of lensing anomaly with Planck PR4 likelihoods may depend on non-CMB data sets. (iv) The Hubble tension persists at 3.6σ─4.2σ with CMB+BAO+SNe; WL data have minimal impact.

NASA ADS 1998-02-00
708 citations

Initial results from the CHOOZ long baseline reactor neutrino oscillation experiment

Apollonio, M., Baldini, A., Bemporad, C., Caffau, E., Cei, F., Déclais, Y., de Kerret, H., Dieterle, B., Etenko, A., George, J., Giannini, G., Grassi, M., Kozlov, Y., Kropp, W., Kryn, D., Laiman, M., Lane, C. E., Lefièvre, B., Machulin, I., Martemyanov, A., Martemyanov, V., Mikaelyan, L., Nicolò, D., Obolensky, M., Pazzi, R., Pieri, G., Price, L., Riley, S., Reeder, R., Sabelnikov, A., Santin, G., Skorokhvatov, M., Sobel, H., Steele, J., Steinberg, R., Sukhotin, S., Tomshaw, S., Veron, D., Vyrodov, V.

Physics Letters B

Show Abstract

Initial results are presented from CHOOZ, a long-baseline reactor-neutrino vacuum-oscillation experiment. The data reported here were taken during the period March to October 1997, when the two reactors ran at combined power levels varying from zero to values approaching their full rated power of 8.5 (thermal). Electron antineutrinos from the reactors were detected by a liquid scintillation calorimeter located at a distance of about 1. The detector was constructed in a tunnel protected from cosmic rays by a 300 rock overburden. This massive shielding strongly reduced potentially troublesome backgrounds due to cosmic-ray muons, leading to a background rate of about one event per day, more than an order of magnitude smaller than the observed neutrino signal. From the statistical agreement between detected and expected neutrino event rates, we find (at 90% confidence level) no evidence for neutrino oscillations in the disappearance mode for the parameter region given approximately by for maximum mixing and for large .

arXiv 2002-10-31

Very Long Baseline Neutrino Oscillation Experiment for Precise Determination of Oscillation Parameters and Search for nu_mu -> nu_e Appearance and CP Violation

BNL Neutrino Working Group, M. Diwan

arXiv:hep-ex/0211001v1 [hep-ex]

Show Abstract

The possibility of making a low cost, very intense (1MW) high energy proton source at the Brookhaven Alternating Gradient Synchrotron (BNL-AGS) along with the forthcoming new large underground detectors (approaching 1 MT in mass) at the National Underground Science and Engineering Laboratory (NUSEL) in Homestake, South Dakota or at the Waste Isolation Pilot Plant (WIPP) in Carlsbad, New Mexico, allows us to propose a program of experiments that will address fundamental aspects of neutrino oscillations and CP-invariance violation. This program is unique because of the very long baseline of more than 2500 km from BNL to the underground laboratory in the West. We used the running scenario of a low energy, wide band neutrino beam with 1 MW AGS, 500 kT of fiducial mass water Cherenkov detector, and 5x10^7 seconds of running time. In this report we show that with these conditions we precisely measure dm^2_32 and sin^2(2theta_23) and have excellent sensitivity to sin^2(2theta_13) with a distinctive signal spectrum. If sin^2(2theta_13) > 0.01 the experiment is sensitive to the CP-violating phase in the mixing matrix with only neutrino running. By running in the anti-neutrino mode we distinguish between the cases dm^2_31 > 0 versus dm^2_31 < 0 using distinctive distortions to the electron or positron spectrum. Lastly, the very long baseline allows the measurement of dm^2_21 (in the LMA region) with approximately the same resolution as KAMLAND but in the nu_mu -> nu_e appearance channel.

arXiv 2004-12-06

Report of the Solar and Atmospheric Neutrino Experiments Working Group of the APS Multidivisional Neutrino Study

Solar / Atmospheric Neutrino Experiments Working Group

arXiv:hep-ex/0412016v2 [hep-ex]

