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1

Double Beta Decay and Majorana Neutrino  

Microsoft Academic Search

This review consists of three parts: Various properties of the quantized neutrino fields are summarized in part I from the viewpoint that a Dirac neutrino consists of two Majorana neutrinos with a degenerate mass but with opposite CP sings. It is shown why the Dirac neutrino has a freedom of the phase transformation to guarantee the lepton number conservation, while

Masaru Doi; Tsuneyuki Kotani; Eiichi Takasugi

1985-01-01

2

Neutrinos  

E-print Network

In these lectures the following topics are considered: historical remarks and general properties, Dirac and Majorana neutrino masses, effective lagrangian approach, the seesaw mechanism, the number of active left-hauded neutrino species, the light neutrino mass matrix, the direct measurement of neutrino masses, double beta decay, neutrino oscillations in vacuum and neutrino oscillations in matter.

J. Bernabeu

2000-12-22

3

Search for Majorana neutrinos in B- ? ?+ ?- ?- decays.  

PubMed

A search for heavy Majorana neutrinos produced in the B- ? ?+ ?- ?- decay mode is performed using 3??fb(-1) of integrated luminosity collected with the LHCb detector in pp collisions at center-of-mass energies of 7 and 8 TeV at the LHC. Neutrinos with masses in the range 250 to 5000 MeV and lifetimes from zero to 1000 ps are probed. In the absence of a signal, upper limits are set on the branching fraction B(B- ? ?+ ?- ?-) as functions of neutrino mass and lifetime. These limits are on the order of 10(-9) for short neutrino lifetimes of 1 ps or less. Limits are also set on the coupling between the muon and a possible fourth-generation neutrino. PMID:24745405

Aaij, R; Adeva, B; Adinolfi, M; Affolder, A; Ajaltouni, Z; Albrecht, J; Alessio, F; Alexander, M; Ali, S; Alkhazov, G; Alvarez Cartelle, P; Alves, A A; Amato, S; Amerio, S; Amhis, Y; Anderlini, L; Anderson, J; Andreassen, R; Andreotti, M; Andrews, J E; Appleby, R B; Aquines Gutierrez, O; Archilli, F; Artamonov, A; Artuso, M; Aslanides, E; Auriemma, G; Baalouch, M; Bachmann, S; Back, J J; Badalov, A; Balagura, V; Baldini, W; Barlow, R J; Barschel, C; Barsuk, S; Barter, W; Batozskaya, V; Bauer, T; Bay, A; Beddow, J; Bedeschi, F; Bediaga, I; Belogurov, S; Belous, K; Belyaev, I; Ben-Haim, E; Bencivenni, G; Benson, S; Benton, J; Berezhnoy, A; Bernet, R; Bettler, M-O; van Beuzekom, M; Bien, A; Bifani, S; Bird, T; Bizzeti, A; Bjørnstad, P M; Blake, T; Blanc, F; Blouw, J; Blusk, S; Bocci, V; Bondar, A; Bondar, N; Bonivento, W; Borghi, S; Borgia, A; Borsato, M; Bowcock, T J V; Bowen, E; Bozzi, C; Brambach, T; van den Brand, J; Bressieux, J; Brett, D; Britsch, M; Britton, T; Brook, N H; Brown, H; Bursche, A; Busetto, G; Buytaert, J; Cadeddu, S; Calabrese, R; Callot, O; Calvi, M; Calvo Gomez, M; Camboni, A; Campana, P; Campora Perez, D; Carbone, A; Carboni, G; Cardinale, R; Cardini, A; Carranza-Mejia, H; Carson, L; Carvalho Akiba, K; Casse, G; Castillo Garcia, L; Cattaneo, M; Cauet, C; Cenci, R; Charles, M; Charpentier, P; Cheung, S-F; Chiapolini, N; Chrzaszcz, M; Ciba, K; Cid Vidal, X; Ciezarek, G; Clarke, P E L; Clemencic, M; Cliff, H V; Closier, J; Coca, C; Coco, V; Cogan, J; Cogneras, E; Collins, P; Comerma-Montells, A; Contu, A; Cook, A; Coombes, M; Coquereau, S; Corti, G; Counts, I; Couturier, B; Cowan, G A; Craik, D C; Cruz Torres, M; Cunliffe, S; Currie, R; D'Ambrosio, C; Dalseno, J; David, P; David, P N Y; Davis, A; De Bonis, I; De Bruyn, K; De Capua, S; De Cian, M; De Miranda, J M; De Paula, L; De Silva, W; De Simone, P; Decamp, D; Deckenhoff, M; Del Buono, L; Déléage, N; Derkach, D; Deschamps, O; Dettori, F; Di Canto, A; Dijkstra, H; Donleavy, S; Dordei, F; Dorigo, M; Dorosz, P; Dosil Suárez, A; Dossett, D; Dovbnya, A; Dupertuis, F; Durante, P; Dzhelyadin, R; Dziurda, A; Dzyuba, A; Easo, S; Egede, U; Egorychev, V; Eidelman, S; Eisenhardt, S; Eitschberger, U; Ekelhof, R; Eklund, L; El Rifai, I; Elsasser, C; Falabella, A; Färber, C; Farinelli, C; Farry, S; Ferguson, D; Fernandez Albor, V; Ferreira Rodrigues, F; Ferro-Luzzi, M; Filippov, S; Fiore, M; Fiorini, M; Fitzpatrick, C; Fontana, M; Fontanelli, F; Forty, R; Francisco, O; Frank, M; Frei, C; Frosini, M; Furfaro, E; Gallas Torreira, A; Galli, D; Gandelman, M; Gandini, P; Gao, Y; Garofoli, J; Garra Tico, J; Garrido, L; Gaspar, C; Gauld, R; Gersabeck, E; Gersabeck, M; Gershon, T; Ghez, P; Gianelle, A; Gibson, V; Giubega, L; Gligorov, V V; Göbel, C; Golubkov, D; Golutvin, A; Gomes, A; Gordon, H; Grabalosa Gándara, M; Graciani Diaz, R; Granado Cardoso, L A; Graugés, E; Graziani, G; Grecu, A; Greening, E; Gregson, S; Griffith, P; Grillo, L; Grünberg, O; Gui, B; Gushchin, E; Guz, Y; Gys, T; Hadjivasiliou, C; Haefeli, G; Haen, C; Hafkenscheid, T W; Haines, S C; Hall, S; Hamilton, B; Hampson, T; Hansmann-Menzemer, S; Harnew, N; Harnew, S T; Harrison, J; Hartmann, T; He, J; Head, T; Heijne, V; Hennessy, K; Henrard, P; Hernando Morata, J A; van Herwijnen, E; Heß, M; Hicheur, A; Hill, D; Hoballah, M; Hombach, C; Hulsbergen, W; Hunt, P; Huse, T; Hussain, N; Hutchcroft, D; Hynds, D; Iakovenko, V; Idzik, M; Ilten, P; Jacobsson, R; Jaeger, A; Jans, E; Jaton, P; Jawahery, A; Jing, F; John, M; Johnson, D; Jones, C R; Joram, C; Jost, B; Jurik, N; Kaballo, M; Kandybei, S; Kanso, W; Karacson, M; Karbach, T M; Kenyon, I R; Ketel, T; Khanji, B; Khurewathanakul, C; Klaver, S; Kochebina, O; Komarov, I; Koopman, R F; Koppenburg, P; Korolev, M; Kozlinskiy, A; Kravchuk, L; Kreplin, K; Kreps, M; Krocker, G; Krokovny, P; Kruse, F; Kucharczyk, M; Kudryavtsev, V; Kurek, K; Kvaratskheliya, T; La Thi, V N; Lacarrere, D; Lafferty, G; Lai, A; Lambert, D; Lambert, R W; Lanciotti, E; Lanfranchi, G; Langenbruch, C; Latham, T; Lazzeroni, C; Le Gac, R; van Leerdam, J; Lees, J-P; Lefèvre, R; Leflat, A; Lefrançois, J; Leo, S; Leroy, O; Lesiak, T; Leverington, B; Li, Y; Liles, M; Lindner, R; Linn, C; Lionetto, F; Liu, B; Liu, G; Lohn, S; Longstaff, I; Lopes, J H; Lopez-March, N; Lowdon, P; Lu, H; Lucchesi, D; Luisier, J; Luo, H; Luppi, E; Lupton, O; Machefert, F; Machikhiliyan, I V; Maciuc, F; Maev, O; Malde, S; Manca, G; Mancinelli, G; Manzali, M; Maratas, J; Marconi, U; Marino, P; Märki, R; Marks, J; Martellotti, G; Martens, A; Martín Sánchez, A; Martinelli, M; Martinez Santos, D; Martins Tostes, D; Massafferri, A; Matev, R; Mathe, Z; Matteuzzi, C; Mazurov, A; McCann, M; McCarthy, J; McNab, A; McNulty, R; McSkelly, B; Meadows, B; Meier, F; Meissner, M; Merk, M; Milanes, D A; Minard, M-N; Molina Rodriguez, J; Monteil, S; Moran, D; Morandin, M

2014-04-01

4

Can neutrino-electron scattering tell us whether neutrinos are Dirac or Majorana particles  

SciTech Connect

There has recently been interest in the possibility that neutrino-electron scattering experiments could determine whether neutrinos are Dirac or Majorana particles by providing information on their electromagnetic structure. We try to explain why studies of neutrino electromagnetic structure actually cannot distinguish between Dirac and Majorana neutrinos. 9 refs.

Kayser, B.

1988-04-01

5

Majorana neutrinos, neutrino mass spectrum, CP violation, and neutrinoless double ? decay. II. Mixing of four neutrinos  

NASA Astrophysics Data System (ADS)

Assuming four-neutrino mixing and massive Majorana neutrinos, we study the implications of neutrino oscillation solutions of the solar and atmospheric neutrino problems, of the results of the Liquid Scintillation Neutrino Detector (LSND) experiment and of the constraints on neutrino oscillations, obtained in reactor and accelerator experiments, for the predictions of the effective Majorana mass in neutrinoless double beta ((??)0?-) decay, \\|\\|. All four-neutrino mass spectra compatible with the existing neutrino mass and oscillation data are considered: 2+2A,B and 3+1A,B,C. The general case of CP nonconservation is investigated. The predicted values of \\|\\| depend strongly on the value of the lightest neutrino mass m1, on the type of the neutrino mass spectrum, on the LSND neutrino mass-squared difference ?m2SBL, on the solution of the solar neutrino problem, as well as on the values of the three Majorana CP-violating phases, present in the lepton mixing matrix. If CP invariance holds, \\|\\| is very sensitive to the values of the relative CP parities of the massive Majorana neutrinos. We also analyze in detail the question of whether a measurement of \\|\\|>~0.01 eV in the next generation of (??)0?-decay experiments (NEMO3, CUORE, EXO, and GENIUS), combined with the data from the solar, atmospheric, reactor and accelerator neutrino oscillation experiments and from the future neutrino mass 3H ?-decay experiment KATRIN would allow us, and under what conditions, (i) to determine the absolute values of the neutrino masses and thus the neutrino mass spectrum, and (ii) to establish the existence of CP violation in the lepton sector. We have pointed out, in particular, that the 2+2A and 3+1A spectra can be critically tested by the KATRIN experiment. The latter, in particular, can provide information on the value of the lightest neutrino mass m1 in the cases of the spectra 2+2A, 3+1A, 3+1B, and 3+1C. For these neutrino mass spectra there exists a direct relation between \\|\\| or m1 and the neutrino mass measured in 3H ? decay, m?e, and the measurement of \\|\\|>~0.01 eV and of m?e>~0.4 eV will provide the unique possibility to determine the absolute values of all four neutrino masses and to obtain information on CP violation in the lepton sector.

Bilenky, S. M.; Pascoli, S.; Petcov, S. T.

2001-12-01

6

Geometry of Majorana neutrino and new symmetries  

E-print Network

Experimental observation of Majorana fermion matter gives a new impetus to the understanding of the Lorentz symmetry and its extension, the geometrical properties of the ambient space-time structure, matter--antimatter symmetry and some new ways to understand the baryo-genesis problem in cosmology. Based on the primordial Majorana fermion matter assumption, we discuss a possibility to solve the baryo-genesis problem through the the Majorana-Diraco genesis in which we have a chance to understand creation of Q(em) charge and its conservation in our D=1+3 Universe after the Big Bang. In the Majorana-Diraco genesis approach there appears a possibility to check the proton and electron non-stability on the very low energy scale. In particle physics and in our space-time geometry, the Majorana nature of the neutrino can be related to new types of symmetries which are lying beyond the binary Cartan-Killing-Lie algebras/superalgebras. This can just support a conjecture about the non-completeness of the SM in terms of binary Cartan--Killing--Lie symmetries/supersymmetries. As one of the very important applications of such new ternary symmetries could be related with explanation of the nature of the three families and three colour symmetry. The Majorana neutrino can directly indicate the existence of a new extra-dimensional geometry and thanks to new ternary space-time symmetries, could lead at high energies to the unextraordinary phenomenological consequences.

G. G. Volkov

2006-07-30

7

Selected Topics in Majorana Neutrino Physics  

E-print Network

Starting from the original Majorana's article of 1937, the see-saw mechanism is illustrated, first for one and later for three neutrino generations, and neutrinoless double beta decay is considered. Neutrino mixing and oscillations in three flavors are described. The Yukawa couplings to the Higgs field of quarks and leptons are considered, their transformation properties under the corresponding flavor groups are spelled out and the principle of Minimal Flavor Violation is illustrated, in connection with possible new physics beyond the Standard Theory. The idea that the Yukawa couplings may be the vacuum expectation value of some new fields is introduced and natural extrema of potentials which are invariant under quark and lepton flavor groups are characterized. A recent result indicating large mixing of almost degenerate neutrinos is derived from the heavy lepton invariance under flavor ${\\cal O}(3)$.

Luciano Maiani

2014-08-06

8

Scattering processes could distinguish Majorana from Dirac neutrinos  

NASA Astrophysics Data System (ADS)

It is well known that Majorana neutrinos have a pure axial neutral current interaction while Dirac neutrinos have the standard vector-axial interaction. In spite of this crucial difference, usually Dirac neutrino processes differ from Majorana processes by a term proportional to the neutrino mass, resulting in almost unmeasurable observations of this difference. In the present work we show that once the neutrino polarization evolution is considered, there are clear differences between Dirac and Majorana scattering on electrons. The change of polarization can be achieved in astrophysical environments with strong magnetic fields. Furthermore, we show that in the case of unpolarized neutrino scattering onto polarized electrons, this difference can be relevant even for large values of the neutrino energy.

Barranco, J.; Delepine, D.; Gonzalez-Macias, V.; Lujan-Peschard, C.; Napsuciale, M.

2014-12-01

9

Can Gravity Distinguish between Dirac and Majorana Neutrinos?  

SciTech Connect

We show that spin-gravity interaction can distinguish between Dirac and Majorana neutrino wave packets propagating in a Lense-Thirring background. Using time-independent perturbation theory and the gravitational phase to generate a perturbation Hamiltonian with spin-gravity coupling, we show that the associated matrix element for the Majorana neutrino differs significantly from its Dirac counterpart. This difference can be demonstrated through significant gravitational corrections to the neutrino oscillation length for a two-flavor system, as shown explicitly for SN 1987A.

Singh, Dinesh; Mobed, Nader [Department of Physics, University of Regina, Regina, Saskatchewan, S4S 0A2 (Canada); Papini, Giorgio [Department of Physics, University of Regina, Regina, Saskatchewan, S4S 0A2 (Canada); Prairie Particle Physics Institute, Regina, Saskatchewan, S4S 0A2 (Canada); International Institute for Advanced Scientific Studies, 89019 Vietri sul Mare (Saudi Arabia) (Italy)

2006-07-28

10

Can gravity distinguish between Dirac and Majorana neutrinos?  

PubMed

We show that spin-gravity interaction can distinguish between Dirac and Majorana neutrino wave packets propagating in a Lense-Thirring background. Using time-independent perturbation theory and the gravitational phase to generate a perturbation Hamiltonian with spin-gravity coupling, we show that the associated matrix element for the Majorana neutrino differs significantly from its Dirac counterpart. This difference can be demonstrated through significant gravitational corrections to the neutrino oscillation length for a two-flavor system, as shown explicitly for SN 1987A. PMID:16907562

Singh, Dinesh; Mobed, Nader; Papini, Giorgio

2006-07-28

11

New Stringy Instanton Effects And Neutrino Majorana Masses  

SciTech Connect

D-brane instantons can generate open string couplings in the superpotential which violate global abelian symmetries and are therefore perturbatively forbidden. After discussing the main ingredients, focussing for concretenes on Type IIA orientifold compactifications, we exemplify the computation of instanton-induced Majorana mass terms for right-handed neutrinos in a local SU(5) GUT-like model. In particular, we show that the instanton allows for naturally engineering the intermediate scale of the Majorana masses, thereby realizing the seesaw mechanism for neutrinos.

Cvetic, M.; Richter, R.; Weigand, T. [Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104-6396 (United States)

2007-10-03

12

General Majorana Neutrino Mass Matrix from a Low Energy SU(3) Family Symmetry with Sterile Neutrinos  

E-print Network

Within the framework of a local SU(3) family symmetry model, we report a general analysis of the mechanism for neutrino mass generation and mixing, including light sterile neutrinos. In this scenario, ordinary heavy fermions, top and bottom quarks and tau lepton, become massive at tree level from Dirac See-saw mechanisms implemented by the introduction of a new set of $SU(2)_L$ weak singlet vector-like fermions, U,D,E,N, with N a sterile neutrino. Right-handed and the $N_{L,R}$ sterile neutrinos allow the implementation of a 8x8 general Majorana neutrino mass matrix with four or five massless neutrinos at tree level. Hence, light fermions, including light neutrinos get masses from radiative corrections mediated by the massive SU(3) gauge bosons. We report the corresponding Majorana neutrino mass matrix up to one loop. Previous numerical analysis of the free parameters show out solutions for quarks and charged lepton masses within a parameter space region where the vector-like fermion masses $M_U, M_D, M_E$, a...

Hernandez-Galeana, Albino

2014-01-01

13

See-saw Mechanisms for Dirac and Majorana Neutrino Masses  

E-print Network

We investigate the see-saw mechanism for generally non-fine-tuned $n \\times n$ mass matrices involving both Dirac and Majorana neutrinos. We specifically show that the number of naturally light neutrinos cannot exceed half of the dimension of the considered mass matrix. Furthermore, we determine a criterion for mass matrix textures leading to light Dirac neutrinos with the see-saw mechanism. Especially, we study $4 \\times 4$ and $6 \\times 6$ mass matrix textures and give some examples in order to highlight these types of textures. Next, we present a model scheme based on non-Abelian and discrete symmetries fulfilling the above mentioned criterion for light Dirac neutrinos. Finally, we investigate the connection between symmetries and the invariants of a mass matrix on a formal level.

Manfred Lindner; Tommy Ohlsson; Gerhart Seidl

2001-09-27

14

Neutrinos  

PubMed Central

Neutrinos represent a new “window” to the Universe, spanning a large range of energy. We discuss the science of neutrino astrophysics and focus on two energy regimes. At “lower” energies (?1 MeV), studies of neutrinos born inside the sun, or produced in interactions of cosmic rays with the atmosphere, have allowed the first incontrovertible evidence that neutrinos have mass. At energies typically one thousand to one million times higher, sources further than the sun (both within the Milky Way and beyond) are expected to produce a flux of particles that can be detected only through neutrinos. PMID:10588680

Besson, Dave; Cowen, Doug; Selen, Mats; Wiebusch, Christopher

1999-01-01

15

Apparent Lorentz violation with superluminal Majorana neutrinos at OPERA?  

E-print Network

From the data release of OPERA - CNGS experiment, and publicly announced on 23 September 2011, we cast a phenomenological model based on a Majorana neutrino state carrying a fictitious imaginary mass term, already discussed by Majorana in 1932. This mass term can be induced by the interaction with the matter of the Earth's crust during the 735 Km travel. Within the experimental errors, we prove that the model fits with OPERA, MINOS and supernova SN1987a data. Possible violations to Lorentz invariance due to quantum gravity effects have been considered.

F. Tamburini; M. Laveder

2011-09-26

16

Ettore Majorana centennial and neutrino legacy  

NASA Astrophysics Data System (ADS)

"In the world there are various categories of scientists: people of secondary or tertiary standing, who do their best but do not go very far. There are also those of high standing, who come to discoveries of great importance. But then there are geniuses like Galileo and Newton. Well, Ettore was one of them. Majorana had what no one else in the world has...". In this talk we try to put some light on this quite unusual statement by Enrico Fermi about Ettore Majorana, by exploring mainly personal notes left unpublished by the great sicilian physicist. Some emphasis is given on recent achievements about Majorana as a research scientist as well as a teacher in Theoretical Physics.

Esposito, Salvatore

2007-06-01

17

Neutrino physics  

Microsoft Academic Search

In the present lectures the following topics are considered: general properties of neutrinos, neutrino mass phenomenology (Dirac and Majorana masses), neutrino masses in the simplest extensions of the standard model (including the seesaw mech- anism), neutrino oscillations in vacuum, neutrino oscillations in matter (the MSW effect) in 2- and 3-flavour schemes, implications of CP, T and CPT symmetries for neutrino

E. Kh

18

The see-saw mechanism and heavy Majorana neutrino masses in an SO(10) model  

E-print Network

We apply the see-saw mechanism and an SO(10) model to neutrino masses and mixing in order to estimate the heavy Majorana masses. We discuss shortly the decay modes of heavy Majorana neutrinos and calculate their contribution to the lepton number violating processes \\mu\\to e\\gamma, \\tau\\to\\mu\\gamma and \\tau\\to e\\gamma.

W. Alles; L. Frassinetti

2000-08-09

19

Oscillations of Dirac and Majorana neutrinos in matter and a magnetic field  

SciTech Connect

We study the evolution of massive mixed Dirac and Majorana neutrinos in matter under the influence of a transversal magnetic field. The analysis is based on relativistic quantum mechanics. We solve exactly the evolution equation for relativistic neutrinos, find the neutrino wave functions, and calculate the transition probability for spin-flavor oscillations. We analyze the dependence of the transition probability on the external fields and compare the cases of Dirac and Majorana neutrinos. The evolution of Majorana particles in vacuum is also studied and correction terms to the standard oscillation formula are derived and discussed. As a possible application of our results we discuss the spin-flavor transitions in supernovae.

Dvornikov, Maxim [Department of Physics, P.O. Box 35, FIN-40014 University of Jyvaeskylae (Finland); Departamento de Fisica y Centro de Estudios Subatomicos, Universidad Tecnica Federico Santa Maria, Casilla 110-V, Valparaiso (Chile); IZMIRAN, 142190, Troitsk, Moscow Region (Russian Federation); Maalampi, Jukka [Department of Physics, P.O. Box 35, FIN-40014 University of Jyvaeskylae (Finland); Helsinki Institute of Physics, P.O. Box 64, FIN-00014 University of Helsinki (Finland)

2009-06-01

20

Majorana phases, CP violation, sterile neutrinos and neutrinoless double-beta decay  

SciTech Connect

CP violation plays a crucial role in the generation of the baryon asymmetry in the Universe. Within this context we investigate the possibility of CP violation in the lepton sector caused by Majorana neutrino mixing. Focus is put on the model including 1 sterile neutrino. Both cases of normal and inverted neutrino mass spectrum are considered. We address the question whether the Majorana phases can be measured in the neutrinoless double-beta decay experiments with sensitivity to the effective Majorana neutrino mass of the order of 10{sup ?2} eV.

Babi?, Andrej [Department of Nuclear Physics and Biophysics, Faculty of Mathematics, Physics and Informatics, Comenius University, Mlynská dolina, 842 48 Bratislava (Slovakia); Šimkovic, Fedor [Bogoliubov Laboratory of Theoretical Physics, JINR, Joliot-Curie 6, 141980 Dubna, Moscow region, Russia and Institute of Experimental and Applied Physics, Czech Technical University, CZ-128 00 Prague (Czech Republic)

2013-12-30

21

Massive neutrinos and neutrino oscillations  

Microsoft Academic Search

The theory of neutrino mixing and neutrino oscillations, as well as the properties of massive neutrinos (Dirac and Majorana), are reviewed. More specifically, the following topics are discussed in detail: (i) the possible types of neutrino mass terms; (ii) oscillations of neutrinos (iii) the implications of CP invariance for the mixing and oscillations of neutrinos in vacuum; (iv) possible varieties

S. M. Bilenky; S. T. Petcov

1987-01-01

22

Neutrinos  

NASA Astrophysics Data System (ADS)

Neutrinos are electrically neutral ELEMENTARY PARTICLES which experience only the weak nuclear force and gravity. Their existence was introduced as a hypothesis by Wolfgang Pauli in 1930 to explain the apparent violation of energy conservation in radioactive beta decay. Chadwick had discovered in 1914 that the energy spectrum of electrons emitted in beta decay was not monoenergetic but continuous...

Winter, K.; Murdin, P.

2000-11-01

23

Search for Majorana Neutrinos in B[superscript ?] ? ?[superscript +]?[superscript ?]?[superscript ?] Decays  

E-print Network

A search for heavy Majorana neutrinos produced in the B[superscript ?] ? ?[superscript +]?[superscript ?]?[superscript ?] decay mode is performed using 3??fb[superscript ?1] of integrated luminosity collected with the LHCb ...

Counts, Ian Thomas Hunt

24

Arbitrary mass Majorana neutrinos in neutrinoless double beta decay  

NASA Astrophysics Data System (ADS)

We revisit the mechanism of neutrinoless double beta (0 ? ? ? ) decay mediated by the exchange with the heavy Majorana neutrino N of arbitrary mass mN , slightly mixed ˜UeN with the electron neutrino ?e . By assuming the dominance of this mechanism, we update the well-known 0 ? ? ? -decay exclusion plot in the mN-UeN plane taking into account recent progress in the calculation of nuclear matrix elements within quasiparticle random phase approximation and improved experimental bounds on the 0 ? ? ? -decay half-life of Ge 76 and Xe 136 . We also consider the known formula approximating the mN dependence of the 0 ? ? ? -decay nuclear matrix element in a simple explicit form. We analyze its accuracy and specify the corresponding parameters, allowing one to easily calculate the 0 ? ? ? -decay half-life for arbitrary mN for all the experimentally interesting isotopes without resorting to real nuclear structure calculations.

Faessler, Amand; González, Marcela; Kovalenko, Sergey; Šimkovic, Fedor

2014-11-01

25

Determining Majorana nature of neutrino from nucleon decays and n -n ¯ oscillations  

NASA Astrophysics Data System (ADS)

We show that the discovery of baryon number violation in two processes, with at least one obeying the selection rule ? (B -L )=±2 , can determine the Majorana character of neutrinos. Thus, observing p ?e+?0 and n ?e-?+ decays, or p ?e+?0 and n -n ¯ oscillations, or n ?e-?+ and n -n ¯ oscillations would establish that neutrinos are Majorana particles. We discuss this in a model-independent effective operator approach.

Babu, K. S.; Mohapatra, Rabindra N.

2015-01-01

26

The search for Majorana neutrinos with neutrinoless double beta decays: From CUORICINO to LUCIFER experiment  

SciTech Connect

The study of neutrino properties is one of the fundamental challenges in particle physics nowadays. Fifty years of investigations established that neutrinos are massive but the absolute mass scale has not yet been measured. Moreover its true nature is still unknown. Is the neutrino its own antiparticle (thus violating the lepton number) as proposed by Majorana in 1937? The only way to probe the neutrino nature is through the observation of Neutrinoless Double Beta Decay (0{nu}{beta}{beta}), a very rare spontaneous nuclear transition which emits two electrons and no neutrinos. In this paper, after a brief introduction to the theoretical framework of Majorana's neutrino, a presentation of experimental challenges posed by 0{nu}{beta}{beta} search will be given as well as an overview of present status and future perpectives of experiments.

Bellini, F. [Dipartimento di Fisica, Sapienza Universita di Roma, Roma I-00185 (Italy) and INFN - Sezione di Roma, Roma I-00185 (Italy)

2012-11-20

27

Heidelberg - Moscow Experiment. First Evidence for Lepton Number Violation and the Majorana Character of Neutrinos  

Microsoft Academic Search

Nuclear double beta decay provides an extraordinarily broad potential to search for beyond-standard-model physics. The occurrence of the neutrinoless decay (0 ) mode has fundamental consequences: rst total lepton number is not con- served, and second, the neutrino is a Majorana particle. Further the eectiv e mass measured allows to put an absolute scale of the neutrino mass spectrum. In

H. V. Klapdor-Kleingrothausa

28

Magnetic moment of the majorana neutrino in the left-right symmetric model  

SciTech Connect

Corrections to the neutrino magnetic dipole moment from the singly charged Higgs bosons h{sup ({+-})} and {delta}-tilde{sup (}{+-}) were calculated within the left-right symmetric model involving Majorana neutrinos. It is shown that, if the h{sup ({+-})} and {delta}-tilde{sup (}{+-}) bosons lie at the electroweak scale, the contributions from Higgs sector are commensurate with the contribution of charged gauge bosons or may even exceed it. The behavior of the neutrino flux inmatter and in amagnetic field was studied. It was found that resonance transitions between light and heavy neutrinos are forbidden.

Boyarkin, O. M., E-mail: oboyarkin@tut.by; Boyarkina, G. G. [Maxim Tank Belarusian State Pedagogical University (Belarus)] [Maxim Tank Belarusian State Pedagogical University (Belarus)

2013-04-15

29

The quest for neutrinoless double beta decay: Pseudo-Dirac, Majorana, and sterile neutrinos  

NASA Astrophysics Data System (ADS)

In this paper we analyze the neutrinoless double beta decay predictions in some scenarios with admixture of pseudo-Dirac and Majorana neutrinos in the 3 and 3+1 neutrino frameworks. We found that some of the cases can be falsifiable in near-term and future generation of neutrinoless double beta decay experiments even for the normal neutrino mass hierarchy. In the 3+1 framework we consider the sterile neutrino with a mass of the order of 1 eV. The complementarity between cosmological constraints and the future sensitivity for the next generations of the neutrinoless double beta decay searches is exploited.

Meroni, A.; Peinado, E.

2014-09-01

30

Geometry of the effective Majorana neutrino mass in the 0??? decay  

NASA Astrophysics Data System (ADS)

The neutrinoless double-beta (0???) decay is a unique process used to identify the Majorana nature of massive neutrinos, and its rate depends on the size of the effective Majorana neutrino mass ee. We put forward a novel ‘coupling-rod’ diagram to describe ee in the complex plane, by which the effects of the neutrino mass ordering and CP-violating phases on ee are intuitively understood. We show that this geometric language allows us to easily obtain the maximum and minimum of |ee|. It remains usable even if there is a kind of new physics contributing to ee, and it can also be extended to describe the effective Majorana masses e?, e?, ?? and ?? which may appear in some other lepton-number violating processes.

Xing, Zhi-zhong; Zhou, Ye-Ling

2015-01-01

31

Large electron electric dipole moment in minimal flavor violation framework with Majorana neutrinos  

NASA Astrophysics Data System (ADS)

The latest data from the ACME Collaboration have put a stringent constraint on the electric dipole moment de of the electron. Nevertheless, the standard model (SM) prediction for de is many orders of magnitude below the new result, making this observable a powerful probe for physics beyond the SM. We carry out a model-independent study of de in the SM with right-handed neutrinos and its extension with the neutrino seesaw mechanism under the framework of minimal flavor violation. We find that de crucially depends on whether neutrinos are Dirac or Majorana particles. In the Majorana case, de can reach its experimental bound, and it constrains the scale of minimal flavor violation to be above a few hundred GeV or more. We also explore extra CP-violating sources in the Yukawa couplings of the right-handed neutrinos. Such new sources can have important effects on de.

He, Xiao-Gang; Lee, Chao-Jung; Li, Siao-Fong; Tandean, Jusak

2014-05-01

32

Electric dipole moments of leptons in the presence of Majorana neutrinos  

Microsoft Academic Search

We calculate the two-loop diagrams that give a nonzero contribution to the electric dipole moment dl of a charged lepton l due to possible Majorana masses of neutrinos. Using the example with one generation of the standard model leptons and two heavy right-handed neutrinos, we demonstrate that the nonvanishing result for dl first appears in order O(mlm2nuG2F), where mnu is

John Paul Archambault; Andrzej Czarnecki; Maxim Pospelov

2004-01-01

33

Distinguishing between Dirac and Majorana neutrinos with two-particle interferometry.  

PubMed

Two-particle interferometry, a second-order interference effect, is explored as another possible tool to distinguish between massive Dirac and Majorana neutrinos. A simple theoretical framework is discussed in the context of several gedanken experiments. The method can in principle provide both the mass scale and the quantum nature of the neutrino for a certain class of incoherent left-handed source currents. PMID:16605897

Gutierrez, Thomas D

2006-03-31

34

Determining Majorana Nature of Neutrino from Nucleon Decays and n-nbar oscillations  

E-print Network

We show that discovery of baryon number violation in two processes with at least one obeying the selection rule \\Delta (B-L) = \\pm 2 can determine the Majorana character of neutrinos. Thus observing p \\to e^+ \\pi^0 and n \\to e^- \\pi^0 decays, or p \\to e^+ \\pi^0 and n-nbar oscillations, or n \\to e^- \\pi^+ and n-nbar oscillations would establish that neutrinos are Majorana particles. We discuss this in a model-independent effective operator approach.

K. S. Babu; Rabindra N. Mohapatra

2014-08-04

35

Neutrino Physics  

E-print Network

These lectures describe some aspects of the physics of massive neutrinos. After a brief introduction of neutrinos in the Standard Model, I discuss possible patterns for their masses. In particular, I show how the presence of a large Majorana mass term for the right-handed neutrinos can engender tiny neutrino masses for the observed neutrinos. If neutrinos have mass, different flavors of neutrinos can oscillate into one another. To analyze this phenomena, I develop the relevant formalism for neutrino oscillations, both in vacuum and in matter. After reviewing the existing (negative) evidence for neutrino masses coming from direct searches, I discuss evidence for, and hints of, neutrino oscillations in the atmosphere, the sun, and at accelerators. Some of the theoretical implications of these results are emphasized. I close these lectures by briefly outlining future experiments which will shed further light on atmospheric, accelerator and solar neutrino oscillations. A pedagogical discussion of Dirac and Majora...

Peccei, Roberto D

1999-01-01

36

Back-to-back pair correlation of Majorana neutrinos with transit magnetic moments  

SciTech Connect

The pair production of Majorana neutrinos with transit magnetic moments from the annihilation of charged particles in colliding experiments is discussed using the Pauli interaction, through which the neutral neutrinos with magnetic moments can be probed by the photon. The pair of neutrinos with different flavors are produced due to the transit magnetic moment coupling. We discuss the correlations of flavors in pairs produced back-to-back in the center of the mass frame, where the angular distribution peaks at {theta}={pi}/2 with respect to the beam direction. We demonstrate that the flavor mixing angle can be inferred by measuring the flavor correlation in pairs.

Lee, Hyun Kyu [Department of Physics, Hanyang University, Seoul 133-791, Korea and Asia Pacific Center for Theoretical Physics, Pohang 790-784 (Korea, Republic of)

2011-10-01

37

Phenomenology of neutrino oscillations  

Microsoft Academic Search

This review is focused on neutrino mixing and neutrino oscillations in the light of the recent experimental developments. After discussing possible types of neutrino mixing for Dirac and Majorana neutrinos and considering in detail the phenomenology of neutrino oscillations in vacuum and matter, we review all existing evidence and indications in favour of neutrino oscillations that have been obtained in

W. Grimus; C. Giunti

1999-01-01

38

Search for Majorana neutrinos with the first two years of EXO-200 data.  

PubMed

Many extensions of the standard model of particle physics suggest that neutrinos should be Majorana-type fermions-that is, that neutrinos are their own anti-particles-but this assumption is difficult to confirm. Observation of neutrinoless double-? decay (0???), a spontaneous transition that may occur in several candidate nuclei, would verify the Majorana nature of the neutrino and constrain the absolute scale of the neutrino mass spectrum. Recent searches carried out with (76)Ge (the GERDA experiment) and (136)Xe (the KamLAND-Zen and EXO (Enriched Xenon Observatory)-200 experiments) have established the lifetime of this decay to be longer than 10(25)?years, corresponding to a limit on the neutrino mass of 0.2-0.4?electronvolts. Here we report new results from EXO-200 based on a large (136)Xe exposure that represents an almost fourfold increase from our earlier published data sets. We have improved the detector resolution and revised the data analysis. The half-life sensitivity we obtain is 1.9?×?10(25)?years, an improvement by a factor of 2.7 on previous EXO-200 results. We find no statistically significant evidence for 0??? decay and set a half-life limit of 1.1?×?10(25)?years at the 90 per cent confidence level. The high sensitivity holds promise for further running of the EXO-200 detector and future 0??? decay searches with an improved Xe-based experiment, nEXO. PMID:24896189

2014-06-12

39

TeV Scale See-Saw Mechanisms of Neutrino Mass Generation, the Majorana Nature of the Heavy Singlet Neutrinos and $\\betabeta$-Decay  

E-print Network

It is shown that the Majorana nature of the heavy neutrinos $N_j$ having masses in the range of $M_j \\sim (100 - 1000)$ GeV and present in the TeV scale type I and inverse see-saw scenarios of neutrino mass generation, is unlikely to be observable in the currently operating and future planned accelerator experiments (including LHC) due to the existence of very strong constraints on the parameters and couplings responsible for the corresponding $|\\Delta L| = 2$ processes, $L$ being the total lepton charge. If the heavy Majorana neutrinos $N_j$ are observed and they are associated only with the type I or inverse see-saw mechanisms and no additional TeV scale "new physics", they will behave like Dirac fermions to a relatively high level of precision, being actually pseudo-Dirac particles. The observation of effects proving the Majorana nature of $N_j$ would imply that these heavy neutrinos have additional relatively strong couplings to the Standard Model particles (as, e.g. in the type III see-saw scenario), or that light neutrino masses compatible with the observations are generated by a mechanism other than see-saw (e.g., radiatively at one or two loop level) in which the heavy Majorana neutrinos $N_j$ are nevertheless involved.

A. Ibarra; E. Molinaro; S. T. Petcov

2010-07-14

40

Lepton number violating processes mediated by Majorana neutrinos at hadron colliders  

SciTech Connect

We study the lepton number violating like-sign dilepton processes h{sub 1}h{sub 2}{yields}l{sup {+-}}l{sup '{+-}}jjX and h{sub 1}h{sub 2}{yields}l{sup {+-}}l{sup '{+-}}W{sup {+-}}X, mediated by heavy GeV scale Majorana neutrinos. We focus on the resonantly enhanced contributions with a nearly on-mass-shell Majorana neutrino in the s channel. We study the constraints on like-sign dilepton production at the Tevatron and the LHC on the basis of the existing experimental limits on the masses of heavy neutrinos and their mixings U{sub {alpha}}{sub N} with {alpha}={nu}{sub e}, {nu}{sub {mu}}, {nu}{sub {tau}}. Special attention is paid to the constraints from neutrinoless double beta decay. We note that searches for like-sign e{sup {+-}}e{sup {+-}} events at Tevatron and LHC may provide evidence of CP violation in the neutrino sector. We also discuss the conditions under which it is possible to extract individual constraints on the mixing matrix elements in a model independent way.

Kovalenko, Sergey; Lu Zhun; Schmidt, Ivan [Departamento de Fisica, Universidad Tecnica Federico, Santa Maria, Casilla 110-V, Valparaiso (Chile) and Center of Subatomic Physics, Valparaiso (Chile)

2009-10-01

41

Large electron electric dipole moment in minimal flavor violation framework with Majorana neutrinos  

E-print Network

The latest data from the ACME Collaboration have put a stringent constraint on the electric dipole moment d_e of the electron. Nevertheless, the standard model (SM) prediction for d_e is many orders of magnitude below the new result, making this observable a powerful probe for physics beyond the SM. We carry out a model-independent study of d_e in the SM with right handed neutrinos and its extension with the neutrino seesaw mechanism under the framework of minimal flavor violation. We find that d_e crucially depends on whether neutrinos are Dirac or Majorana particles. In the Majorana case, d_e can reach its experimental bound, and it constrains the scale of minimal flavor violation to be above a few hundred GeV or more. We also explore extra CP-violating sources in the Yukawa couplings of the right-handed neutrinos. Such new sources can have important effects on d_e.

Xiao-Gang He; Chao-Jung Lee; Siao-Fong Li; Jusak Tandean

2014-06-04

42

Quasidegeneracy of Majorana neutrinos and the origin of large leptonic mixing  

NASA Astrophysics Data System (ADS)

We propose that the observed large leptonic mixing may just reflect a quasidegeneracy of three Majorana neutrinos. The limit of exact degeneracy of Majorana neutrinos is not trivial, as leptonic mixing and even C P violation may occur. We conjecture that the smallness of |U13|, when compared to the other elements of UP M N S, may be related to the fact that, in the limit of exact mass degeneracy, the leptonic mixing matrix necessarily has a vanishing element. We show that the lifting of the mass degeneracy can lead to the measured value of |U13| while at the same time accommodating the observed solar and atmospheric mixing angles. In the scenario we consider for the breaking of the mass degeneracy, there is only one C P violating phase, already present in the limit of exact degeneracy, which upon the lifting of the degeneracy generates both Majorana and Dirac-type C P violation in the leptonic sector. We analyze some of the correlations among physical observables and point out that, in most of the cases considered, the implied strength of leptonic Dirac-type C P violation is large enough to be detected in the next round of experiments.

Branco, G. C.; Rebelo, M. N.; Silva-Marcos, J. I.; Wegman, Daniel

2015-01-01

43

Production of like sign dileptons in p-p collisions through composite Majorana neutrinos  

NASA Astrophysics Data System (ADS)

The production of like-sign dileptons (LSD) in the high-energy lepton-number-violating (?L=+2) reaction pp-->2 jets+l+l+ (l=e,?,?), of interest for experiments to be performed at the forthcoming CERN Large Hadron Collider (LHC), is investigated in detail, taking up a composite model scenario in which the exchanged virtual composite neutrino is assumed to be a Majorana particle that couples to the light leptons via the SU(2)×U(1) gauge bosons through a magnetic type coupling (???). A helicity projection method is used to evaluate exactly the tree-level amplitudes of the contributing parton subprocesses (2-->4), which allows one to take into account all exchange diagrams and occurring interferences. Numerical estimates of the corresponding signal cross section that implement kinematical cuts needed to suppress the standard model background are presented which show that in some regions of the parameter space the total number of LSD events is well above the background. Assuming nonobservation of the LSD signal it is found that LHC would exclude a composite Majorana neutrino up to ~900 GeV (if one requires 10 events for discovery). The sensitivity of LHC experiments to the parameter space is then compared to that of the next generation of neutrinoless double beta decay (??0?) experiment, GENIUS, and it is shown that they will provide constraints of the same order of magnitude and will play a complementary role.

Panella, O.; Carimalo, C.; Srivastava, Y. N.