Show Abstract

Both the first evidence and the first discoveries of neutrino flavor transformation have come from experiments which use neutrino beams provided by Nature. These discoveries were remarkable not only because they were unexpected--they were discoveries in the purest sense--but that they were made initially by experiments whose primary goals were aimed at other physics. Future solar and atmospheric neutrino experiments will also be sensitive to a broad range of physics and thus to new and unexpected phenomena. We discuss here the physics which can be done by new solar and atmospheric neutrino experiments and what we believe to be the highest priorities for the next generation of detectors.

arXiv 2004-11-12

The Neutrino Factory and Beta Beam Experiments and Development

C. Albright, V. Barger, J. Beacom, S. Brice, J. J. Gomez-Cadenas, M. Goodman, D. Harris, P. Huber, A. Jansson, M. Lindner, O. Mena, P. Rapidis, K. Whisnant, W. Winter, The Neutrino Factory, Muon Collider Collaboration

arXiv:physics/0411123v2 [physics.acc-ph]

Show Abstract

The long-term prospects for fully exploring three-flavor mixing in the neutrino sector depend upon an ongoing and increased investment in the appropriate accelerator R&D. Two new concepts have been proposed that would revolutionize neutrino experiments, namely the Neutrino Factory and the Beta Beam facility. These new facilities would dramatically improve our ability to test the three-flavor mixing framework, measure \textsl{CP} violation in the lepton sector, and perhaps determine the neutrino mass hierarchy, and, if necessary, probe extremely small values of the mixing angle $θ_{13}$. The stunning sensitivity that could be achieved with a Neutrino Factory is described, together with our present understanding of the corresponding sensitivity that might be achieved with a Beta Beam facility. In the Beta Beam case, additional study is required to better understand the optimum Beta Beam energy, and the achievable sensitivity. Neither a Neutrino Factory nor a Beta Beam facility could be built without significant R&D. An impressive Neutrino Factory R&D effort has been ongoing in the U.S. and elsewhere over the last few years and significant progress has been made towards optimizing the design, developing and testing the required accelerator components, and significantly reducing the cost. The recent progress is described here.

arXiv 2009-01-11

UHE neutrino astronomy and neutrino oscillations

V. Berezinsky

Proc. 4th Int. Workshop "Neutrino Oscillations in Venice", ed. Milla Baldo Ceolin, p. 137 - 158, 2008

Show Abstract

UHE neutrinos with $E>10^{17}$ eV can be produced by ultra-high energy cosmic rays (UHECR) interacting with CMB photons (cosmogenic neutrinos) and by top-down sources, such as topological defects (TD), superheavy dark matter (SHDM) and mirror matter. Cosmogenic neutrinos are reliably predicted and their fluxes can be numerically evaluated using the observed flux of UHECR. The lower limit for the flux is obtained for the case of pure proton composition of the observed UHECR. The rigorous upper limit for cosmogenic neutrino flux also exists. The maximum neutrino energy is determined by maximum energy of acceleration, which at least for the shock acceleration is expected not to exceed $10^{21} - 10^{22}$ eV. The top-down sources provide neutrino energies a few orders of magnitude higher, and this can be considered as a signature of these models. Oscillations play important role in UHE neutrino astronomy. At production of cosmogenic neutrinos $τ$-neutrinos are absent and $\barν_e$ neutrinos are suppressed. These species, important for detection, appear in the observed fluxes due to oscillation. Mirror neutrinos cannot be observed directly, but due to oscillations to ordinary neutrinos they can provide the largest neutrino flux at the highest energies.