2000-07-01

44

GENIUS Project, Neutrino Oscillations and Cosmology: Neutrinos Reveal Their Nature?  

NASA Astrophysics Data System (ADS)

The neutrinoless double beta decay as well as any other laboratory experiment has not been able to answer the question of the neutrino's nature. Hints on the answer are available when neutrino oscillations and ( ? ? )0 ? are considered simultaneously. In this case phenomenologically interesting neutrino mass schemes can lead to non-vanishing and large values of < m? >. As a consequence, some schemes with Majorana neutrinos can be ruled out even now. If we assume that in addition neutrinos contribute to Hot Dark Matter then the window for Majorana neutrinos is even more restricted, e.g. GENIUS experiment will be sensitive to scenarios with three Majorana neutrinos.

Czakon, M.; Studnik, J.; Zralek, M.; Gluza, J.

2000-06-01

45

Probing Majorana neutrinos in rare K and D, D{sub s}, B, B{sub c} meson decays  

SciTech Connect

We study lepton number violating decays of charged K, D, D{sub s}, B, and B{sub c} mesons of the form M{sup +}{yields}M{sup '-}l{sup +}l{sup +}, induced by the existence of Majorana neutrinos. These processes provide information complementary to neutrinoless double nuclear beta decays, and are sensitive to neutrino masses and lepton mixing. We explore neutrino mass ranges m{sub N} from below 1 eV to several hundred GeV. We find that in many cases the branching ratios are prohibitively small, however in the intermediate range m{sub {pi}<}m{sub N}neutrino masses, the branching ratios can be at the reach of high luminosity experiments like those at the LHC-b and future super flavor factories, and can provide bounds on the lepton mixing parameters.

Cvetic, G.; Dib, Claudio [Centro Cientifico y Tecnologico de Valparaiso and Department of Physics, Universidad Tecnica Federico Santa Maria, Valparaiso (Chile); Kang, Sin Kyu [School of Liberal Arts, Seoul National University of Technology, Seoul 121-742 (Korea, Republic of); Kim, C. S. [Department of Physics and IPAP, Yonsei University, Seoul 120-749 (Korea, Republic of)

2010-09-01

46

Neutrinos in Nuclear Physics  

E-print Network

Since the discovery of nuclear beta decay, nuclear physicists have studied the weak interaction and the nature of neutrinos. Many recent and current experiments have been focused on the elucidation of neutrino oscillations and neutrino mass. The quest for the absolute value of neutrino mass continues with higher precision studies of the tritium beta decay spectrum near the endpoint. Neutrino oscillations are studied through measurements of reactor neutrinos as a function of baseline and energy. And experiments searching for neutrinoless double beta decay seek to discover violation of lepton number and establish the Majorana nature of neutrino masses.

R. D. McKeown

2014-12-03

47

Connecting Dirac and Majorana neutrino mass matrices in the minimal left-right symmetric model.  

PubMed

Probing the origin of neutrino mass by disentangling the seesaw mechanism is one of the central issues of particle physics. We address it in the minimal left-right symmetric model and show how the knowledge of light and heavy neutrino masses and mixings suffices to determine their Dirac Yukawa couplings. This in turn allows one to make predictions for a number of high and low energy phenomena, such as decays of heavy neutrinos, neutrinoless double beta decay, electric dipole moments of charged leptons, and neutrino transition moments. We also discuss a way of reconstructing the neutrino Dirac Yukawa couplings at colliders such as the LHC. PMID:25167249

Nemevšek, Miha; Senjanovi?, Goran; Tello, Vladimir

2013-04-12

48

NEXT, high-pressure xenon gas experiments for ultimate sensitivity to Majorana neutrinos  

E-print Network

In this paper we describe an innovative type of Time Projection Chamber (TPC), which uses high-pressure xenon gas (HPXe) and electroluminescence amplification of the ionization charge as the basis of an apparatus capable of fully reconstructing the energy and topological signature of rare events. We will discuss a specific design of such HPXe TPC, the NEXT-100 detector, that will search for neutrinoless double beta decay events using 100-150 kg of xenon enriched in the isotope Xe-136. NEXT-100 is currently under construction, after completion of an accelerated and very successful R&D period. It will be installed at the Laboratorio Subterr\\'aneo de Canfranc (LSC), in Spain. The commissioning run is expected for late 2013 or early 2014. We will also present physics arguments that suggest that the HPXe technology can be extrapolated to the next-to-next generation (e.g, a fiducial mass of 1 ton of target), which will fully explore the Majorana nature of the neutrino if the mass hierarchy is inverse.

J. J. Gómez-Cadenas; J. Martín-Albo; F. Monrabal; for the NEXT Collaboration

2012-11-21

49

Neutrino Experiments  

SciTech Connect

Recent studies of neutrino oscillations have established the existence of finite neutrino masses and mixing between generations of neutrinos. The combined results from studies of atmospheric neutrinos, solar neutrinos, reactor antineutrinos and neutrinos produced at accelerators paint an intriguing picture that clearly requires modification of the standard model of particle physics. These results also provide clear motivation for future neutrino oscillation experiments as well as searches for direct neutrino mass and nuclear double-beta decay. I will discuss the program of new neutrino oscillation experiments aimed at completing our knowledge of the neutrino mixing matrix.

McKeown, R. D. [W. K. Kellogg Radiation Laboratory, California Institute of Technology, Pasadena, CA (United States)

2010-08-04

50

Constraints on TeV Scale Majorana Neutrino Phenomenology from the Vacuum Stability of the Higgs  

NASA Astrophysics Data System (ADS)

The vacuum stability condition of the Standard Model (SM) Higgs potential with mass in the range of 124-127 GeV puts an upper bound on the Dirac mass of the neutrinos. We study this constraint with the right-handed neutrino masses up to TeV scale. The heavy neutrinos contribute to ?L = 2 processes like neutrinoless double beta decay and same-sign-dilepton (SSD) production in the colliders. The vacuum stability criterion also restricts the light-heavy neutrino mixing and constrains the branching ratio (BR) of lepton flavor-violating process, like ??e? mediated by the heavy neutrinos. We show that neutrinoless double beta decay with a lifetime 1025 years can be observed if the lightest heavy neutrino mass is <4.5 TeV. We show that the vacuum stability condition and the experimental bound on ??e ? together put a constrain on heavy neutrino mass MR>3.3 TeV. Finally we show that the observation of SSDs associated with jets at the LHC needs much larger luminosity than available at present. We have estimated the possible maximum cross-section for this process at the LHC and show that with an integrated luminosity 100 fb-1 it may be possible to observe the SSD signals as long as MR < 400 GeV.

Chakrabortty, Joydeep; Das, Moumita; Mohanty, Subhendra

2013-04-01

51

Neutrinos, a window on new physics  

E-print Network

This paper reviews some aspects of the physics of neutrinos, in particular neutrino masses and the issue of Dirac versus Majorana neutrinos. The see-saw mechanism is described and it is argued that the Majorana nature of neutrinos can be tested by measuring the invisible decays of the Higgs particle, as its decay into neutrinos is determined by their Yukawa couplings, i.e. the Dirac masses, rather than the physical Majorana masses. The measurement would allow us to probe the scale M of the large Majorana masses for right-handed singlet neutrinos. The optimal machine for performing such a measurement would be a future electron-positron collider.

van Holten, J W

2014-01-01

52

Neutrinos, a window on new physics  

E-print Network

This paper reviews some aspects of the physics of neutrinos, in particular neutrino masses and the issue of Dirac versus Majorana neutrinos. The see-saw mechanism is described and it is argued that the Majorana nature of neutrinos can be tested by measuring the invisible decays of the Higgs particle, as its decay into neutrinos is determined by their Yukawa couplings, i.e. the Dirac masses, rather than the physical Majorana masses. The measurement would allow us to probe the scale M of the large Majorana masses for right-handed singlet neutrinos. The optimal machine for performing such a measurement would be a future electron-positron collider.

J. W. van Holten

2014-12-13

53

Neutrino Oscillations with Reactor Neutrinos  

E-print Network

Prospect measurements of neutrino oscillations with reactor neutrinos are reviewed in this document. The following items are described: neutrinos oscillations status, reactor neutrino experimental strategy, impact of uncertainties on the neutrino oscillation sensitivity and, finally, the experiments in the field. This is the synthesis of the talk delivered during the NOW2006 conference at Otranto (Italy) during September 2006.

Anatael Cabrera

2007-01-11

54

Observables in Neutrino Mass Spectroscopy Using Atoms  

E-print Network

The process of collective de-excitation of atoms in a metastable level into emission mode of a single photon plus a neutrino pair, called radiative emission of neutrino pair (RENP), is sensitive to the absolute neutrino mass scale, to the neutrino mass hierarchy and to the nature (Dirac or Majorana) of massive neutrinos. We investigate how the indicated neutrino mass and mixing observables can be determined from the measurement of the corresponding continuous photon spectrum taking the example of a transition between specific levels of the Yb atom. The possibility of determining the nature of massive neutrinos and, if neutrinos are Majorana fermions, of obtaining information about the Majorana phases in the neutrino mixing matrix, is analyzed in the cases of normal hierarchical, inverted hierarchical and quasi-degenerate types of neutrino mass spectrum. We find, in particular, that the sensitivity to the nature of massive neutrinos depends critically on the atomic level energy difference relevant in the RENP.

D. N. Dinh; S. T. Petcov; N. Sasao; M. Tanaka; M. Yoshimura

2012-09-21

55

B-L Neutrinos  

E-print Network

Neutrino masses and mixings are analyzed in terms of left-handed fields and a 6x6 complex symmetric mass matrix whose singular values are the neutrino masses. An angle theta_nu characterizes the kind of the neutrinos, with theta_nu=0 for Dirac neutrinos and theta_nu=pi/2 for Majorana neutrinos. At theta_nu = 0 baryon-minus-lepton number is conserved. If theta_nu is approximately zero, the six neutrino masses coalesce into three nearly degenerate pairs. Thus the tiny mass differences exhibited in the solar and atmospheric neutrino experiments are naturally explained by the approximate conservation of B-L. Neutrinos are nearly Dirac fermions. This B-L model leads to these predictions: neutrinos oscillate mainly between flavor eigenfields and sterile eigenfields, and so the appearance of neutrinos and antineutrinos is suppressed; neutrinos may well be of cosmological importance; in principle the disappearance of the tau neutrino should be observable; and neutrinoless double-beta decay is suppressed by an extra factor of 10^(-5) and so will not be seen in the Heidelberg/Moscow, IGEX, GENIUS, or CUORE experiments.

Kevin Cahill

1999-12-26

56

Search for Heavy Majorana Neutrinos in ?[superscript ±]?[superscript ±] + just and e[superscript ±]e[superscript ±] + jets events in pp collisions at ?s = 7 TeV  

E-print Network

A search is performed for heavy Majorana neutrinos (N) using an event signature defined by two same-sign charged leptons of the same flavour and two jets. The data correspond to an integrated luminosity of 4.98 fb[superscript ...

Apyan, Aram

57

Sterile neutrinos?  

E-print Network

The notion of sterile neutrinos is discussed. The schemes of mixing of four massive neutrinos, which imply the existence of sterile neutrinos, are briefly considered. Several model independent methods that allow to reveal possible transitions of solar neutrinos into sterile states are presented.

S. M. Bilenky; C. Giunti

1999-05-05

58

Solar Neutrinos  

E-print Network

Present results and future measurements of solar neutrinos are discussed. The results to date indicate that solar electron neutrinos are changing to other active types and that transitions solely to sterile neutrinos are disfavored. The flux of $^{8}B$ solar neutrinos produced in the Sun, inferred assuming only active neutrino types, is found to be in very good agreement with solar model calculations. Future measurements will focus on greater accuracy for charged current and neutral current sensitive reactions to provide more accurate measurements of neutrino flavour change and further studies of day-night flux differences and spectral shape. Other experiments sensitive to lower energy solar neutrinos will be in operation soon.

A. B. McDonald

2002-09-21

59

Tau Neutrino Appearance via Neutrino Oscillations in Atmospheric Neutrinos  

E-print Network

Tau Neutrino Appearance via Neutrino Oscillations in Atmospheric Neutrinos A Dissertation Presented of the Dissertation Tau Neutrino Appearance via Neutrino Oscillations in Atmospheric Neutrinos by Tokufumi Kato Doctor of Philosophy in Physics Stony Brook University 2007 A search for the appearance of tau neutrinos from µ

Tokyo, University of

60

An alternative for righthanded neutrinos: lefthanded see--saw  

E-print Network

A new lefthanded see-saw mechanism is constructed, implying both the smallness of active-neutrino masses and decoupling of heavy passive neutrinos, similarly to the situation in the case of conventional see-saw. But now, in place of the conventional righthanded neutrinos, the lefthanded sterile neutrinos play the role of heavy passive neutrinos, the righthanded neutrinos and righthanded sterile neutrinos being absent. In this case, the neutrino mass term is necessarily of pure Majorana type.

Wojciech Krolikowski

1999-09-10

61

Neutrino Detectors  

NASA Astrophysics Data System (ADS)

The neutrino was postulated by Wolfgang Pauli in the early 1930s, but could only be detected for the first time in the 1950s. Ever since scientists all around the world have worked on the detection and understanding of this particle which so scarcely interacts with matter. Depending on the origin and nature of the neutrino, various types of experiments have been developed and operated. In this entry, we will review neutrino detectors in terms of neutrino energy and associated detection technique as well as the scientific outcome of some selected examples. After a brief historical introduction, the detection of low-energy neutrinos originating from nuclear reactors or from the Earth is used to illustrate the principles and difficulties which are encountered in detecting neutrinos. In the context of solar neutrino spectroscopy, where the neutrino is used as a probe for astrophysics, three different types of neutrino detectors are presented - water ?erenkov, radiochemical, and liquid-scintillator detectors. Moving to higher neutrino energies, we discuss neutrinos produced by astrophysical sources and from accelerators. The entry concludes with an overview of a selection of future neutrino experiments and their scientific goals.

von Feilitzsch, Franz; Lanfranchi, Jean-Côme; Wurm, Michael

62

Neutrino Lensing  

E-print Network

Due to the intrinsic properties of neutrinos, the gravitational lens effect for neutrino should be more colorful and meaningful than the normal lens effect of photon. Other than the oscillation experiments operated at terrestrial laboratory, in principle, we can propose a completely new astrophysical method to determine not only the nature of gravity and spacetime of lens objects but also the mixing parameters of neutrinos by analyzing neutrino trajectories near the central objects. However, compared with the contemporaneous telescopes through the observation of the electromagnetic radiation, the angular, energy and time resolution of the neutrino telescopes are still comparatively poor, we just concentrate on the two classical tests of general relativity, i.e. the angular deflection and time delay of neutrino by a lens object as a preparative work in this paper. In addition, some simple properties of neutrino lensing are investigated.

Luo Xin-Lian

2009-09-28

63

Search for heavy Majorana neutrinos in $\\mu^\\pm \\mu^\\pm$+jets events in proton-proton collisions at $\\sqrt{s}$ = 8 TeV  

E-print Network

A search is performed for heavy Majorana neutrinos (N) using an event signature defined by two muons of the same charge and two jets ($\\mu^\\pm \\mu^\\pm \\mathrm{j j}$). The data correspond to an integrated luminosity of 19.7 fb$^{-1}$ of proton-proton collisions at a center-of-mass energy of 8 TeV, collected with the CMS detector at the CERN LHC. No excess of events is observed beyond the expected standard model background and upper limits are set on $|V_{\\mu\\mathrm{N}}|^2$ as a function of Majorana neutrino mass $\\mathrm{m}_{\\mathrm{N}}$ for masses in the range of 40-500 GeV, where $|V_{\\mu\\mathrm{N}}|$ is the mixing element of the heavy neutrino with the standard model muon neutrino. The limits obtained are $|V_{\\mu\\mathrm{N}}|^2 \\le 0.00470$ for $\\mathrm{m}_{\\mathrm{N}} = 90$ GeV, $|V_{\\mu\\mathrm{N}}|^2 \\le 0.0123$ for $\\mathrm{m}_{\\mathrm{N}} = 200$ GeV, and $|V_{\\mu\\mathrm{N}}|^2 \\le 0.583$ for $\\mathrm{m}_{\\mathrm{N}} = 500$ GeV. These results extend considerably the regions excluded by previous direct s...

Khachatryan, Vardan; CMS Collaboration; Tumasyan, Armen; Adam, Wolfgang; Bergauer, Thomas; Dragicevic, Marko; Erö, Janos; Friedl, Markus; Fruehwirth, Rudolf; Ghete, Vasile Mihai; Hartl, Christian; Hörmann, Natascha; Hrubec, Josef; Jeitler, Manfred; Kiesenhofer, Wolfgang; Knünz, Valentin; Krammer, Manfred; Krätschmer, Ilse; Liko, Dietrich; Mikulec, Ivan; Rabady, Dinyar; Rahbaran, Babak; Rohringer, Herbert; Schöfbeck, Robert; Strauss, Josef; Treberer-Treberspurg, Wolfgang; Waltenberger, Wolfgang; Wulz, Claudia-Elisabeth; Mossolov, Vladimir; Shumeiko, Nikolai; Suarez Gonzalez, Juan; Alderweireldt, Sara; Bansal, Sunil; Cornelis, Tom; De Wolf, Eddi A; Janssen, Xavier; Knutsson, Albert; Lauwers, Jasper; Luyckx, Sten; Ochesanu, Silvia; Rougny, Romain; Van De Klundert, Merijn; Van Haevermaet, Hans; Van Mechelen, Pierre; Van Remortel, Nick; Van Spilbeeck, Alex; Blekman, Freya; Blyweert, Stijn; D'Hondt, Jorgen; Daci, Nadir; Heracleous, Natalie; Keaveney, James; Lowette, Steven; Maes, Michael; Olbrechts, Annik; Python, Quentin; Strom, Derek; Tavernier, Stefaan; Van Doninck, Walter; Van Mulders, Petra; Van Onsem, Gerrit Patrick; Villella, Ilaria; Caillol, Cécile; Clerbaux, Barbara; De Lentdecker, Gilles; Dobur, Didar; Favart, Laurent; Gay, Arnaud; Grebenyuk, Anastasia; Léonard, Alexandre; Mohammadi, Abdollah; Perniè, Luca; Randle-conde, Aidan; Reis, Thomas; Seva, Tomislav; Thomas, Laurent; Vander Velde, Catherine; Vanlaer, Pascal; Wang, Jian; Zenoni, Florian; Adler, Volker; Beernaert, Kelly; Benucci, Leonardo; Cimmino, Anna; Costantini, Silvia; Crucy, Shannon; Fagot, Alexis; Garcia, Guillaume; Mccartin, Joseph; Ocampo Rios, Alberto Andres; Poyraz, Deniz; Ryckbosch, Dirk; Salva Diblen, Sinem; Sigamani, Michael; Strobbe, Nadja; Thyssen, Filip; Tytgat, Michael; Yazgan, Efe; Zaganidis, Nicolas; Basegmez, Suzan; Beluffi, Camille; Bruno, Giacomo; Castello, Roberto; Caudron, Adrien; Ceard, Ludivine; Da Silveira, Gustavo Gil; Delaere, Christophe; Du Pree, Tristan; Favart, Denis; Forthomme, Laurent; Giammanco, Andrea; Hollar, Jonathan; Jafari, Abideh; Jez, Pavel; Komm, Matthias; Lemaitre, Vincent; Nuttens, Claude; Pagano, Davide; Perrini, Lucia; Pin, Arnaud; Piotrzkowski, Krzysztof; Popov, Andrey; Quertenmont, Loic; Selvaggi, Michele; Vidal Marono, Miguel; Vizan Garcia, Jesus Manuel; Beliy, Nikita; Caebergs, Thierry; Daubie, Evelyne; Hammad, Gregory Habib; Aldá Júnior, Walter Luiz; Alves, Gilvan; Brito, Lucas; Correa Martins Junior, Marcos; Dos Reis Martins, Thiago; Molina, Jorge; Mora Herrera, Clemencia; Pol, Maria Elena; Rebello Teles, Patricia; Carvalho, Wagner; Chinellato, Jose; Custódio, Analu; Da Costa, Eliza Melo; De Jesus Damiao, Dilson; De Oliveira Martins, Carley; Fonseca De Souza, Sandro; Malbouisson, Helena; Matos Figueiredo, Diego; Mundim, Luiz; Nogima, Helio; Prado Da Silva, Wanda Lucia; Santaolalla, Javier; Santoro, Alberto; Sznajder, Andre; Tonelli Manganote, Edmilson José; Vilela Pereira, Antonio; Bernardes, Cesar Augusto; Dogra, Sunil; Tomei, Thiago; De Moraes Gregores, Eduardo; Mercadante, Pedro G; Novaes, Sergio F; Padula, Sandra; Aleksandrov, Aleksandar; Genchev, Vladimir; Hadjiiska, Roumyana; Iaydjiev, Plamen; Marinov, Andrey; Piperov, Stefan; Rodozov, Mircho; Stoykova, Stefka; Sultanov, Georgi; Vutova, Mariana; Dimitrov, Anton; Glushkov, Ivan; Litov, Leander; Pavlov, Borislav; Petkov, Peicho; Bian, Jian-Guo; Chen, Guo-Ming; Chen, He-Sheng; Chen, Mingshui; Cheng, Tongguang; Du, Ran; Jiang, Chun-Hua; Plestina, Roko; Romeo, Francesco; Tao, Junquan; Wang, Zheng; Asawatangtrakuldee, Chayanit; Ban, Yong; Liu, Shuai; Mao, Yajun; Qian, Si-Jin; Wang, Dayong; Xu, Zijun; Zhang, Fengwangdong; Zhang, Linlin; Zou, Wei; Avila, Carlos; Cabrera, Andrés; Chaparro Sierra, Luisa Fernanda; Florez, Carlos; Gomez, Juan Pablo; Gomez Moreno, Bernardo; Sanabria, Juan Carlos; Godinovic, Nikola; Lelas, Damir; Polic, Dunja; Puljak, Ivica; Antunovic, Zeljko; Kovac, Marko; Brigljevic, Vuko; Kadija, Kreso; Luetic, Jelena; Mekterovic, Darko; Sudic, Lucija; Attikis, Alexandros; Mavromanolakis, Georgios; Mousa, Jehad; Nicolaou, Charalambos; Ptochos, Fotios; Razis, Panos A; Rykaczewski, Hans; Bodlak, Martin; Finger, Miroslav; Finger Jr, Michael; Assran, Yasser; Elgammal, Sherif; Ellithi Kamel, Ali; Radi, Amr; Kadastik, Mario; Murumaa, Marion; Raidal, Martti; Tiko, Andres; Eerola, Paula; Voutilainen, Mikko; Härkönen, Jaakko; Karimäki, Veikko; Kinnunen, Ritva; Kortelainen, Matti J; Lampén, Tapio; Lassila-Perini, Kati; Lehti, Sami; Lindén, Tomas; Luukka, Panja-Riina; Mäenpää, Teppo; Peltola, Timo; Tuominen, Eija

2015-01-01

64

Neutrino factory  

NASA Astrophysics Data System (ADS)

The properties of the neutrino provide a unique window on physics beyond that described by the standard model. The study of subleading effects in neutrino oscillations, and the race to discover CP-invariance violation in the lepton sector, has begun with the recent discovery that ?13>0 . The measured value of ?13 is large, emphasizing the need for a facility at which the systematic uncertainties can be reduced to the percent level. The neutrino factory, in which intense neutrino beams are produced from the decay of muons, has been shown to outperform all realistic alternatives and to be capable of making measurements of the requisite precision. Its unique discovery potential arises from the fact that only at the neutrino factory is it practical to produce high-energy electron (anti)neutrino beams of the required intensity. This paper presents the conceptual design of the neutrino factory accelerator facility developed by the European Commission Framework Programme 7 EURO ? Design Study consortium. EURO ? coordinated the European contributions to the International Design Study for the Neutrino Factory (the IDS-NF) collaboration. The EURO ? baseline accelerator facility will provide 1 021 muon decays per year from 12.6 GeV stored muon beams serving a single neutrino detector situated at a source-detector distance of between 1 500 km and 2 500 km. A suite of near detectors will allow definitive neutrino-scattering experiments to be performed.

Bogomilov, M.; Matev, R.; Tsenov, R.; Dracos, M.; Bonesini, M.; Palladino, V.; Tortora, L.; Mori, Y.; Planche, T.; Lagrange, J. B.; Kuno, Y.; Benedetto, E.; Efthymiopoulos, I.; Garoby, R.; Gilardoini, S.; Martini, M.; Wildner, E.; Prior, G.; Blondel, A.; Karadzhow, Y.; Ellis, M.; Kyberd, P.; Bayes, R.; Laing, A.; Soler, F. J. P.; Alekou, A.; Apollonio, M.; Aslaninejad, M.; Bontoiu, C.; Jenner, L. J.; Kurup, A.; Long, K.; Pasternak, J.; Zarrebini, A.; Poslimski, J.; Blackmore, V.; Cobb, J.; Tunnell, C.; Andreopoulos, C.; Bennett, J. R. J.; Brooks, S.; Caretta, O.; Davenne, T.; Densham, C.; Edgecock, T. R.; Fitton, M.; Kelliher, D.; Loveridge, P.; McFarland, A.; Machida, S.; Prior, C.; Rees, G.; Rogers, C.; Rooney, M.; Thomason, J.; Wilcox, D.; Booth, C.; Skoro, G.; Back, J. J.; Harrison, P.; Berg, J. S.; Fernow, R.; Gallardo, J. C.; Gupta, R.; Kirk, H.; Simos, N.; Stratakis, D.; Souchlas, N.; Witte, H.; Bross, A.; Geer, S.; Johnstone, C.; Makhov, N.; Neuffer, D.; Popovic, M.; Strait, J.; Striganov, S.; Morfín, J. G.; Wands, R.; Snopok, P.; Bagacz, S. A.; Morozov, V.; Roblin, Y.; Cline, D.; Ding, X.; Bromberg, C.; Hart, T.; Abrams, R. J.; Ankenbrandt, C. M.; Beard, K. B.; Cummings, M. A. C.; Flanagan, G.; Johnson, R. P.; Roberts, T. J.; Yoshikawa, C. Y.; Graves, V. B.; McDonald, K. T.; Coney, L.; Hanson, G.

2014-12-01

65

Neutrino oscillometry  

NASA Astrophysics Data System (ADS)

Neutrino oscillations are studied employing sources of low energy monoenergetic neutrinos following electron capture by the nucleus and measuring electron recoils. Since the neutrino energy is very low the oscillation length L23 appearing in this electronic neutrino disappearance experiment can be so small that the full oscillation can take place inside the detector so that one may determine very accurately the neutrino oscillation parameters. In particular, since the oscillation probability is proportional to sin2 2?13, one can measure or set a better limit on the unknown parameter ?13. One, however, has to pay the price that the expected counting rates are very small. Thus one needs a very intensive neutrino source and a large detector with as low as possible energy threshold and high energy and position resolution. Both spherical gaseous and cylindrical liquid detectors are studied. Different source candidates are considered.

Vergados, J. D.; Giomataris, Y.; Novikov, Yu. N.

2012-08-01

66

Perturbed S{sub 3} neutrinos  

SciTech Connect

We study the effects of the perturbation, which violates the permutation symmetry of three Majorana neutrinos but preserves the well-known (23) interchange symmetry. This is done in the presence of an arbitrary Majorana phase {psi}, which serves to ensure the degeneracy of the three neutrinos at the unperturbed level.

Jora, Renata [Grup de Fisica Teorica, Universitat Autonoma de Barcelona, E-08193 Belaterra, Barcelona (Spain); Schechter, Joseph; Shahid, M. Naeem [CP3-Origins, Campusvej 55, DK-5230 Odense M (Denmark); Department of Physics, Syracuse University, Syracuse, New York 13244-1130 (United States)

2009-11-01

67

Probing Late Neutrino Mass Properties with Supernova Neutrinos  

E-print Network

Models of late-time neutrino mass generation contain new interactions of the cosmic background neutrinos with supernova relic neutrinos (SRNs) through exchange of the on-shell light boson, leading to significant modification of the differential SRN flux observed at earth. We consider Abelian U(1) model for generating neutrino masses at low scales and we show that there is a large parameter space in this model for which the changes induced in the flux by the exchange of the light bosons might allow one to distinguish between neutrinos being Majorana or Dirac particles, the type of neutrino mass hierarchy (normal or inverted or quasi-degenerate), and could also possibly determine the absolute values of the neutrino masses. Measurements of the presence of these effects would be possible at the next-generation water Cerenkov detectors enriched with Gadolinium, or a large 100 kton liquid argon detector.

Joseph L. Baker; Haim Goldberg; Gilad Perez; Ina Sarcevic

2007-08-08

68

Probing late neutrino mass properties with supernova neutrinos  

NASA Astrophysics Data System (ADS)

Models of late-time neutrino mass generation contain new interactions of the cosmic background neutrinos with supernova relic neutrinos (SRNs). Exchange of an on-shell light scalar may lead to significant modification of the differential SRN flux observed at earth. We consider an Abelian U(1) model for generating neutrino masses at low scales, and show that there are cases for which the changes induced in the flux allow one to distinguish the Majorana or Dirac nature of neutrinos, as well as the type of neutrino mass hierarchy (normal or inverted or quasidegenerate). In some region of parameter space the determination of the absolute values of the neutrino masses is also conceivable. Measurements of the presence of these effects may be possible at the next-generation water Cerenkov detectors enriched with Gadolinium, or a 100 kton liquid argon detector.

Baker, Joseph; Goldberg, Haim; Perez, Gilad; Sarcevic, Ina

2007-09-01

69

An unorthodox alternative for righthanded neutrinos: lefthanded see-saw  

E-print Network

A new lefthanded see-saw mechanism is constructed, implying both the smallness of active-neutrino masses and decoupling of heavy passive neutrinos, similarly to the situation in the case of conventional see-saw. But now, in place of the conventional righthanded neutrinos, the lefthanded sterile neutrinos play the role of heavy passive neutrinos, the righthanded neutrinos and righthanded sterile neutrinos being absent. Here, the lefthanded sterile neutrinos are different from charge conjugates of conventional righthanded neutrinos because their lepton numbers differ. In this case, the neutrino mass term is necessarily of pure Majorana type.

W. Krolikowski

1999-11-02

70

Neutrino Observatories  

NSDL National Science Digital Library

This online article, from Cosmic Horizons: Astronomy at the Cutting Edge, takes an in-depth look at the new generation of astronomy equipment. It provides an overview of the discovery of neutrinos, subatomic particles, and their role in the developing field of physics, studies that showed that nuclear reactions, including those that power the stars, produce an enormous number of neutrinos, the creation of neutrino observatories deep underground and the stunning and unexpected advances these observatories have already made.

71

Atmospheric neutrinos and discovery of neutrino oscillations  

PubMed Central

Neutrino oscillation was discovered through studies of neutrinos produced by cosmic-ray interactions in the atmosphere. These neutrinos are called atmospheric neutrinos. They are produced as decay products in hadronic showers resulting from collisions of cosmic rays with nuclei in the atmosphere. Electron-neutrinos and muon-neutrinos are produced mainly by the decay chain of charged pions to muons to electrons. Atmospheric neutrino experiments observed zenith-angle and energy dependent deficit of muon-neutrino events. Neutrino oscillations between muon-neutrinos and tau-neutrinos explain these data well. Neutrino oscillations imply that neutrinos have small but non-zero masses. The small neutrino masses have profound implications to our understanding of elementary particle physics and the Universe. This article discusses the experimental discovery of neutrino oscillations. PMID:20431258

Kajita, Takaaki

2010-01-01

72

Small neutrino masses from supersymmetry breaking  

Microsoft Academic Search

An alternative to the conventional seesaw mechanism is proposed to explain the origin of small neutrino masses in supersymmetric theories. The masses and couplings of the right-handed neutrino field are suppressed by supersymmetry breaking, in a way similar to the suppression of the Higgs doublet mass mu. New mechanisms for light Majorana and Dirac neutrinos arise, depending on the degree

Nima Arkani-Hamed; Lawrence Hall; Hitoshi Murayama; David Smith; Neal Weiner

2001-01-01

73

Massive neutrinos in particle physics and astrophysics  

SciTech Connect

The concepts of Majorana and Dirac neutrinos are reviewed from an operational point of view and survey the experimental search for neutrino mass. Also reviewed are the work of Mikheyev and Smirnov on the enhancement of neutrino oscillations via the mechanism of Wolfenstein matter oscillations. Results of an extensive computation of MSW effects in the sun are described. 41 refs., 6 figs.

Rosen, S.P.

1986-01-01

74

Solar Neutrinos  

E-print Network

Solar neutrino investigation has represented one of the most active field of particle physics over the past decade, accumulating important and sometimes unexpected achievements. After reviewing some of the most recent impressive successes, the future perspectives of this exciting area of neutrino research will be discussed.

Bellini, G.; Ranucci, G.

2010-01-01

75

Neutrino astronomy  

SciTech Connect

Current knowledge and proposed experiments in the field of neutrino astronomy are reviewed, with particular emphasis on expected sources and existing and proposed detectors for intermediate-energy (10 to 50 MeV) and ultrahigh energy (greater than 10 GeV) neutrinos. Following a brief discussion of the counting rate obtained in the solar neutrino experiment of Davis (1978) and possible statistical sources for the discrepancy between the expected and observed rates, consideration is given to the physics of neutrino ejection in stellar gravitational collapse and sources of high-energy proton collisions giving rise to ultrahigh energy neutrinos. The capabilities of operating Cerenkov detectors at the Homestake Gold Mine, the Mt. Blanc Tunnel and in the Soviet Caucasus are considered in relation to the detection of gravitational collapse in the center of the galaxy, and it is pointed out that neutrino detectors offer a more reliable means of detecting collapses in the Galaxy than do gravitational wave detectors. The possibility of using Cerenkov detectors for ultrahigh energy neutrino detection is also indicated, and applications of large neutrino detectors such as the proposed DUMAND array to measure the lifetime of the proton are discussed.

Schramm, D.N.

1980-01-01

76

Neutrino Telescopes  

SciTech Connect

Neutrino telescopes complement gamma ray telescopes in the observations of energetic astronomical sources as well as in searching for the dark matter. This paper gives the status of the current generation neutrino telescopes projects: Baikal, AMANDA, NESTOR, NEMO and ANTARES with particular emphasis on the ANTARES telescope in the Mediterranean Sea.

Carr, John [Centre de Physiques des Particules de Marseille, IN2P3/CNRS (France)

2005-02-21

77

Neutrino mass  

SciTech Connect

Neutrinos play a dominant role in both particle physics, astrophysics, and cosmology. In the our present understanding of the strong, weak, and electromagnetic forces, the group structure of the Standard Model is SU(3){sub C} {circle_times} SU(2){sub L} {circle_times} U(I){sub EM}. In the Weinberg-Salam-Glashow Standard Electroweak Model, left-handed neutrinos sit in a doublet, while right-handed neutrinos are in a singlet, and therefore do not interact with the other known particles. Also in this model, the neutrinos are intrinsically massless. However, while the W-S-G model provides an amazingly accurate picture of our present cold Universe, It has a number of deficits. The Standard Model does not explain the origin of the group structure, It does not reduce the number of coupling constants required, nor does it offer any prediction for the physical masses of the particles. Thus, it is generally assumed that the Standard Model is but a subset of some larger gauge theory. A wide variety of Grand Unified field Theories (GUTs), Super Symmetric Models (SUSY), and Superstring models have been proposed as the model for this larger structure. In general, these models predict nonzero neutrino masses and contain mechanisms that provide for lepton-number violation. Thus, a variety of new phenomena are predicted, including finite neutrino masses and the possibility that neutrinos can oscillate from one type to another. This report looks at the possibility of detecting neutrino vat mass.

Bowles, T.J.

1993-04-01

78

Neutrino mass  

SciTech Connect

Neutrinos play a dominant role in both particle physics, astrophysics, and cosmology. In the our present understanding of the strong, weak, and electromagnetic forces, the group structure of the Standard Model is SU(3)[sub C] [circle times] SU(2)[sub L] [circle times] U(I)[sub EM]. In the Weinberg-Salam-Glashow Standard Electroweak Model, left-handed neutrinos sit in a doublet, while right-handed neutrinos are in a singlet, and therefore do not interact with the other known particles. Also in this model, the neutrinos are intrinsically massless. However, while the W-S-G model provides an amazingly accurate picture of our present cold Universe, It has a number of deficits. The Standard Model does not explain the origin of the group structure, It does not reduce the number of coupling constants required, nor does it offer any prediction for the physical masses of the particles. Thus, it is generally assumed that the Standard Model is but a subset of some larger gauge theory. A wide variety of Grand Unified field Theories (GUTs), Super Symmetric Models (SUSY), and Superstring models have been proposed as the model for this larger structure. In general, these models predict nonzero neutrino masses and contain mechanisms that provide for lepton-number violation. Thus, a variety of new phenomena are predicted, including finite neutrino masses and the possibility that neutrinos can oscillate from one type to another. This report looks at the possibility of detecting neutrino vat mass.

Bowles, T.J.

1993-01-01

79

Neutrino telescopes  

SciTech Connect

Neutrino astrophysics offers a new possibility to observe our Universe: high-energy neutrinos, produced by the most energetic phenomena in our Galaxy and in the Universe, carry complementary (if not exclusive) information about the cosmos: this young discipline extends in fact the conventional astronomy beyond the usual electromagnetic probe. The weak interaction of neutrinos with matter allows them to escape from the core of astrophysical objects and in this sense they represent a complementary messenger with respect to photons. However, their detection on Earth due to the small interaction cross section requires a large target mass. The aim of this article is to review the scientific motivations of the high-energy neutrino astrophysics, the detection principles together with the description of a running apparatus, the experiment ANTARES, the performance of this detector with some results, and the presentation of other neutrino telescope projects.

Costantini, H., E-mail: costant@cppm.in2p3.fr [CPPM, Aix-Marseille Universite, CNRS/IN2P3 (France)

2012-09-15

80

Sterile Plus Active Neutrinos and Neutrino Oscillations  

NASA Astrophysics Data System (ADS)

Using a 3 + 1 neutrino model with one sterile and the three standard active neutrinos with a 4 × 4 unitary transformation matrix, U, relating flavor to mass neutrino states, the probability of ? ? to ? e transition is estimated using sterile-active neutrino masses determined by MiniBooNE and other experiments and sterile-active neutrino angles in the 4 × 4 U matrix.

Kisslinger, Leonard S.

2014-09-01

81

Radiative Emission of Neutrino Pairs in Atoms and Light Sterile Neutrinos  

E-print Network

The process of Radiative Emission of Neutrino Pair (RENP) in atoms is sensitive to the absolute neutrino mass scale, the type of spectrum neutrino masses obey and the nature - Dirac or Majorana - of massive neutrinos. We analyse the possibility to test the hypothesis of existence of neutrinos with masses at the eV scale coupled to the electron in the weak charged lepton current in an RENP experiment. The presence of eV scale neutrinos in the neutrino mixing is associated with the existence of sterile neutrinos which mix with the active flavour neutrinos. At present there are a number of hints for active-sterile neutrino oscillations driven by $\\Delta m^2 \\sim 1~{\\rm eV^2}$. We perform a detailed analysis of the RENP phenomenology within the "3 + 1" scheme with one sterile neutrino.

D. N. Dinh; S. T. Petcov

2014-11-27

82

Ultrahigh Energy Tau Neutrinos  

E-print Network

We study ultrahigh energy astrophysical neutrinos and the contribution of tau neutrinos from neutrino oscillations, relative to the contribution of the other flavors. We show the effect of tau neutrino regeneration and tau energy loss as they propagate through the Earth. We consider a variety of neutrino fluxes, such as cosmogenic neutrinos and neutrinos that originate in Active Galactic Nuclei. We discuss signals of tau neutrinos in detectors such as IceCube, RICE and ANITA.

J. Jones; I. Mocioiu; M. H. Reno; I Sarcevic

2005-07-30

83

Ultrahigh Energy Tau Neutrinos  

NASA Astrophysics Data System (ADS)

We study ultrahigh energy astrophysical neutrinos and the contribution of tau neutrinos from neutrino oscillations, relative to the contribution of the other flavors. We show the effect of tau neutrino regeneration and tau energy loss as they propagate through the Earth. We consider a variety of neutrino fluxes, such as cosmogenic neutrinos and neutrinos that originate in Active Galactic Nuclei. We discuss signals of tau neutrinos in detectors such as IceCube, RICE and ANITA.

Jones, J.; Mocioiu, I.; Sarcevic, I.; Reno, M. H.

84

The ideal neutrino beams  

Microsoft Academic Search

The advance in neutrino oscillation physics is driven by the availability of well characterized and high flux neutrino beams. The three present options for the next generation neutrino oscillation facility are super beams, neutrino factories and beta-beams. A super-beam is a very high intensity classical neutrino beam generated by protons impinging on a target where the neutrinos are generated by

Mats Lindroos

2009-01-01

85

Neutrino oscillations in dense neutrino gases  

NASA Astrophysics Data System (ADS)

We consider oscillations of neutrinos under conditions in which the neutrino density is sufficiently large that neutrino-neutrino interactions cannot be neglected. A formalism is developed to treat this highly nonlinear system. Numerical analysis reveals a rich array of phenomena. In certain gases, a self-induced Mikheyev-Smirnov-Wolfenstein effect occurs in which electron neutrinos are resonantly converted into muon neutrinos. In another relatively low-density gas, an unexpected parametric resonant conversion takes place. Finally, neutrino-neutrino interactions maintain coherence in one system for which a priori one expected decoherence.

Samuel, Stuart

1993-08-01

86

Bounds on neutrino magnetic moment tensor from solar neutrinos  

E-print Network

Solar neutrinos with non-zero magnetic moments will contribute to the electron scattering rates in the Super-Kamiokande experiment. The magnetic moment scattering events in Super-K can be accommodated in the standard VO or MSW solutions by a change of the parameter space of mass square difference and mixing angle-but the shifted neutrino parameters obtained from Super-K will (for some values of neutrino magnetic moments) become incompatible with the fits from SNO, Gallium and Chlorine experiments. We compute the upper bounds on the Dirac and Majorana magnetic moments of solar neutrinos by simultaneously fitting all the observed solar neutrino rates. The bounds the magnetic moment matrix elements are of the order of 10^{-10} Bohr magnetron.

Anjan S. Joshipura; Subhendra Mohanty

2002-06-05

87

Neutrino Mixing and Neutrino Telescopes  

E-print Network

Measuring flux ratios of ultra-high energy neutrinos is an alternative method to determine the neutrino mixing angles and the CP phase delta. We conduct a systematic analysis of the neutrino mixing probabilities and of various flux ratios measurable at neutrino telescopes. The considered cases are neutrinos from pion, neutron and muon-damped sources. Explicit formulae in case of mu-tau symmetry and its special case tri-bimaximal mixing are obtained, and the leading corrections due to non-zero theta_{13} and non-maximal theta_{23} are given. The first order correction is universal as it appears in basically all ratios. We study in detail its dependence on theta_{13}, theta_{23} and the CP phase, finding that the dependence on theta_{23} is strongest. The flavor compositions for the considered neutrino sources are evaluated in terms of this correction. A measurement of a flux ratio is a clean measurement of the universal correction (and therefore of theta_{13}, theta_{23} and delta) if the zeroth order ratio does not depend on theta_{12}. This favors pion sources over the other cases, which in turn are good candidates to probe theta_{12}. The only situations in which the universal correction does not appear are certain ratios in case of a neutron and muon-damped source, which depend mainly on theta_{12} and receive only quadratic corrections from the other parameters. We further show that there are only two independent neutrino oscillation probabilities, give the allowed ranges of the considered flux ratios and of all probabilities, and show that none of the latter can be zero or one.