OpenAlex 1998-08-24
5081 citations

Evidence for Oscillation of Atmospheric Neutrinos

Y. Fukuda, T. Hayakawa, E. Ichihara, K. Inoue, K. Ishihara, H. Ishino, Y. Itow, T. Kajita, J. Kameda, S. Kasuga, Kazuyoshi Kobayashi, Yoshiyuki Kobayashi, Y. Koshio, M. Miura, M. Nakahata, S. Nakayama, Atsushi Okada, K. Okumura, N. Sakurai, M. Shiozawa, Y. Suzuki, Y. Takeuchi, Y. Totsuka, S. Yamada, M. Earl, A. Habig, E. Kearns, M. D. Messier, K. Scholberg, J. L. Stone, L. Sulak, C. W. Walter, M. Goldhaber, T. Barszczxak, D. Casper, W. Gajewski, P. G. Halverson, Jonathan Y. Hsu, W. R. Kropp, L. R. Price, F. Reines, M. Smy, H. W. Sobel, M. R. Vagins, K. S. Ganezer, W. E. Keig, R. W. Ellsworth, S. Tasaka, J. Flanagan, A. Kibayashi, J. G. Learned, S. Matsuno, V. J. Stenger, D. Takemori, T. Ishii, J. Kanzaki, T. Kobayashi, S. Mine, K. Nakamura, K. Nishikawa, Y. Oyama, Akito Sakai, M. Sakuda, O. Sasaki, S. Echigo, M. Kohama, Y. Suzuki, T. J. Haines, E. Blaufuss, B. K. Kim, R. Sanford, R. Svoboda, M. L. Chen, Z. Conner, J. A. Goodman, G. W. Sullivan, J. Hill, C. K. Jung, K. Martens, C. Mauger, C. McGrew, E. Sharkey, B. Viren, C. Yanagisawa, W. Doki, K. Miyano, H. Okazawa, C. Saji, M. Takahata, Y. Nagashima, M. Takita, Tomohiro Yamaguchi, M. Yoshida, S. B. Kim, Masato Eto, K. Fujita, T. Hasegawa, T. Hasegawa, S. Hatakeyama, T. Iwamoto

Physical Review Letters

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We present an analysis of atmospheric neutrino data from a 33.0 kton yr (535-day) exposure of the Super-Kamiokande detector. The data exhibit a zenith angle dependent deficit of muon neutrinos which is inconsistent with expectations based on calculations of the atmospheric neutrino flux. Experimental biases and uncertainties in the prediction of neutrino fluxes and cross sections are unable to explain our observation. The data are consistent, however, with two-flavor ${\ensuremath{\nu}}_{\ensuremath{\mu}}\ensuremath{\leftrightarrow}{\ensuremath{\nu}}_{\ensuremath{\tau}}$ oscillations with ${sin}^{2}2\ensuremath{\theta}&gt;0.82$ and $5\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}4}&lt;\ensuremath{\Delta}{m}^{2}&lt;6\ifmmode\times\else\texttimes\fi{}1{0}^{\ensuremath{-}3}\mathrm{eV}{}^{2}$ at 90% confidence level.

OpenAlex 2002-06-13
2996 citations

Direct Evidence for Neutrino Flavor Transformation from Neutral-Current Interactions in the Sudbury Neutrino Observatory

Rushdy Ahmad, R. C. Allen, Thomas Andersen, J. D. Anglin, J. C. Barton, E. W. Beier, M. Bercovitch, J. Bigu, S. D. Biller, R. A. Black, I. Blevis, R. J. Boardman, J. Boger, E. Bonvin, M. G. Boulay, M. G. Bowler, T. J. Bowles, S. J. Brice, M. C. Browne, T. V. Bullard, G. Bühler, J. Cameron, Y. D. Chan, H. H. Chen, M. Chen, X. Chen, B. T. Cleveland, E. T. H. Clifford, J. H. M. Cowan, D. F. Cowen, G. A. Cox, X. Dai, F. Dalnoki‐Veress, W.F. Davidson, P. J. Doe, G. Doucas, M. R. Dragowsky, C. A. Duba, F. A. Duncan, M. Dunford, J. Dunmore, E. D. Earle, S. R. Elliott, H. C. Evans, G. T. Ewan, J. Farine, H. Fergani, A. P. Ferraris, R. Ford, J. A. Formaggio, M. M. Fowler, K. C. Frame, E.D. Frank, W. Frati, N. Gagnon, J. V. Germani, Salvador Gil, K. Graham, D. R. Grant, R. L. Hahn, A. L. Hallin, E. D. Hallman, A. S. Hamer, A. A. Hamian, W. B. Handler, Rizwan Haq, C. K. Hargrove, P. J. Harvey, R. Hazama, K. M. Heeger, W. J. Heintzelman, J. Heise, R. L. Helmer, J. D. Hepburn, H. Heron, JoAnne L. Hewett, A. Hime, M. Howe, J. G. Hykawy, M. C. Perillo Isaac, P. Jagam, N.A. Jelley, C. Jillings, G. Jonkmans, K. Kazkaz, P. Keener, J. R. Klein, A. Knox, R. J. Komar, R. T. Kouzes, T. Kutter, Christopher C. M. Kyba, J. Law, I. Lawson, M. Lay, H. W. Lee, K. T. Lesko, J. R. Leslie, I. Levine, W. Locke