Werner Rodejohann

2007-01-03

88

Solar Neutrinos and the Decaying Neutrino Hypothesis  

E-print Network

We explore, mostly using data from solar neutrino experiments, the hypothesis that the neutrino mass eigenstates are unstable. We find that, by combining $^8$B solar neutrino data with those on $^7$Be and lower-energy solar neutrinos, one obtains a mostly model-independent bound on both the $\

Jeffrey M. Berryman; Andre de Gouvea; Daniel Hernandez

2014-11-02

89

Neutrino Oscillations and the Sudbury Neutrino Observatory  

NASA Astrophysics Data System (ADS)

When the existence of the neutrino was almost apologetically first proposed by Wolfgang Pauli it was intended to explain the mysterious apparent absence of energy and momentum in beta decay. 70 years later the neutrino has indeed solved that mystery, but it has generated still more of its own. Are neutrinos massive? Is it possible to create a neutrino with its spin in the same direction as its momentum? What fraction of the mass of the Universe is made up of neutrinos? Are the flavour labels which we put on neutrinos, like electron and muon, really fixed or can they change? Why does no experiment see the predicted flux of neutrinos from the Sun? Why do there appear to be roughly equal numbers of muon and electron neutrinos created in our atmosphere, rather than the 2:1 ratio we would expect? Many of these questions were coupled when Bruno Pontecorvo first suggested that the shortfall in solar neutrino measurements were caused by neutrino oscillations - neutrinos spontaneously changing flavour as they travel from the Sun. 30 years later we still await definitive proof of that conjecture, and providing that proof is the reason for the Sudbury Neutrino Observatory. The talk will discuss the current state of neutrino oscillations studies, and show how the unique capabilities of the Sudbury Neutrino Observatory can provide definitive proof of whether neutrino oscillations are the long-sought answer to the solar neutrino problem.

Wark, David

2001-04-01

90

Solar Neutrinos  

E-print Network

Experimental work with solar neutrinos has illuminated the properties of neutrinos and tested models of how the sun produces its energy. Three experiments continue to take data, and at least seven are in various stages of planning or construction. In this review, the current experimental status is summarized, and future directions explored with a focus on the effects of a non-zero theta-13 and the interesting possibility of directly testing the luminosity constraint. Such a confrontation at the few-percent level would provide a prediction of the solar irradiance tens of thousands of years in the future for comparison with the present-day irradiance. A model-independent analysis of existing low-energy data shows good agreement between the neutrino and electromagnetic luminosities at the +/- 20 % level.

R. G. H. Robertson

2006-02-05

91

Gravitational form factors of the neutrino  

E-print Network

The gravitational properties of the neutrino is studied in the weak field approximation. By imposing the hermiticity condition, CPT and CP invariance on the \\em tensor matrix element, we shown that the allowed gravitational form factors for Dirac and Majorana neutrinos are very different. In a CPT and CP invariant theory, the \\em tensor for a Dirac neutrino of the same specie is characterized by four gravitational form factors. As a result of CPT invariance, the \\em tensor for a Majorana neutrino of the same specie has five form factors. In a CP invariant theory, if the initial and final Majorana neutrinos have the same (opposite) CP parity, then only tensor (pseudo-tensor) type transition are allowed.

K. L. Ng

1993-05-03

92

Neutrino masses, neutrino oscillations, and cosmological implications  

NASA Technical Reports Server (NTRS)

Theoretical concepts and motivations for considering neutrinos having finite masses are discussed and the experimental situation on searches for neutrino masses and oscillations is summarized. The solar neutrino problem, reactor, deep mine and accelerator data, tri decay experiments and double beta-decay data are considered and cosmological implications and astrophysical data relating to neutrino masses are reviewed. The neutrino oscillation solution to the solar neutrino problem, the missing mass problem in galaxy halos and galaxy cluster galaxy formation and clustering, and radiative neutrino decay and the cosmic ultraviolet background radiation are examined.

Stecker, F. W.

1982-01-01

93

Neutrino masses, neutrino oscillations, and cosmological implications  

SciTech Connect

Theoretical concepts and motivations for considering neutrinos having finite masses are discussed and the experimental situation on searches for neutrino masses and oscillations is summarized. The solar neutrino problem, reactor, deep mine and accelerator data, tri-decay experiments and double beta-decay data are considered and cosmological implications and astrophysical data relating to neutrino masses are reviewed. The neutrino oscillation solution to the solar neutrino problem, the missing mass problem in galaxy halos and galaxy cluster galaxy formation and clustering, and radiative neutrino decay and the cosmic ultraviolet background radiation are examined.

Stecker, F.W.

1982-03-01

94

Neutrino Helicity Reversal and Fundamental Symmetries  

E-print Network

A rather elusive helicity reversal occurs in a gedanken experiment in which a massive left-handed Dirac neutrino, traveling at a velocity u experiment thus implies the existence of right-handed, light neutrinos, which are not completely sterile. Furthermore, overtaking a bunch of massive right-handed Dirac neutrinos leads to gradual de-sterilization. We discuss the helicity reversal and the concomitant sterilization and de-sterilization mechanisms by way of an illustrative example calculation, with a special emphasis on massive Dirac and Majorana neutrinos. We contrast the formalism with a modified Dirac neutrino described by a Dirac equation with a pseudoscalar mass term proportional to the fifth current.

U. D. Jentschura; B. J. Wundt

2014-03-12

95

Neutrinos and Symmetries  

E-print Network

Three facets of symmetries in neutrino physics are briefly reviewed: i) The SO(5) symmetry of the neutrino mass and and its connection to the see-saw mechanism; ii) Flavor SU(N) symmetries of dense, self-interacting neutrino gases in astrophysical settings; iii) The neutrino mixing angle theta13 and possible CP-violation in the neutrino sector.

A. B. Balantekin

2009-10-09

96

Decaying Dirac neutrinos  

Microsoft Academic Search

Constraints on Dirac-neutrino decay into invisible particles are surveyed. Neutrino lifetimes short enough to explain the solar-neutrino problem are allowed by present terrestrial and cosmological measurements. A model in which Dirac neutrinos can have such short lifetimes is proposed. The recently resurrected 17-keV neutrino is incorporated into this model.

A. Acker; S. Pakvasa; J. Pantaleone

1992-01-01

97

Solar Neutrinos  

E-print Network

The status of the solar neutrino problem is reviewed. Attempts to explain the observed deficit and spectral distortion, both by astrophysical and particle physics methods, are described. It is argued that the comparison of all experiments strongly prefers the particle physics solutions.

Paul Langacker

1994-11-19

98

Electromagnetic properties of neutrinos  

E-print Network

A short review on electromagnetic properties of neutrinos is presented. In spite of many efforts in the theoretical and experimental studies of neutrino electromagnetic properties, they still remain one of the main puzzles related to neutrinos.

Carlo Giunti; Alexander Studenikin

2010-06-08

99

The Neutrinos of the Neighboring Brane  

E-print Network

The phenomenon of neutrino oscillations is studied usually as a mixing between the flavor neutrinos and the neutrinos having a definite mass. The mixing angles and the mass eigenvalues are treated independently in order to accommodate the experimental data. We suggest that neutrino oscillations are connected to the structure of spacetime. We expand on a recently proposed model, where two "mirror" branes coexist. One brane hosts left-handed particles (our brane), while the other brane hosts right-handed particles. Majorana-type couplings mixes neutrinos in an individual brane, while Dirac-type couplings mixes neutrinos across the brares. We first focus our attention in a single brane. The mass matrix, determined by the Majorana mass, leads to mass eigenstates and further to mixing angles identical to the mixing angles proposed by the tri-bimaximal mixing. When we include the Dirac-type coupling, connecting the two branes, we obtain a definite prediction for the transition to a sterile neutrino (right-handed neutrino). With m_L (m_R) the Majorana mass for the left (right) brane, we are able to explain the solar and the atmospheric neutrino data with m_L = 2m_R and m_R = 10**(-2) eV.

A. Nicolaidis

2013-03-24

100

NEUTRINO FACTORIES - PHYSICS POTENTIALS.  

SciTech Connect

The recent results from Super-Kamiokande atmospheric and solar neutrino observations opens a new era in neutrino physics and has sparked a considerable interest in the physics possibilities with a Neutrino Factory based on the muon storage ring. We present physics opportunities at a Neutrino Factory, and prospects of Neutrino oscillation experiments. Using the precisely known flavor composition of the beam, one could envision an extensive program to measure the neutrino oscillation mixing matrix, including possible CP violating effects. These and Neutrino Interaction Rates for examples of a Neutrino Factory at BNL (and FNAL) with detectors at Gran Sasso, SLAC and Sudan are also presented.

PARSA,Z.

2001-02-16

101

Neutrino Mass Seesaw Version 3: Recent Developments  

SciTech Connect

The origin of neutrino mass is usually attributed to a seesaw mechanism, either through a heavy Majorana fermion singlet (version 1) or a heavy scalar triplet (version 2). Recently, the idea of using a heavy Majorana fermion triplet (version 3) has gained some attention. This is a review of the basic idea involved, its U(1) gauge extension, and some recent developments.

Ma, Ernest [Physics and Astronomy Department, University of California, Riverside, California 92521 (United States)

2009-04-20

102

Solar neutrino experiments and neutrino oscillations  

SciTech Connect

This report gives the results of the Brookhaven solar neutrino experiment that is based upon the neutrino capture reaction, /sup 37/Cl(..nu..,e/sup -/)/sup 37/Ar. The experiment was built in 1967 to test the theory of solar energy production, and it is well known that the neutrino capture rate in the detector is lower than that expected from theoretical models of the sun. The results will be compared to the current solar model calculations. One possible explanation of the low solar neutrino capture rate is that the neutrinos oscillate between two or more neutrino states, a topic of particular interest to this conference. This question is discussed in relation to the /sup 37/Cl experiment, and to other solar neutrino detectors that are capable of observing the lower energy neutrinos from the sun. A radiochemical solar neutrino detector located deep underground has a very low background and is capable of detecting the monoenergetic neutrinos from megacurie sources of radioisotopes that decay by electron capture. Experiments of this nature are described that are capable of testing for neutrino oscillations with a omicronm/sup 2/ as low as 0.2 eV/sup 2/ if there is maximum mixing between two neutrino states.

Cleveland, B.T.; Davis, R. Jr.; Rowley, J.K.

1981-01-01

103

Sterile neutrinos as dark matter  

SciTech Connect

The simplest model that can accommodate a viable nonbaryonic dark matter candidate is the standard electroweak theory with the addition of right-handed or sterile neutrinos. This model has been studied extensively in the context of the hot dark matter scenario. We reexamine this model and find that hot, warm, and cold dark matter are all possibilities. We focus on the case where sterile neutrinos are the dark matter. Since their only direct coupling is to left-handed or active neutrinos, the most efficient production mechanism is via neutrino oscillations. If the production rate is always less than the expansion rate, then these neutrinos will never be in thermal equilibrium. However, they may still play a significant role in the dynamics of the Universe and possibly provide the missing mass necessary for closure. We consider a single generation of neutrino fields ({nu}{sub L}, {nu}{sub R}) with a Dirac mass, {mu}, and a Majorana mass for the right-handed components only, M. For M {much_gt} {mu} we show that the number density of sterile neutrinos is proportional to {mu}{sup 2}/M so that the energy density today is independent of M. However M is crucial in determining the large scale structure of the Universe. In particular, M {approx_equal} 0.1--1.0 key leads to warm dark matter and a structure formation scenario that may have some advantages over both the standard hot and cold dark matter scenarios.

Dodelson, S. [Fermi National Accelerator Lab., Batavia, IL (United States); Widrow, L.M. [Queen`s Univ., Kingston, ON (Canada). Dept. of Physics]|[Toronto Univ., ON (Canada). Canadian Inst. for Theoretical Astrophysics

1993-03-01

104

Sterile neutrinos as dark matter  

SciTech Connect

The simplest model that can accommodate a viable nonbaryonic dark matter candidate is the standard electroweak theory with the addition of right-handed or sterile neutrinos. This model has been studied extensively in the context of the hot dark matter scenario. We reexamine this model and find that hot, warm, and cold dark matter are all possibilities. We focus on the case where sterile neutrinos are the dark matter. Since their only direct coupling is to left-handed or active neutrinos, the most efficient production mechanism is via neutrino oscillations. If the production rate is always less than the expansion rate, then these neutrinos will never be in thermal equilibrium. However, they may still play a significant role in the dynamics of the Universe and possibly provide the missing mass necessary for closure. We consider a single generation of neutrino fields ([nu][sub L], [nu][sub R]) with a Dirac mass, [mu], and a Majorana mass for the right-handed components only, M. For M [much gt] [mu] we show that the number density of sterile neutrinos is proportional to [mu][sup 2]/M so that the energy density today is independent of M. However M is crucial in determining the large scale structure of the Universe. In particular, M [approx equal] 0.1--1.0 key leads to warm dark matter and a structure formation scenario that may have some advantages over both the standard hot and cold dark matter scenarios.

Dodelson, S. (Fermi National Accelerator Lab., Batavia, IL (United States)); Widrow, L.M. (Queen's Univ., Kingston, ON (Canada). Dept. of Physics Toronto Univ., ON (Canada). Canadian Inst. for Theoretical Astrophysics)

1993-03-01

105

Muons and Neutrinos 2007  

E-print Network

This paper is the written version of the rapporteur talk on Section HE-2, muons and neutrinos, presented at the 30th International Cosmic Ray Conference, Merida, Yucatan, July 11, 2007. Topics include atmospheric muons and neutrinos, solar neutrinos and astrophysical neutrinos as well as calculations and instrumentation related to these topics.

Thomas K. Gaisser

2008-01-29

106

Whatâs a Neutrino?  

NSDL National Science Digital Library

This website contains an introduction to neutrinos, one of the fundamental particles that make up the universe. A description of neutrinos and their properties is provided. The site also includes a chronology of neutrinos studies and discoveries, frequently asked questions, and links to more information about neutrinos.

2006-11-30

107

New Neutrinos Algal Biofuels  

E-print Network

New Neutrinos Algal Biofuels Charged-Particle Vision Primordial Soup LOS ALAMOS SCIENCE in Illinois, a beam of neutrino particles streams through the MiniBooNE detector. This experiment tests the degree to which neutrinos shift from one "flavor" to another. Each neutrino normally travels as a mixture

108

Neutrino oscillations in matter  

Microsoft Academic Search

The effect of coherent forward scattering must be taken into account when considering the oscillations of neutrinos traveling through matter. In particular, for the case of massless neutrinos for which vacuum oscillations cannot occur, oscillations can occur in matter if the neutral current has an off-diagonal piece connecting different neutrino types. Applications discussed are solar neutrinos and a proposed experiment

L. Wolfenstein

1978-01-01

109

Underground neutrino astronomy  

SciTech Connect

A review is made of possible astronomical neutrino sources detectable with underground facilities. Comments are made about solar neutrinos and gravitational-collapse neutrinos, and particular emphasis is placed on ultra-high-energy astronomical neutrino sources. An appendix mentions the exotic possibility of monopolonium.

Schramm, D.N.

1983-02-01

110

The cosmic neutrino background  

NASA Technical Reports Server (NTRS)

The cosmic neutrino background is expected to consist of relic neutrinos from the big bang, of neutrinos produced during nuclear burning in stars, of neutrinos released by gravitational stellar collapse, and of neutrinos produced by cosmic ray interactions with matter and radiation in the interstellar and intergalactic medium. Formation of baryonic dark matter in the early universe, matter-antimatter annihilation in a baryonic symmetric universe, and dark matter annihilation could have also contributed significantly to the cosmic neutrino background. The purpose of this paper is to review the properties of these cosmic neutrino backgrounds, the indirect evidence for their existence, and the prospects for their detection.

Dar, Arnon

1991-01-01

111

Cosmic neutrino cascades from secret neutrino interactions  

NASA Astrophysics Data System (ADS)

The first detection of high-energy astrophysical neutrinos by IceCube provides new opportunities for tests of neutrino properties. The long baseline through the cosmic neutrino background (C?B) is particularly useful for directly testing secret neutrino interactions (?SI) that would cause neutrino-neutrino elastic scattering at a larger rate than the usual weak interactions. We show that IceCube can provide competitive sensitivity to ?SI compared to other astrophysical and cosmological probes, which are complementary to laboratory tests. We study the spectral distortions caused by ?SI with a large s-channel contribution, which can lead to a dip, bump, or cutoff on an initially smooth spectrum. Consequently, ?SI may be an exotic solution for features seen in the IceCube energy spectrum. More conservatively, IceCube neutrino data could be used to set model-independent limits on ?SI. Our phenomenological estimates provide guidance for more detailed calculations, comparisons to data, and model building.

Ng, Kenny C. Y.; Beacom, John F.

2014-09-01

112

Light right-handed neutrinos: + an incursion in cosmology  

E-print Network

Light right-handed neutrinos: why not? + an incursion in cosmology R. Barbieri "Neutrinos in Venice to include neutrino masses L(!-mass) = Li"! i jNjv+NiMi jNj L(!-mass) = (!T NT ) 0 "v "vM ! N with , N each 3-vectors and , M 3x3 matrices 3 alternatives for the light neutrinos: 1 - 3 light Majorana neu's ( M large

Abbondandolo, Alberto

113

Neutrino electromagnetic interactions: a window to new physics  

E-print Network

We review the theory and phenomenology of neutrino electromagnetic interactions, which give us powerful tools to probe the physics beyond the Standard Model. After a derivation of the general structure of the electromagnetic interactions of Dirac and Majorana neutrinos in the one-photon approximation, we discuss the effects of neutrino electromagnetic interactions in terrestrial experiments and in astrophysical environments. We present the experimental bounds on neutrino electromagnetic properties and we confront them with the predictions of theories beyond the Standard Model.

Carlo Giunti; Alexander Studenikin

2014-03-25

114

Relic neutrino absorption spectroscopy  

NASA Astrophysics Data System (ADS)

Resonant annihilation of extremely high-energy cosmic neutrinos on big-bang relic anti-neutrinos (and vice versa) into Z bosons leads to sizable absorption dips in the neutrino flux to be observed at Earth. The high-energy edges of these dips are fixed, via the resonance energies, by the neutrino masses alone. Their depths are determined by the cosmic neutrino background density, by the cosmological parameters determining the expansion rate of the Universe, and by the large redshift history of the cosmic neutrino sources. We investigate the possibility of determining the existence of the cosmic neutrino background within the next decade from a measurement of these absorption dips in the neutrino flux. As a by-product, we study the prospects to infer the absolute neutrino mass scale. We find that, with the presently planned neutrino detectors (ANITA, Auger, EUSO, OWL, RICE, and SalSA) operating in the relevant energy regime above 1021 eV, relic neutrino absorption spectroscopy becomes a realistic possibility. It requires, however, the existence of extremely powerful neutrino sources, which should be opaque to nucleons and high-energy photons to evade present constraints. Furthermore, the neutrino mass spectrum must be quasidegenerate to optimize the dip, which implies m??0.1 eV for the lightest neutrino. With a second generation of neutrino detectors, these demanding requirements can be relaxed considerably.

Eberle, Birgit; Ringwald, Andreas; Song, Liguo; Weiler, Thomas J.

2004-07-01

115

Measuring anisotropies in the cosmic neutrino background  

NASA Astrophysics Data System (ADS)

Neutrino capture on tritium has emerged as a promising method for detecting the cosmic neutrino background (C ? B ). We show that relic neutrinos are captured most readily when their spin vectors are antialigned with the polarization axis of the tritium nuclei and when they approach along the direction of polarization. As a result, C ? B observatories may measure anisotropies in the cosmic neutrino velocity and spin distributions by polarizing the tritium targets. A small dipole anisotropy in the C ? B is expected due to the peculiar velocity of the lab frame with respect to the cosmic frame and due to late-time gravitational effects. The PTOLEMY experiment, a tritium observatory currently under construction, should observe a nearly isotropic background. This would serve as a strong test of the cosmological origin of a potential signal. The polarized-target measurements may also constrain nonstandard neutrino interactions that would induce larger anisotropies and help discriminate between Majorana versus Dirac neutrinos.

Lisanti, Mariangela; Safdi, Benjamin R.; Tully, Christopher G.

2014-10-01

116

a Neutrino Mass Model with Reflection Symmetry  

NASA Astrophysics Data System (ADS)

We demonstrate that an SU(2)L×U(1)Y model with the same particle content as Standard Model (SM) and discrete reflection symmetry between second and third generations of leptons gives rise to charged lepton and neutrino mass matrices which can accommodate the present solar, atmospheric, WMAP neutrino experimental results. The model predicts the value of |U13| which could be tested in neutrino factories and the effective Majorana neutrino mass which is at the lower end of the present experimental value. Neutrino masses are generated through dim=5 operators and the scale of which are constrained by the value of . If, in future neutrinoless double beta decay experiments namely, MOON, EXO, GENIUS shift the lower bound on by one order, the present model will fail to accommodate the solar neutrino mixing angle due to LMA solution.

Ghosal, Ambar

117

Discriminating Neutrino See-Saw Models  

E-print Network

We consider how well current theories can predict neutrino mass and mixing parameters, and construct a statistical discriminator which allows us to compare different models to each other. As an example we consider see-saw models based on family symmetry, and single right-handed neutrino dominance, and compare them to each other and to the case of neutrino anarchy with random entries in the neutrino Yukawa and Majorana mass matrices. The predictions depend crucially on the range of the undetermined coefficients over which we scan, and we speculate on how future theories might lead to more precise predictions for the coefficients and hence for neutrino observables. Our results indicate how accurately neutrino masses and mixing angles need to be measured by future experiments in order to discriminate between current models.

M. Hirsch; S. F. King

2001-02-08

118

A See-Saw Mechanism with light sterile neutrinos  

E-print Network

The usual see-saw mechanism for the generation of light neutrino masses is based on the assumption that all of the flavours of right-handed (more properly, sterile) neutrinos are heavy. If the sterile Majorana mass matrix is singular, one or more of the sterile neutrinos will have zero mass before mixing with the active (left-handed) neutrinos and be light after that mixing is introduced. In particular, a rank 1 sterile mass matrix leads naturally to two pseudo-Dirac pairs, one very light active Majorana neutrino and one heavy sterile Majorana neutrino. For any pattern of Dirac masses, there exists a region of parameter space in which the two pseudo-Dirac pairs are nearly degenerate in mass. This, in turn, leads to large amplitude mixing of active states as well as mixing into sterile states.

B. H. J. McKellar; G. J. Stephenson Jr; T. Goldman; M. Garbutt

2001-06-12

119

Neutrino magnetic moments, flavor mixing, and the SuperKamiokande solar data  

E-print Network

We find that magnetic neutrino-electron scattering is unaffected by oscillations for vacuum mixing of Dirac neutrinos with only diagonal moments and for Majorana neutrinos with two flavors. For MSW mixing, these cases again obtain, though the effective moments can depend on the neutrino energy. Thus, e.g., the magnetic moments measured with $\\bar{\

J. F. Beacom; P. Vogel

1999-10-25

120

The Neutrino and the SNP  

NSDL National Science Digital Library

This site from the Sudbury Neutrino Observatory provides an explanation of neutrinos and of the former discrepancy between theoretical models and solar neutrino data known as the Solar Neutrino Problem (SNP). The site contains a brief history of the study of neutrinos, a graph of the solar neutrinos spectrum, and a discussion of their flux. The role of the Sudbury Neutrino Observatory in collecting neutrinos data is also presented.

2006-12-03

121

Solar Neutrinos: History  

NSDL National Science Digital Library

This site, authored by John Bahcall of the School of Natural Sciences, offers several articles about neutrinos, the neutrino oscillations, and the sun. The page is structured in this fashion: a historical overview of solar models, a theoretical description of solar neutrinos, an experimental description of solar neutrinos, an explanation of how the sun shines, and the evolution of neutrino astronomy. The page links users to pdfs of useful papers concerning these topics. This is a useful resource for those looking for a comprehensive history of solar neutrinos.

Bahcall, John

2009-04-15

122

Neutrino Nucleosynthesis in Supernovae  

SciTech Connect

Neutrino nucleosynthesis is an important synthesis process for light elements in supernovae. One important physics input of neutrino nucleosynthesis is cross sections of neutrino-nucleus reactions. The cross sections of neutrino-{sup 12}C and {sup 4}He reactions are derived using new shell model Hamiltonians. With the new cross sections, light element synthesis of a supernova is investigated. The appropriate range of the neutrino temperature for supernovae is constrained to be between 4.3 MeV and 6.5 MeV from the {sup 11}B abundance in Galactic chemical evolution. Effects by neutrino oscillations are also discussed.

Yoshida, Takashi [Division of Theoretical Astronomy, National Astronomical Observatory of Japan (Japan); Suzuki, Toshio [Department of Physics, College of Humanities and Sciences, Nihon University (Japan); Chiba, Satoshi [Advanced Science Research Center, Japan Atomic Energy Agency (Japan); Kajino, Toshitaka [Division of Theoretical Astronomy, National Astronomical Observatory of Japan (Japan); Department of Astronomy, Graduate School of Science, University of Tokyo (Japan); Yokomakura, Hidekazu; Kimura, Keiichi [Department of Physics, Graduate School of Science, Nagoya University (Japan); Takamura, Akira [Department of Mathematics, Toyota National College of Technology (Japan); Hartmann, Dieter H. [Department of Physics and Astronomy, Clemson University (United States)

2009-05-04

123

Neutrinos in Physics and Astrophysics  

Microsoft Academic Search

The observed flavor oscillations of solar and atmospheric neutrinos determine several elements of the leptonic mixing matrix, but leave open the small mixing angle Theta13, a possible CP-violating phase, the mass ordering, the absolute mass scale mnu,and the Dirac vs. Majorana property. Progress will be made by long-baseline, tritium endpoint, and 2beta decay experiments. The best constraint on mnu obtains

Georg G. Raffelt

2003-01-01

124

Relic neutrinos: neutrino properties from cosmology  

E-print Network

After a short introduction on the predicted cosmic neutrino background in the universe, we review some of the cosmological bounds related to neutrinos. In particular we show how the recent data on the anisotropies of the cosmic microwave background radiation from the WMAP satellite, combined with other experimental results, can constrain the radiation content of the universal energy density and the sum of neutrino masses.

Sergio Pastor

2003-06-24

125

Revisiting pseudo-Dirac neutrinos  

NASA Astrophysics Data System (ADS)

We study the pseudo-Dirac mixing of left- and right-handed neutrinos in the case where the Majorana masses ML and MR are small when compared with the Dirac mass, MD. The light Majorana masses could be generated by a non-renormalizable operator reflecting effects of new physics at some high energy scale. In this context, we obtain a simple model independent closed bound for MD. A phenomenologically consistent scenario is achieved with ML,MR~=10-7 eV and MD~=10-5-10-4 eV. This precludes the possibility of positive mass searches in the planned future experiments like GENIUS or in tritium decay experiments. If on the other hand, GENIUS does observe a positive signal for a Majorana mass >=10-3 eV, then with very little fine tuning of neutrino parameters, the scale of new physics could be in the TeV range, but pseudo-Dirac scenario in that case is excluded. We briefly discuss the constraints from cosmology when a fraction of the dark matter is composed of nearly degenerate neutrinos.

Balaji, K. R. S.; Kalliomäki, Anna; Maalampi, Jukka

2002-01-01

126

PREFACE: Nobel Symposium 129 on Neutrino Physics  

NASA Astrophysics Data System (ADS)

Nobel Symposium 129 on Neutrino Physics was held at Haga Slott in Enköping, Sweden during August 19 24, 2004. Invited to the symposium were around 40 globally leading researchers in the field of neutrino physics, both experimental and theoretical. In addition to these participants, some 30 local researchers and graduate students participated in the symposium. The dominant theme of the lectures was neutrino oscillations, which after several years were recently verified by results from the Super-Kamiokande detector in Kamioka, Japan and the SNO detector in Sudbury, Canada. Discussion focused especially on effects of neutrino oscillations derived from the presence of matter and the fact that three different neutrinos exist. Since neutrino oscillations imply that neutrinos have mass, this is the first experimental observation that fundamentally deviates from the standard model of particle physics. This is a challenge to both theoretical and experimental physics. The various oscillation parameters will be determined with increased precision in new, specially designed experiments. Theoretical physics is working intensively to insert the knowledge that neutrinos have mass into the theoretical models that describe particle physics. It will probably turn out that the discovery of neutrino oscillations signifies a breakthrough in the description of the very smallest constituents of matter. The lectures provided a very good description of the intensive situation in the field right now. The topics discussed also included mass models for neutrinos, neutrinos in extra dimensions as well as the `seesaw mechanism', which provides a good description of why neutrino masses are so small. Also discussed, besides neutrino oscillations, was the new field of neutrino astronomy. Among the questions that neutrino astronomy hopes to answer are what the dark matter in the Universe consists of and where cosmic radiation at extremely high energies comes from. For this purpose, large neutrino telescopes are built deep in the Antarctic ice, in the Baikal Lake, and in the Mediterranean Sea. Among prominent unanswered questions, highlighted as one of the most important, was whether neutrinos are Dirac or Majorana particles. By studying neutrino double beta decay, researchers hope to answer this question, but it will put very large demands on detectors. The programme also included ample time for lively and valuable discussions, which cannot normally be held at ordinary conferences. The symposium concluded with a round-table discussion, where participants discussed the future of neutrino physics.Without a doubt, neutrino physics today is moving toward a very exciting and interesting period. An important contribution to the success of the symposium was the wonderful setting that the Haga Slott manor house hotel and conference center offered to the participants.

Bergström, Lars; Botner, Olga; Carlson, Per; Hulth, Per Olof; Ohlsson, Tommy

2005-01-01

127

Astroparticle physics with solar neutrinos  

PubMed Central

Solar neutrino experiments observed fluxes smaller than the expectations from the standard solar model. This discrepancy is known as the “solar neutrino problem”. Flux measurements by Super-Kamiokande and SNO have demonstrated that the solar neutrino problem is due to neutrino oscillations. Combining the results of all solar neutrino experiments, parameters for solar neutrino oscillations are obtained. Correcting for the effect of neutrino oscillations, the observed neutrino fluxes are consistent with the prediction from the standard solar model. In this article, results of solar neutrino experiments are reviewed with detailed descriptions of what Kamiokande and Super-Kamiokande have contributed to the history of astroparticle physics with solar neutrino measurements. PMID:21558758

NAKAHATA, Masayuki

2011-01-01

128

Neutrino mixing scenarios and AGN  

E-print Network

Active galactic nuclei (AGN) have been suggested to be sources of very high energy neutrinos. We consider the possibility of using AGN neutrinos to test neutrino mixings. From the atmospheric, solar and laboratory data on neutrino oscillations we derive the flavour composition of the AGN neutrino flux in different neutrino mixing schemes. We show that most of the schemes considered can be distinguished from each other and the existence of a sterile neutrino can be specially tested. AGN neutrinos can also be used to test those four-neutrino scenarios where solar neutrinos oscillate into an arbitrary mixture of $\

Luis Bento; Petteri Keränen; Jukka Maalampi

2000-02-01

129

The Neutrino Underground  

NSF Publications Database

... the facility that produces the neutrino beam at the Fermi National Accelerator Laboratory in Batavia ... detector at Fermilab, will monitor the neutrino beam as it heads outward. The other, the 6,000-ton ...

130

Neutrino Oscillation Physics  

SciTech Connect

To complement the neutrino-physics lectures given at the 2011 International School on Astro Particle Physics devoted to Neutrino Physics and Astrophysics (ISAPP 2011; Varenna, Italy), at the 2011 European School of High Energy Physics (ESHEP 2011; Cheila Gradistei, Romania), and, in modified form, at other summer schools, we present here a written description of the physics of neutrino oscillation. This description is centered on a new way of deriving the oscillation probability. We also provide a brief guide to references relevant to topics other than neutrino oscillation that were covered in the lectures. Neutrinos and photons are by far the most abundant elementary particles in the universe. Thus, if we would like to comprehend the universe, we must understand the neutrinos. Of course, studying the neutrinos is challenging, since the only known forces through which these electrically-neutral leptons interact are the weak force and gravity. Consequently, interactions of neutrinos in a detector are very rare events, so that very large detectors and intense neutrino sources are needed to make experiments feasible. Nevertheless, we have confirmed that the weak interactions of neutrinos are correctly described by the Standard Model (SM) of elementary particle physics. Moreover, in the last 14 years, we have discovered that neutrinos have nonzero masses, and that leptons mix. These discoveries have been based on the observation that neutrinos can change from one 'flavor' to another - the phenomenon known as neutrino oscillation. We shall explain the physics of neutrino oscillation, deriving the probability of oscillation in a new way. We shall also provide a very brief guide to references that can be used to study some major neutrino-physics topics other than neutrino oscillation.

Kayser, Boris

2012-06-01

131

Geo-neutrino Observation  

SciTech Connect

Observations of geo-neutrinos measure radiogenic heat production within the earth, providing information on the thermal history and dynamic processes of the mantle. Two detectors currently observe geo-neutrinos from underground locations. Other detection projects in various stages of development include a deep ocean observatory. This paper presents the current status of geo-neutrino observation and describes the scientific capabilities of the deep ocean observatory, with emphasis on geology and neutrino physics.

Dye, S. T. [University of Hawaii at Manoa, Honolulu, Hawaii 96822 (United States); Hawaii Pacific University, Kaneohe, Hawaii 96744 (United States); Alderman, M.; Batygov, M.; Learned, J. G.; Matsuno, S.; Mahoney, J. M.; Pakvasa, S.; Rosen, M.; Smith, S.; Varner, G. [University of Hawaii at Manoa, Honolulu, Hawaii 96822 (United States); McDonough, W. F. [University of Maryland, College Park, Maryland 20742 (United States)

2009-12-17

132

The Sudbury Neutrino Observatory  

Microsoft Academic Search

The Sudbury Neutrino Observatory is a second-generation water Cherenkov detector designed to determine whether the currently observed solar neutrino deficit is a result of neutrino oscillations. The detector is unique in its use of D2O as a detection medium, permitting it to make a solar model-independent test of the neutrino oscillation hypothesis by comparison of the charged- and neutral-current interaction

J Boger; R. L Hahn; J. K Rowley; A. L Carter; B Hollebone; D Kessler; I Blevis; F Dalnoki-Veress; A DeKok; J Farine; D. R Grant; C. K Hargrove; G Laberge; I Levine; K McFarlane; H Mes; A. T Noble; V. M Novikov; M O'Neill; M Shatkay; C Shewchuk; D Sinclair; E. T. H Clifford; R Deal; E. D Earle; E Gaudette; G Milton; B Sur; J Bigu; J. H. M Cowan; D. L Cluff; E. D Hallman; R. U Haq; J Hewett; J. G Hykawy; G Jonkmans; R Michaud; A Roberge; J Roberts; E Saettler; M. H Schwendener; H Seifert; D Sweezey; R Tafirout; C. J Virtue; D. N Beck; Y. D Chan; X Chen; M. R Dragowsky; F. W Dycus; J Gonzalez; M. C. P Isaac; Y Kajiyama; G. W Koehler; K. T Lesko; M. C Moebus; E. B Norman; C. E Okada; A. W. P Poon; P Purgalis; A Schuelke; A. R Smith; R. G Stokstad; S Turner; I Zlimen; J. M Anaya; T. J Bowles; S. J Brice; Ernst-Ingo Esch; M. M Fowler; Azriel Goldschmidt; A Hime; A. F McGirt; G. G Miller; W. A Teasdale; J. B Wilhelmy; J. M Wouters; J. D Anglin; M Bercovitch; W. F Davidson; R. S Storey; S Biller; R. A Black; R. J Boardman; M. G Bowler; J Cameron; B Cleveland; A. P Ferraris; G Doucas; H Heron; C Howard; N. A Jelley; A. B Knox; M Lay; W Locke; J Lyon; S Majerus; M Moorhead; M Omori; N. W Tanner; R. K Taplin; M Thorman; D. L Wark; J. C Barton; P. T Trent; R Kouzes; M. M Lowry; A. L Bell; E Bonvin; M Boulay; M Dayon; F Duncan; L. S Erhardt; H. C Evans; G. T Ewan; R Ford; A Hallin; A Hamer; P. M Hart; P. J Harvey; D Haslip; C. A. W Hearns; R Heaton; J. D Hepburn; C. J Jillings; E. P Korpach; H. W Lee; J. R Leslie; M.-Q Liu; H. B Mak; A. B McDonald; J. D MacArthur; W McLatchie; B. A Moffat; S Noel; T. J Radcliffe; B. C Robertson; P Skensved; R. L Stevenson; X Zhu; S Gil; J Heise; R. L Helmer; R. J Komar; C. W Nally; H. S Ng; C. E Waltham; R. C Allen; G Bühler; H. H Chen; G Aardsma; T Andersen; K Cameron; M. C Chon; R. H Hanson; P Jagam; J Karn; J Law; R. W Ollerhead; J. J Simpson; N Tagg; J.-X Wang; C Alexander; E. W Beier; J. C Cook; D. F Cowen; E. D Frank; W Frati; P. T Keener; J. R Klein; G Mayers; D. S McDonald; M. S Neubauer; F. M Newcomer; R. J Pearce; R. G. Van de Water; R. Van Berg; P Wittich; Q. R Ahmad; J. M Beck; M. C Browne; T. H Burritt; P. J Doe; C. A Duba; S. R Elliott; J. E Franklin; J. V Germani; P Green; A. A Hamian; K. M Heeger; M Howe; R. Meijer Drees; A Myers; R. G. H Robertson; M. W. E Smith; T. D Steiger; T. Van Wechel; J. F Wilkerson

2000-01-01

133

Atmospheric Neutrinos in SNO  

NASA Astrophysics Data System (ADS)

The Sudbury Neutrino Observatory (SNO) was designed primarily to detect solar neutrinos. Its detection of atmospheric neutrinos, however, will be a nice bonus, providing an independent flux measurement in a geomagnetic environment very different from SuperKamiokande. This talk will provide a brief overview of atmospheric neutrino detection in SNO, including the advantages that come from being 2 km underground, as well as further detail on what we expect to see and some of what has been seen so far.

Nally, Christian

2000-05-01

134

NOVA: Hunting Solar Neutrinos  

NSDL National Science Digital Library

Check out this NOVA site for an interview with the late astrophysicist John Bahcall, who produced a detailed theory of solar neutrino emission. In the interview he describes his decades-long effort to reconcile the differences between his theory and solar neutrino measurements and the eventual resolution. The site also includes photographs and links to more information about neutrinos.

2006-12-01

135

Solar Neutrinos Kamioka Observatory  

E-print Network

Solar Neutrinos Y. Suzuki Kamioka Observatory Institute for Cosmic Ray Research University of Tokyo Higashi-Mozumi, Kamioka Gifu 506-1205, Japan 1 Introduction We now recognize that neutrinos have #12;nite masses. In 1998, the Super-Kamiokande experiment found evidence for the atmospheric neutrino oscillation

Tokyo, University of

136

Neutrino Magnetic Moment  

E-print Network

Current experimental and observational limits on the neutrino magnetic moment are reviewed. Implications of the recent results from the solar and reactor neutrino experiments for the value of the neutrino magnetic moment are discussed. It is shown that spin-flavor precession in the Sun is suppressed.

A. B. Balantekin

2006-01-13

137

Neutrino Astronomy Scott Wilbur  

E-print Network

V protons, which should be created with neutrinos, have been seen Can be used to observe possible dark Particle Physics Extremely long baseline for neutrino oscillation studies Dark Matter Searches Many dark Detector Picture from AMANDA II Web Site: http://www.amanda.uci.edu #12;Advantages of Neutrino Astronomy

Golwala, Sunil

138

Neutrino oscillations and neutrino-electron scattering  

SciTech Connect

Neutrino flavor oscillations can significantly alter the cross section for neutrino-electron scattering. As a result, such oscillations can affect the comparison between existing reactor data and theories of neutral-current processes. They may also lead to strikingly large effects in high-energy accelerator experiments.

Kayser, B.; Rosen, S.P.

1980-10-01

139

Neutrino observations from the Sudbury Neutrino Observatory  

SciTech Connect

The Sudbury Neutrino Observatory (SNO) is a water imaging Cherenkov detector. Its usage of 1000 metric tons of D{sub 2}O as target allows the SNO detector to make a solar-model independent test of the neutrino oscillation hypothesis by simultaneously measuring the solar {nu}{sub e} flux and the total flux of all active neutrino species. Solar neutrinos from the decay of {sup 8}B have been detected at SNO by the charged-current (CC) interaction on the deuteron and by the elastic scattering (ES) of electrons. While the CC reaction is sensitive exclusively to {nu}{sub e}, the ES reaction also has a small sensitivity to {nu}{sub {mu}} and {nu}{sub {tau}}. In this paper, recent solar neutrino results from the SNO experiment are presented. It is demonstrated that the solar flux from {sup 8}B decay as measured from the ES reaction rate under the no-oscillation assumption is consistent with the high precision ES measurement by the Super-Kamiokande experiment. The {nu}{sub e} flux deduced from the CC reaction rate in SNO differs from the Super-Kamiokande ES results by 3.3{sigma}. This is evidence for an active neutrino component, in additional to {nu}{sub e}, in the solar neutrino flux. These results also allow the first experimental determination of the total active {sup 8}B neutrino flux from the Sun, and is found to be in good agreement with solar model predictions.