Physical Review Letters

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Observations of neutral-current $\ensuremath{\nu}$ interactions on deuterium in the Sudbury Neutrino Observatory are reported. Using the neutral current (NC), elastic scattering, and charged current reactions and assuming the standard ${}^{8}\mathrm{B}$ shape, the ${\ensuremath{\nu}}_{e}$ component of the ${}^{8}\mathrm{B}$ solar flux is ${\ensuremath{\varphi}}_{e}{\phantom{\rule{0ex}{0ex}}=\phantom{\rule{0ex}{0ex}}1.76}_{\ensuremath{-}0.05}^{+0.05}(\mathrm{stat}{)}_{\ensuremath{-}0.09}^{+0.09}(\mathrm{syst})\ifmmode\times\else\texttimes\fi{}{10}^{6}\phantom{\rule{0ex}{0ex}}{\mathrm{cm}}^{\ensuremath{-}2}{\mathrm{s}}^{\ensuremath{-}1}$ for a kinetic energy threshold of 5 MeV. The non- ${\ensuremath{\nu}}_{e}$ component is ${\ensuremath{\varphi}}_{\ensuremath{\mu}\ensuremath{\tau}}{\phantom{\rule{0ex}{0ex}}=\phantom{\rule{0ex}{0ex}}3.41}_{\ensuremath{-}0.45}^{+0.45}(\mathrm{stat}{)}_{\ensuremath{-}0.45}^{+0.48}(\mathrm{syst})\ifmmode\times\else\texttimes\fi{}{10}^{6}\phantom{\rule{0ex}{0ex}}{\mathrm{cm}}^{\ensuremath{-}2}{\mathrm{s}}^{\ensuremath{-}1}$, $5.3\ensuremath{\sigma}$ greater than zero, providing strong evidence for solar ${\ensuremath{\nu}}_{e}$ flavor transformation. The total flux measured with the NC reaction is ${\ensuremath{\varphi}}_{\mathrm{NC}}{\phantom{\rule{0ex}{0ex}}=\phantom{\rule{0ex}{0ex}}5.09}_{\ensuremath{-}0.43}^{+0.44}(\mathrm{stat}{)}_{\ensuremath{-}0.43}^{+0.46}(\mathrm{syst})\ifmmode\times\else\texttimes\fi{}{10}^{6}\phantom{\rule{0ex}{0ex}}{\mathrm{cm}}^{\ensuremath{-}2}{\mathrm{s}}^{\ensuremath{-}1}$, consistent with solar models.

OpenAlex 2013-11-21
1620 citations

Evidence for High-Energy Extraterrestrial Neutrinos at the IceCube Detector

IceCube Collaboration

Science

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We report on results of an all-sky search for high-energy neutrino events interacting within the IceCube neutrino detector conducted between May 2010 and May 2012. The search follows up on the previous detection of two PeV neutrino events, with improved sensitivity and extended energy coverage down to about 30 TeV. Twenty-six additional events were observed, substantially more than expected from atmospheric backgrounds. Combined, both searches reject a purely atmospheric origin for the 28 events at the 4σ level. These 28 events, which include the highest energy neutrinos ever observed, have flavors, directions, and energies inconsistent with those expected from the atmospheric muon and neutrino backgrounds. These properties are, however, consistent with generic predictions for an additional component of extraterrestrial origin.