Ahmad, Q.R.; Allen, R.C.; Andersen, T.C.; Anglin, J.D.; Barton,J.C.; Beier, E.W.; Bercovitch, M.; Bigu, J.; Biller, S.D.; Black, R.A.; Blevis, I.; Boardman, R.J.; Boger, J.; Bonvin, E.; Boulay, M.G.; Bowler,M.G.; Bowles, T.J.; Brice, S.J.; Browne, M.C.; Bullard, T.V.; Buhler, G.; Cameron, J.; Chan, Y.D.; Chen, H.H.; Chen, M.; Chen, X.; Cleveland, B.T.; Clifford, E.T.H.; Cowan, J.H.M.; Cowen, D.F.; Cox, G.A.; Dai, X.; Dalnoki-Veress, F.; Davidson, W.F.; Doe, P.J.; Doucas, G.; Dragowsky,M.R.; Duba, C.A.; Duncan, F.A.; Dunford, M.; Dunmore, J.A.; Earle, E.D.; Elliott, S.R.; Evans, H.C.; Ewan, G.T.; Farine, J.; Fergani, H.; Ferraris, A.P.; Ford, R.J.; Formaggio, J.A.; Fowler, M.M.; Frame, K.; Frank, E.D.; Frati, W.; Gagnon, N.; Germani, J.V.; Gil, S.; Graham, K.; Grant, D.R.; Hahn, R.L.; Hallin, A.L.; Hallman, E.D.; Hamer, A.S.; Hamian, A.A.; Handler, W.B.; Haq, R.U.; Hargrove, C.K.; Harvey, P.J.; Hazama, R.; Heeger, K.M.; Heintzelman, W.J.; Heise, J.; Helmer, R.L.; Hepburn, J.D.; Heron, H.; Hewett, J.; Hime, A.; Hykawy, J.G.; Isaac,M.C.P.; Jagam, P.; Jelley, N.A.; Jillings, C.; Jonkmans, G.; Kazkaz, K.; Keener, P.T.; Klein, J.R.; Knox, A.B.; Komar, R.J.; Kouzes, R.; Kutter,T.; Kyba, C.C.M.; Law, J.; Lawson, I.T.; Lay, M.; Lee, H.W.; Lesko, K.T.; Leslie, J.R.; Levine, I.; Locke, W.; Luoma, S.; Lyon, J.; Majerus, S.; Mak, H.B.; Maneira, J.; Manor, J.; Marino, A.D.; McCauley, N.; McDonald,D.S.; McDonald, A.B.; McFarlane, K.; McGregor, G.; Meijer, R.; Mifflin,C.; Miller, G.G.; Milton, G.; Moffat, B.A.; Moorhead, M.; Nally, C.W.; Neubauer, M.S.; Newcomer, F.M.; Ng, H.S.; Noble, A.J.; Norman, E.B.; Novikov, V.M.; O'Neill, M.; Okada, C.E.; Ollerhead, R.W.; Omori, M.; Orrell, J.L.; Oser, S.M.; Poon, A.W.P.; Radcliffe, T.J.; Roberge, A.; Robertson, B.C.; Robertson, R.G.H.; Rosendahl, S.S.E.; Rowley, J.K.; Rusu, V.L.; Saettler, E.; Schaffer, K.K.; Schwendener,M.H.; Schulke, A.; Seifert, H.; Shatkay, M.; Simpson, J.J.; Sims, C.J.; et al.

2001-09-24

140

Neutrinoless Double Beta Decay and Neutrino Oscillations  

NASA Astrophysics Data System (ADS)

Double beta decay is indispensable to solve the question of the neutrino mass matrix together with ? oscillation experiments. Recent analysis of the most sensitive experiment since eight years - the HEIDELBERG-MOSCOW experiment in Gran-Sasso - yields an evidence for the neutrinoless decay mode. This result is the first evidence for lepton number violation and proves the neutrino to be a Majorana particle. We give the present status of the analysis in these Proceedings. It excludes several of the neutrino mass scenarios allowed from present neutrino oscillation experiments - only degenerate and inverse hierarchy mass scenarios survive. This result allows neutrinos to still play an important role as dark matter in the Universe. To improve the present accuracy, considerably enlarged experiments are required, such as GENIUS. A GENIUS Test Facility has just been funded and will come into operation by end of 2002.

Klapdor-Kleingrothaus, H. V.

2002-12-01

141

Low Temperature Detectors for Neutrino Physics  

NASA Astrophysics Data System (ADS)

Recent years have witnessed many exciting breakthroughs in neutrino physics. The detection of neutrino oscillations has proved that neutrinos are massive particles but the assessment of their absolute mass scale is still an outstanding challenge in today particle physics and cosmology. Due to their abundance as big-bang relics, massive neutrinos strongly affect the large-scale structure and dynamics of the universe. In addition, the knowledge of the scale of neutrino masses, together with their hierarchy pattern, is invaluable to clarify the origin of fermion masses beyond the Higgs mechanism. The mass hierarchy is not the only missing piece in the puzzle. Theories of neutrino mass generation call into play Majorana neutrinos and there are experimental observations pointing to the existence of sterile neutrinos in addition to the three ones weakly interacting. Since low temperature detectors were first proposed for neutrino physics experiments in 1984, there have been impressive technical progresses: today this technique offers the high energy resolution and scalability required for leading edges and competitive experiments addressing the still open questions.

Nucciotti, A.

2014-09-01

142

New Results on Neutrino Magnetic Moments and on Democratic Neutrinos  

E-print Network

I discuss the two separate issues on neutrino physics. First, the new bounds on tensorial couplings of neutrinos to charged fermions from the existing limits on neutrino transition magnetic moments. Second, explanation of the atmospheric and solar neutrino data in the democratic neutrino theory with only one free parameter (in the leading order), using the effect of incoherence.

Dmitry Zhuridov

2014-05-08

143

Neutrinos and Mass  

NSDL National Science Digital Library

This week's In the News highlights neutrinos and the recent discovery that neutrinos have mass -- a discovery that has forced physicists to rethink the behavior of elementary particles. The seven resources provided discuss various aspects of the topic. First hypothesized by Wolfgang Pauli in 1931, the existence of neutrinos was not proven until 1956, by Drs. Frederick Reines and Clyde Cowan of the Los Alamos National Laboratory. In a collaborative effort between Japan and the US (at the Kamioka Neutrino Observatory), scientists recently reported their findings at a Neutrino Conference in Japan.

Harris, Kathryn L.

144

Mass determination of neutrinos  

NASA Technical Reports Server (NTRS)

A time-energy correlation method has been developed to determine the signature of a nonzero neutrino mass in a small sample of neutrinos detected from a distant source. The method is applied to the Kamiokande II (Hirata et al., 1987) and IMB (Bionta et al., 1987) observations of neutrino bursts from SN 1987A. Using the Kamiokande II data, the neutrino rest mass is estimated at 2.8 + 2.0, - 1.4 eV and the initial neutrino pulse is found to be less than 0.3 sec full width, followed by an emission tail lasting at least 10 sec.

Chiu, Hong-Yee

1988-01-01

145

The Sudbury Neutrino Observatory  

NSDL National Science Digital Library

The size of a ten-story building, 6800 feet underground at the Creighton mine in Ontario; the Sudbury Neutrino Observatory is a telescope built to study neutrinos and the core of the sun. Students can learn how Cherenkov Radiation is produced and used to detect neutrino properties. Scientists can read the newly published paper dealing with the measurement of Total Active 8B Solar Neutrino Flux using NaCl, as well as other published papers and Conference Proceedings. The site also offers illustrations such as neutrinos striking heavy water and the attractive Double-Ring Event.

146

Neutrinos from AGN  

NASA Technical Reports Server (NTRS)

The great penetrating power of neutrinos makes them ideal probe of astrophysical sites and conditions inaccessible to other forms of radiation. These are the centers of stars (collapsing or not) and the centers of Active Galactic Nuclei (AGN). It has been suggested that AGN presented a very promising source of high energy neutrinos, possibly detectable by underwater neutrino detectors. This paper reviews the evolution of ideas concerning the emission of neutrinos from AGN in view of the more recent developments in gamma-ray astronomy and their implications for the neutrino emission from these class of objects.

Kazanas, Demosthenes; White, Nicholas E. (Technical Monitor)

2000-01-01

147

Nucleosynthesis and Neutrinos  

SciTech Connect

Neutrinos play the critical roles in nucleosynthesis of light-to-heavy mass nuclei in core-collapse supernovae. We study the nucleosynthesis induced by neutrino interactions and find suitable average neutrino temperatures in order to explain the observed solar system abundances of several isotopes {sup 7}Li, {sup 11}B, {sup 138}La and {sup 180}Ta. These isotopes are predominantly synthesized by the supernova {nu}-process. We also study the neutrino oscillation effects on their abundances and propose a method to determine the unknown neutrino oscillation parameters, i.e. {theta}{sub 13} and mass hierarchy.

Kajino, Toshitaka [National Astronomical Observatory, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan); Department of Astronomy, Graduate School of Science, University of Tokyo, Hongo 7-3-1, Bunkyo-ku, Tokyo 113-0033 (Japan)

2011-05-06

148

Weighing the neutrino  

NASA Astrophysics Data System (ADS)

We investigate the potential of short-baseline experiments in order to measure the dispersion relation of the (muon) neutrino, with a prospect of eventually measuring the neutrino mass. As a byproduct, the experiment would help to constrain parameters of Lorentz-violating effects in the neutrino sector. The potential of a high-flux laser-accelerated proton beam (e.g., at the upcoming ELI facility), incident on a thick target composed of a light element to produce pions, with a subsequent decay to muons and muon-neutrinos, is discussed. We find a possibility for a muon neutrino mass measurement of unprecedented accuracy.

Jentschura, U. D.; Horváth, D.; Nagy, S.; Nándori, I.; Trócsányi, Z.; Ujvári, B.

2014-02-01

149

Supernova Neutrino Detection  

E-print Network

A core-collapse supernova will produce an enormous burst of neutrinos of all flavors in the few-tens-of-MeV range. Measurement of the flavor, time and energy structure of a nearby core-collapse neutrino burst will yield answers to many physics and astrophysics questions. The neutrinos left over from past cosmic supernovae are also observable, and their detection will improve knowledge of core collapse rates and average neutrino emission. This review describes experimental techniques for detection of core-collapse neutrinos, as well as the sensitivities of current and future detectors.

Kate Scholberg

2012-05-27

150

Effects of nonzero neutrino masses on black hole evaporation  

E-print Network

We study the consequences of nonzero neutrino masses for black holes evaporating by the emission of Hawking radiation. We find that the evolution of small, hot, black holes may be unaffected (if neutrinos are Majorana particles), or may show an increase in neutrino luminosity and a decrease in lifetime by up to a factor of 1.85 (if neutrinos are Dirac particles). However, for sufficiently large (e.g., stellar mass) black holes, neutrino emission is largely or entirely suppressed, resulting in a decrease in emitted power and an increase in lifetime by up to a factor of 7.5.

Daniel Bambeck; William A. Hiscock

2005-06-08

151

Effect of transition magnetic moments on collective supernova neutrino oscillations  

SciTech Connect

We study the effect of Majorana transition magnetic moments on the flavor evolution of neutrinos and antineutrinos inside the core of Type-II supernova explosions. We find non-trivial collective oscillation effects relating neutrinos and antineutrinos of different flavors, even if one restricts the discussion to Majorana transition electromagnetic moment values that are not much larger than those expected from standard model interactions and nonzero neutrino Majorana masses. This appears to be, to the best of our knowledge, the only potentially observable phenomenon sensitive to such small values of Majorana transition magnetic moments. We briefly comment on the effect of Dirac transition magnetic moments and on the consequences of our results for future observations of the flux of neutrinos of different flavors from a nearby supernova explosion.

Gouvêa, André de; Shalgar, Shashank, E-mail: degouvea@northwestern.edu, E-mail: shashank@northwestern.edu [Department of Physics and Astronomy, Northwestern University, Evanston IL 60208-3112 (United States)

2012-10-01

152

Democratic Neutrino Theory  

E-print Network

New theory of neutrino masses and mixing is introduced. This theory is based on a simple S_3 symmetric democratic neutrino mass matrix, and predicts the neutrino mass spectrum of normal ordering. Taking into account the matter effect and proper averaging of the oscillations, this theory agrees with the variety of atmospheric, solar and accelerator neutrino data. Moreover, the absolute scale of the neutrino masses m of 0.03 eV is determined in this theory, using the atmospheric neutrino oscillation data. In case of tiny perturbations in the democratic mass matrix only one this scale parameter m allows to explain the mentioned above neutrino results, and the theory has huge predictive power.

Dmitry Zhuridov

2014-05-21

153

Properties of neutrinos: Recent results  

SciTech Connect

Recent progress in experimental determinations of the properties of neutrinos is summarized. In particular, the extensive work on direct kinematic measurements of neutrino mass, on neutrino counting and on neutrino oscillations is highlighted. It is concluded that there may already be sufficient information to fix the masses of the neutrinos, but the evidence is still far from convincing. 63 refs., 13 figs.

Robertson, R.G.H.

1987-01-01

154

Effective Theories of Neutrino Masses  

NASA Astrophysics Data System (ADS)

The importance of improving the bounds on those effective non-standard neutrino interactions (NSI) which are a signal of all fermionic-mediated Seesaws is stressed: they are revealed as non-unitarity of the leptonic mixing matrix, and at experimental reach for seesaw scales ? O(TeV). Some recent activity in the literature on other - theoretically not well motivated - ill-constrained NSI are also summarized. Furthermore, the status of the simplest Seesaw scenario with only two heavy neutrinos is reviewed. This model happens to be a explicit realization of the effective Minimal Flavour Violation approach. We derive the scalar potential for the fields whose background values are the Yukawa couplings of that model, and explore its minima. The Majorana character plays a distinctive role: the minimum of the potential allows for large mixing angles - in contrast to the simplest quark case - and predicts a maximal Majorana phase. This points in turn to a strong correlation between neutrino mass hierarchy and mixing pattern.

Gavela, M. B.

2013-02-01

155

Neutrino Dark Energy and Baryon Asymmetry from Higgs Sector  

E-print Network

We propose a new model to explain the neutrino masses, the dark energy and the baryon asymmetry altogether. In this model, neutrinos naturally acquire small Majorana masses via type-II seesaw mechanism, while the pseudo-Nambu-Goldstone bosons associated with the neutrino mass-generation mechanism provide attractive candidates for dark energy. The baryon asymmetry of the universe is produced from the Higgs triplets decay with CP-violation.

Pei-Hong Gu; Hong-Jian He; Utpal Sarkar

2007-04-16

156

Models of Neutrino Masses from Oscillations with Maximal Mixing  

E-print Network

We discuss models of neutrino masses that lead to a large mixing angle for atmospheric neutrino oscillations. In particular we study a mechanism where a simple texture for the Dirac matrix leads to the observed pattern of mixings for a continuous range of Majorana matrices in a reasonably natural way. Both nearly maximal and small mixing solutions for solar neutrinos are compatible with this model. Possible dynamical realizations are discussed and a detailed example in terms of horizontal U(1) charges is presented.

Guido Altarelli; Ferruccio Feruglio

1998-09-30

157

SuperGZK neutrinos  

E-print Network

The sources and fluxes of superGZK neutrinos, $E>10^{20}$ eV, are discussed. The fluxes of {\\em cosmogenic neutrinos}, i.e. those produced by ultra-high energy cosmic rays (UHECR) interacting with CMB photons, are calculated in the models, which give the good fit to the observed flux of UHECR. The best fit given in no-evolutionary model with maximum acceleration energy $E_{\\rm max}=1\\times 10^{21}$ eV results in very low flux of superGZK neutrinos an order of magnitude lower than the observed flux of UHECR. The predicted neutrino flux becomes larger and observable by next generation detectors at energies $10^{20} - 10^{21}$ eV in the evolutionary models with $E_{\\rm max}=1\\times 10^{23}$ eV. The largest cosmogenic neutrino flux is given in models with very flat generation spectrum, e.g. $\\propto E^{-2}$. The neutrino energies are naturally high in the models of {\\em superheavy dark matter and topological defects}. Their fluxes can also be higher than those of cosmogenic neutrinos. The largest fluxes are given by {\\em mirror neutrinos}, oscillating into ordinary neutrinos. Their fluxes obey some theoretical upper limit which is very weak, and in practice these fluxes are most efficiently limited now by observations of radio emission from neutrino-induced showers.

V. Berezinsky

2005-09-22

158

The ideal neutrino beams  

NASA Astrophysics Data System (ADS)

The advance in neutrino oscillation physics is driven by the availability of well characterized and high flux neutrino beams. The three present options for the next generation neutrino oscillation facility are super beams, neutrino factories and beta-beams. A super-beam is a very high intensity classical neutrino beam generated by protons impinging on a target where the neutrinos are generated by the secondary particles decaying in a tunnel down streams of the target. In a neutrino factory the neutrinos are generated from muons decaying in a storage ring with long straight sections pointing towards the detectors. In a beta-beam the neutrinos are also originating from decay in a storage ring but the decaying particles are radioactive ions rather than muons. I will in this presentation review the three options and discuss the pros and cons of each. The present joint design effort for a future high intensity neutrino oscillation in Europe within a common EU supported design study, EURONU, will also be presented. The design study will explore the physics reach, the detectors, the feasibility, the safety issues and the cost for each of the options so that the the community can take a decision on what to build when the facilities presently under exploitation and construction have to be replaced.

Lindroos, Mats

2009-06-01

159

Acquiring information about neutrino parameters by detecting supernova neutrinos  

SciTech Connect

We consider the supernova shock effects, the Mikheyev-Smirnov-Wolfenstein effects, the collective effects, and the Earth matter effects in the detection of type II supernova neutrinos on the Earth. It is found that the event number of supernova neutrinos depends on the neutrino mass hierarchy, the neutrino mixing angle {theta}{sub 13}, and neutrino masses. Therefore, we propose possible methods to identify the mass hierarchy and acquire information about {theta}{sub 13} and neutrino masses by detecting supernova neutrinos. We apply these methods to some current neutrino experiments.

Huang, Ming-Yang; Guo, Xin-Heng [College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875 (China); Young, Bing-Lin [Department of Physics and Astronomy, Iowa State University, Ames, Iowa 5001 (United States); Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing 100190 (China)

2010-08-01

160

Jiangmen Underground Neutrino Observatory  

E-print Network

The Jiangmen Underground Neutrino Observatory (JUNO) is a multipurpose neutrino-oscillation experiment designed to determine the neutrino mass hierarchy and to precisely measure oscillation parameters by detecting reactor antineutrinos, observe supernova neutrinos, study the atmospheric, solar neutrinos and geo-neutrinos, and perform exotic searches, with a 20 kiloton liquid scintillator detector of unprecedented $3\\%$ energy resolution (at 1 MeV) at 700-meter deep underground and to have other rich scientific possibilities. Currently MC study shows a sensitivity of the mass hierarchy to be $\\overline{\\Delta\\chi^2}\\sim 11$ and $\\overline{\\Delta\\chi^2}\\sim 16$ in a relative and an absolute measurement, respectively. JUNO has been approved by Chinese Academy of Sciences in 2013, and an international collaboration was established in 2014. The civil construction is in preparation and the R$\\&$D of the detectors are ongoing. A new offline software framework was developed for the detector simulation, the event ...

He, Miao

2014-01-01

161

Neutrino physics with an intense \  

E-print Network

We study some of the physics potential of an intense $1\\,\\mathrm{MCi}$ $^{51}\\mathrm{Cr}$ source combined with the {\\sc Majorana Demonstrator} enriched germanium detector array. The {\\sc Demonstrator} will consist of detectors with ultra-low radioactive backgrounds and extremely low energy thresholds of~$\\sim 400\\,\\mathrm{eV}$. We show that it can improve the current limit on the neutrino magnetic dipole moment. We briefly discuss physics applications of the charged-current reaction of the $^{51}\\mathrm{Cr} neutrino with the $^{73}\\mathrm{Ge} isotope. Finally, we argue that the rate from a realistic, intense tritium source is below the detectable limit of even a tonne-scale HPGe experiment

R. Henning

2010-11-16

162

Neutrinos: Nature's Ghosts?  

SciTech Connect

Dr. Don Lincoln introduces one of the most fascinating inhabitants of the subatomic realm: the neutrino. Neutrinos are ghosts of the microworld, almost not interacting at all. In this video, he describes some of their properties and how they were discovered. Studies of neutrinos are expected to be performed at many laboratories across the world and to form one of the cornerstones of the Fermilab research program for the next decade or more.

Lincoln, Don

2013-06-18

163

Neutrinos from gravitational collapse  

SciTech Connect

Detailed calculations are made of the neutrino spectra emitted during gravitational collapse events (Type II supernovae). Those aspects of the neutrino signal which are relatively independent of the collapse model and those aspects which are sensitive to model details are discussed. The easier-to-detect high energy tail of the emitted neutrinos has been calculated using the Boltzmann equation which is compared with the result of the traditional multi-group flux limited diffusion calculations. 8 figs., 28 refs.

Mayle, R.; Wilson, J.R.; Schramm, D.N.

1986-05-01

164

Borexino and solar neutrinos  

Microsoft Academic Search

Borexino, a large volume detector for low energy neutrino spectroscopy, is currently running underground at the Laboratori Nazionali del Gran Sasso, Italy. The measured in- teraction rate of the 0.862 MeV 7Be neutrinos equals to 49 3stat 4syst counts\\/(day 100 ton). The hypothesis of no oscillation for 7Be solar neutrinos is inconsistent with the Borexino measurement at the 4 C.L..

I. N. Machulina; C. Arpesella; M. Balata; G. Bellini; J. Benziger; S. Bonetti; A. Brigatti; B. Cac; L. Cadonati; F. Calaprice; C. Carraro; G. Cecchet; A. Chavarria; M. Chen; D. D'Angelo; A. de Bari; A. de Bellefon; A. Derbin; M. Deutsch; A. di Credico; R. Eisenstein; F. Elisei; A. Etenko; R. Fernholz; K. Fomenko; R. Ford; D. Franco; B. Freudiger; C. Galbiati; F. Gatti; S. Gazzana; M. Giammarchi; D. Giugni; M. Goeger; T. Goldbrunner; A. Goretti; C. Grieb; C. Hagner; W. Hampel; E. Harding; S. Hardy; F. X. Hartman; T. Hertrich; G. Heusser; Aldo Ianni; Andrea Ianni; M. Joyce; J. Kiko; T. Kirsten; V. Kobychev; G. Korga; G. Korschinek; D. Kryn; V. Lagomarsino; P. Lamarche; M. Lauben; C. Lendvai; M. Leung; T. Lewke; E. Litvinovich; B. Loer; P. Lombardi; L. Ludhova; I. Machulin; S. Malvezzi; S. Manecki; J. Maneira; W. Maneschg; I. Manno; D. Manuzio; G. Manuzio; A. Martemianov; F. Masetti; U. Mazzucato; K. McCarty; D. McKinsey; Q. Meindl; E. Meroni; L. Miramonti; M. Misiaszek; D. Montanari; M. E. Monzani; V. Muratova; P. Mu; H. Neder; A. Nelson; L. Niedermeier; L. Oberauer; M. Obolensky; M. Orsini; F. Ortica; M. Pallavicini; L. Papp; S. Parmeggiano; L. Perasso; A. Pocar; R. S. Raghavan; G. Ranucci; W. Rau; A. Razeto; E. Resconi; P. Risso; A. Romani; D. Rountree; A. Sabelnikov; R. Sal; C. Salvo; D. Schimizzi; S. Schonert; T. Shutt; H. Simgen; M. Skorokhvatov; O. Smirnov; A. Sonnenschein; A. Sotnikov; S. Sukhotin; Y. Suvorov; R. Tartaglia; G. Testera; D. Vignaud; S. Vitale; R. B. Vogelaar; F. von Feilitzsch; R. von Hentig; T. von Hentig; M. Wojcik; M. Wurm; O. Zaimidoroga; S. Zavatarelli; G. Zuzel

165

Neutrinos in the Electron  

SciTech Connect

I will show that one half of the rest mass of the electron consists of electron neutrinos and that the other half of the rest mass of the electron consists of the mass in the energy of electric oscillations. With this composition we can explain the rest mass of the electron, its charge, its spin and its magnetic moment We have also determined the rest masses of the muon neutrino and the electron neutrino.

Koschmieder, E. L. [Center for Statistical Mechanics, University of Texas at Austin, Austin TX 78712 (United States)

2007-04-28

166

Neutrinos: Nature's Ghosts?  

ScienceCinema

Dr. Don Lincoln introduces one of the most fascinating inhabitants of the subatomic realm: the neutrino. Neutrinos are ghosts of the microworld, almost not interacting at all. In this video, he describes some of their properties and how they were discovered. Studies of neutrinos are expected to be performed at many laboratories across the world and to form one of the cornerstones of the Fermilab research program for the next decade or more.

Lincoln, Don

2014-08-12

167

Bolometric detection of neutrinos  

NASA Technical Reports Server (NTRS)

Elastic neutrino scattering off electrons in crystalline silicon at 1-10 mK results in measurable temperature changes in macroscopic amounts of material, even for low-energy (less than 0.41-MeV) pp neutrinos from the sun. New detectors for bolometric measurement of low-energy neutrino interactions, including coherent nuclear elastic scattering, are proposed. A new and more sensitive search for oscillations of reactor antineutrinos is practical (about 100 kg of Si), and would lay the groundwork for a more ambitious measurement of the spectrum of pp, Be-7, and B-8 solar neutrinos, and of supernovae anywhere in the Galaxy (about 10 tons of Si).

Cabrera, B.; Krauss, L. M.; Wilczek, F.

1985-01-01

168

Multimessenger Astronomy and Neutrinos  

NASA Astrophysics Data System (ADS)

Neutrinos play a very important role in multimessenger astronomy. In this talk, I start with a simple argument on how bright the Universe is in both photons and neutrinos. It is remarkable that one can easily show that the neutrinos, especially those emitted from past core-collapse supernovae, form the brightest radiation component in the Universe, ever emitted from astrophysical sources. The detection of this cosmic supernova neutrino background has not been made yet, but is almost guaranteed in the near future. Thus, I review theoretical predictions of the supernova neutrino background, and the latest upper limits experimentally obtained on its flux. Then I discuss prospects of detecting supernova neutrinos from nearby galaxies. With upcoming Mton detectors, or hopefully with a multi-Mton detector, one could study not only supernova neutrinos but also a true stellar death rate, hidden black-hole formation, etc. Finally, I discuss detectability of high-energy neutrinos and implications for underlying supernova-gamma-ray burst connection. Detecting neutrinos will not only give unique diagnostics but also help find gravitational waves.

Ando, Shin'ichiro

2013-04-01

169

Neutrino Oscillation Physics  

E-print Network

To complement the neutrino-physics lectures given at the 2011 International School on Astro Particle Physics devoted to Neutrino Physics and Astrophysics (ISAPP 2011; Varenna, Italy), at the 2011 European School of High Energy Physics (ESHEP 2011; Cheila Gradistei, Romania), and, in modified form, at other summer schools, we present here a written description of the physics of neutrino oscillation. This description is centered on a new way of deriving the oscillation probability. We also provide a brief guide to references relevant to topics other than neutrino oscillation that were covered in the lectures.

Kayser, Boris

2014-01-01

170

Molybdenum solar neutrino experiment  

SciTech Connect

The goal of the molybdenum solar neutrino experiment is to deduce the /sup 8/B solar neutrino flux, averaged over the past several million years, from the concentration of /sup 98/Tc in a deeply buried molybdenum deposit. The experiment is important to an understanding of stellar processes because it will shed light on the reason for the discrepancy between theory and observation of the chlorine solar neutrino experiment. Possible reasons for the discrepancy may lie in the properties of neutrinos (neutrino oscillations or massive neutrinos) or in deficiencies of the standard solar model. The chlorine experiment only measures the /sup 8/B neutrino flux in current times and does not address possible temporal variations in the interior of the sun, which are also not considered in the standard model. In the molybdenum experiment, we plan to measure /sup 98/Tc (4.2 Myr), also produced by /sup 8/B neutrinos, and possibly /sup 97/Tc (2.6 Myr), produced by lower energy neutrinos.

Wolfsberg, K.; Cowan, G.A.; Bryant, E.A.; Daniels, K.S.; Downey, S.W.; Haxton, W.C.; Niesen, V.G.; Nogar, N.S.; Miller, C.M.; Rokop, D.J.

1984-01-01

171

?-? symmetry, sterile right-handed neutrinos, and leptogenesis  

NASA Astrophysics Data System (ADS)

Leptogenesis is studied in a seesaw model with ?-? symmetry for SUL(2)-singlet right-handed neutrinos. It is shown that lepton asymmetry is not zero and is given by the square of the solar neutrino mass difference and can be of the right order of magnitude. Further it involves the same Majorana phase which appears in the neutrinoless double ?-decay. In this framework one of the right-handed seesaw partners of light neutrinos can be made massless. This can be identified with a sterile neutrino, once it acquires a tiny mass (?1eV) when ?-? symmetry is broken in the right-handed neutrino sector. The above mentioned sterile neutrino together with another one can be identified to explain the MiniBooNE and LSND results. The light 5×5 neutrino mass matrix is completely fixed if CP is conserved and so is the effective mass for neutrinoless double ?-decay.

Riazuddin

2008-01-01

172

Massive neutrinos and invisible axion minimally connected  

E-print Network

We survey a few minimal scalar extensions of the standard electroweak model that provide a simple setup for massive neutrinos in connection with an invisible axion. The presence of a chiral $U(1)$ \\`a la Peccei-Quinn drives the pattern of Majorana neutrino masses while providing a dynamical solution to the strong CP problem and an axion as a dark matter candidate. We paradigmatically apply such a renormalizable framework to type-II seesaw and to two viable models for neutrino oscillations where the neutrino masses arise at one and two loops, respectively. We comment on the naturalness of the effective setups as well as on their implications for vacuum stability and electroweak baryogenesis.

Bertolini, Stefano; Kolešová, Helena; Malinský, Michal

2014-01-01

173

Neutrino Masses and Leptogenesis from Extra Fermions  

NASA Astrophysics Data System (ADS)

Generation of the neutrino masses and leptogenesis (LG) in the standard model extended by the heavy Majorana fermions is considered. Classification of LG scenarios according to the new fermion mass spectra is given, where singlet-triplet LG is considered for the first time. The upper bound on the CP asymmetry relevant for LG with hierarchical heavy neutrinos (Davidson-Ibarra bound) is revised, and shown that in the case of one massless neutrino it essentially depends on the type of the light neutrino mass hierarchy. The resonant scenarios, which help to avoid the problem of extremely high reheating temperature in the early universe, are discussed. In particular, we present new simplified, generalized and detailed formulation of freed LG, which violates Davidson-Ibarra bound in a special class of models.

Zhuridov, Dmitry V.

2013-08-01

174

High Energy Neutrinos with a Mediterranean Neutrino Telescope  

SciTech Connect

The high energy neutrino detection by a km{sup 3} Neutrino Telescope placed in the Mediterranean sea provides a unique tool to both determine the diffuse astrophysical neutrino flux and the neutrino nucleon cross section in the extreme kinematical region, which could unveil the presence of new physics. Here is performed a brief analysis of possible NEMO site performances.

Borriello, E.; /Naples U. /INFN, Naples /Valencia U., IFIC; Cuoco, A.; /Aarhus U.; Mangano, G.; /Naples U. /INFN, Naples; Miele, G.; /Naples U. /INFN, Naples /Valencia U.,; Pastor, Sergio; /Valencia U., IFIC; Pisanti, O.; /Naples U. /INFN, Naples; Serpico, Pasquale Dario; /Fermilab

2007-09-01

175

Neutrino oscillations in the early Universe with nonequilibrium neutrino distributions  

NASA Astrophysics Data System (ADS)

Around one second after the big bang, neutrino decoupling and e+-e- annihilation distorted the Fermi-Dirac spectrum of neutrino energies. Assuming neutrinos have masses and can mix, we compute the distortions using nonequilibrium thermodynamics and the Boltzmann equation. The flavor behavior of neutrinos is studied during and following the generation of the distortion.

Kostelecký, V. Alan; Samuel, Stuart

1995-09-01

176

Reactor Monitoring with Neutrinos  

E-print Network

The fundamental knowledge on neutrinos acquired in the recent years open the possibility of applied neutrino physics. Among it the automatic and non intrusive monitoring of nuclear reactor by its antineutrino signal could be very valuable to IAEA in charge of the control of nuclear power plants. Several efforts worldwide have already started.

M. Cribier

2007-04-06

177

Monte Carlo Neutrino Oscillations  

E-print Network

We demonstrate that the effects of matter upon neutrino propagation may be recast as the scattering of the initial neutrino wavefunction. Exchanging the differential, Schrodinger equation for an integral equation for the scattering matrix S permits a Monte Carlo method for the computation of S that removes many of the numerical difficulties associated with direct integration techniques.

James P. Kneller; Gail C. McLaughlin

2005-09-29

178

The Sudbury Neutrino Observatory  

Microsoft Academic Search

The Sudbury Neutrino Observatory is a 1000 tonne heavy water Cerenkov detector built to observe neutrinos from the sun and from supernovae. It is located deep underground to reduce the cosmic background radiation to negligible levels. The observatory is nearing completion and will commence full data taking early in 1999. Some aspects of its design and construction, and some of

R. L. Helmer; R. L. Hahn; J. K. Rowley; A. L. Carter; B. Hollebone; D. Kessler; I. Blevis; F. Dalnoki-Veress; A. DeKok; J. Farine; D. R. Grant; C. K. Hargrove; G. Laberge; I. Levine; K. McFarlane; H. Mes; A. T. Noble; V. M. Novikov; M. O'Neill; M. Shatkay; C. Shewchuk; D. Sinclair; E. T. H. Clifford; R. Deal; E. D. Earle; E. Gaudette; G. Milton; B. Sur; J. Bigu; J. H. M. Cowan; D. L. Cluff; E. D. Hallman; R. U. Haq; J. Hewett; J. G. Hykawy; G. Jonkmans; R. Michaud; A. Roberge; J. Roberts; E. Saettler; M. H. Schwendener; H. Seifert; D. Sweezey; R. Tafirout; C. J. Virtue; D. N. Beck; Y. D. Chan; X. Chen; M. R. Dragowsky; F. W. Dycus; J. Gonzalez; M. C. P. Isaac; Y. Kajiyama; G. W. Koehler; K. T. Lesko; M. C. Moebus; E. B. Norman; C. E. Okada; A. W. P. Poon; P. Purgalis; A. Schuelke; A. R. Smith; R. G. Stokstad; S. Turner; I. Zlimen; J. M. Anaya; T. J. Bowles; S. J. Brice; E.-I. Esch; M. M. Fowler; A. Goldschmidt; A. Hime; A. F. McGirt; G. G. Miller; W. A. Teasdale; J. B. Wilhelmy; J. M. Wouters; J. D. Anglin; M. Bercovitch; W. F. Davidson; R. S. Storey; S. Biller; R. A. Black; R. J. Boardman; M. G. Bowler; J. Cameron; B. Cleveland; A. P. Ferraris; G. Doucas; H. Heron; C. Howard; N. A. Jelley; A. B. Knox; M. Lay; W. Locke; J. Lyon; S. Majerus; M. Moorhead; M. Omori; N. W. Tanner; R. K. Taplin; M. Thorman; D. L. Wark; J. C. Barton; P. T. Trent; R. Kouzes; M. M. Lowry; A. L. Bell; E. Bonvin; M. Boulay; M. Dayon; F. Duncan; L. S. Erhardt; H. C. Evans; G. T. Ewan; R. Ford; A. Hallin; A. Hamer; P. M. Hart; P. J. Harvey; D. Haslip; C. A. W. Hearns; R. Heaton; J. D. Hepburn; C. J. Jillings; E. P. Korpach; H. W. Lee; J. R. Leslie; M.-Q. Liu; H. B. Mak; A. B. McDonald; J. D. MacArthur; W. McLatchie; B. A. Moffat; S. Noel; T. J. Radcliffe; B. C. Robertson; P. Skensved; R. L. Stevenson; X. Zhu; S. Gil; J. Heise; R. J. Komar; C. W. Nally; H. S. Ng; C. E. Waltham; R. C. Allen; G. Bühler; H. H. Chen; G. Aardsma; T. Andersen; K. Cameron; M. C. Chon; R. H. Hanson; P. Jagam; J. Karn; J. Law; R. W. Ollerhead; J. J. Simpson; N. Tagg; J.-X. Wang; C. Alexander; E. W. Beier; J. C. Cook; D. F. Cowen; E. D. Frank; W. Frati; P. T. Keener; J. R. Klein; G. Mayers; D. S. McDonald; M. S. Neubauer; F. M. Newcomer; R. J. Pearce; R. G. V. de Water; R. V. Berg; P. Wittich; Q. R. Ahmad; J. M. Beck; M. C. Browne; T. H. Burritt; P. J. Doe; C. A. Duba; S. R. Elliott; J. E. Franklin; J. V. Germani; P. Green; A. A. Hamian; K. M. Heeger; M. Howe; R. M. Drees; A. Myers; R. G. H. Robertson; M. W. E. Smith; T. D. Steiger; T. V. Wechel; J. F. Wilkerson

2000-01-01

179

Neutrino 2012: Outlook - theory  

E-print Network

Ongoing developments in theory and phenomenology are related to the measured large value of 1-3 mixing and indications of significant deviation of the 2-3 mixing from maximal one. "Race" for the mass hierarchy has started and there is good chance that multi-megaton scale atmospheric neutrino detectors with low threshold (e.g. PINGU) will establish the type of hierarchy. Two IceCube candidates of the PeV cosmic neutrinos if confirmed, is the beginning of new era of high energy neutrino astronomy. Accumulation of data on solar neutrinos (energy spectrum, D-N asymmetry, value of $\\Delta m^2_{21}$) may uncover some new physics. The Tri-bimaximal mixing is disfavored and the existing discrete symmetry paradigm may change. The confirmed QLC prediction, $\\theta_{13} \\approx \\theta_{C}/\\sqrt{2}$, testifies for GUT, seesaw and some symmetry at very high scales. However, the same value of 1-3 mixing can be obtained in various ways which have different implications. The situation in lepton sector changes from special (with specific neutrino symmetries, etc.) to normal, closer to that in the quark sector. Sterile neutrinos are challenge for neutrino physics but also opportunity with many interesting phenomenological consequences. Further studies of possible connections between neutrinos and the dark sector of the Universe may lead to breakthrough both in particle physics and cosmology.

A. Yu. Smirnov

2012-10-15

180

Neutrino 2012: Outlook - theory  

NASA Astrophysics Data System (ADS)

Ongoing developments in theory and phenomenology are related to the measured large value of 1-3 mixing and indications of significant deviation of the 2-3 mixing from maximal one. "Race" for the mass hierarchy has started and there is good chance that multi-megaton scale atmospheric neutrino detectors with low threshold (e.g. PINGU) will establish the type of hierarchy. Two IceCube candidates of the PeV cosmic neutrinos if confirmed, is the beginning of new era of high energy neutrino astronomy. Accumulation of data on solar neutrinos (energy spectrum, D-N asymmetry, value of ?m212) may uncover some new physics. The Tri-bimaximal mixing is disfavored and the existing discrete symmetry paradigm may change. The confirmed QLC prediction, ?13??C/?{2}, testifies for GUT, seesaw and some symmetry at very high scales. However, the same value of 1-3 mixing can be obtained in various ways which have different implications. The situation in lepton sector changes from special (with specific neutrino symmetries, etc.) to normal, closer to that in the quark sector. Sterile neutrinos are challenge for neutrino physics but also opportunity with many interesting phenomenological consequences. Further studies of possible connections between neutrinos and the dark sector of the Universe may lead to breakthrough both in particle physics and cosmology.

Smirnov, A. Yu.

2013-02-01

181

Constraint on the heavy sterile neutrino mixing angles in the SO(10) model with double see-saw mechanism  

E-print Network

Constraints on the heavy sterile neutrino mixing angles are studied in the framework of a minimal supersymmetric ${\\rm SO}(10)$ model with {\\it double see-saw mechanism}. A new singlet matter in addition to the right-handed neutrinos is introduced to realize the double see-saw mechanism. The minimal ${\\rm SO}(10)$ model gives an unambiguous Dirac neutrino mass matrix, which enables us to predict the masses and the mixing angles in the enlarged $9 \\times 9$ neutrino mass matrix. Mixing angles between the light Majorana neutrinos and the heavy sterile neutrinos are shown to be within the LEP experimental bound on all ranges of the Majorana phases.

Takeshi Fukuyama; Tatsuru Kikuchi; Koichi Matsuda

2005-10-05

182

Neutrino-antineutrino correlations in dense anisotropic media  

NASA Astrophysics Data System (ADS)

We derive the most general evolution equations describing in-medium (anti)neutrino propagation in the mean-field approximation. In particular, we consider various types of neutrino-antineutrino mixing, for both Dirac and Majorana fields, resulting either from nontrivial pair correlations or from helicity coherence due to the nonvanishing neutrino masses. We show that, unless the medium is spatially homogeneous and isotropic, these correlations are sourced by the usual neutrino and antineutrino densities. This may be of importance in astrophysical environments such as core-collapse supernovae.

Serreau, Julien; Volpe, Cristina

2014-12-01

183

Neutrino-antineutrino correlations in dense anisotropic media  

E-print Network

We derive the most general evolution equations describing in-medium (anti)neutrino propagation in the mean-field approximation. In particular, we consider various types of neutrino-antineutrino mixing, for both Dirac and Majorana fields, resulting either from nontrivial pair correlations or from helicity coherence due to the nonvanishing neutrino masses. We show that, unless the medium is spatially homogeneous and isotropic, these correlations are sourced by the usual neutrino and antineutrino densities. This may be of importance in astrophysical environments such as core-collapse supernovae.

Julien Serreau; Cristina Volpe

2015-01-08

184

Physics and Astrophysics of Neutrinos  

Microsoft Academic Search

Observations of neutrinos being emitted by the supernova SN1987A, star neutrinos, and atmospheric neutrinos by means of underground detectors have provided new insights into astronomy. These observations have brought to light new unresolved phenomena such as the solar neutrino problem, spurring investigative studies among particle physicists and astrophysicists. Today, intense interaction and continual cooperation between specialists in the field of

Masataka Fukugita; Atsuto Suzuki

1994-01-01

185

Neutrino assisted gauge mediation  

NASA Astrophysics Data System (ADS)

Recent observation shows that the Higgs mass is at around 125 GeV while the prediction of the minimal supersymmetric standard model is below 120 GeV for stop mass lighter than 2 TeV unless the top squark has a maximal mixing. We consider the right-handed neutrino supermultiplets as messengers in addition to the usual gauge mediation to obtain sizeable trilinear soft parameters A t needed for the maximal stop mixing. Neutrino messengers can explain the observed Higgs mass for stop mass around 1 TeV. Neutrino assistance can also generate charged lepton flavor violation including ?? e? as a possible signature of the neutrino messengers. We consider the S 4 discrete flavor model and show the relation of the charged lepton flavor violation, ? 13 of neutrino oscillation and the muon's g-2.

Kim, Hyung Do; Mo, Doh Young; Seo, Min-Seok

2013-06-01

186

Solar neutrinos: Probing the sun or neutrinos  

SciTech Connect

The decade of the 1990's should prove to be a landmark period for the study of solar neutrino physics. Current observations show 2-3 times fewer neutrinos coming from the sun than are theoretically expected. As we enter the decade, new experiments are poised to attempt and discover whether this deficit is a problem with our understanding of how the sun works, is a hint of new neutrino properties beyond those predicted by the standard model of particle physics, or perhaps a combination of both. This paper will review the current status of the field and point out how future measurements should help solve this interesting puzzle. 11 refs., 3 figs., 1 tab.

Wilkerson, J.F.

1991-01-01

187

Coherent scattering of cosmic neutrinos  

NASA Technical Reports Server (NTRS)

It is shown that cosmic neutrino scattering can be non-negligible when coherence effects previously neglected are taken into account. The coherent neutrino scattering cross section is derived and the neutrino index of refraction evaluated. As an example of coherent neutrino scattering, a detector using critical reflection is described which in principle can detect the low energy cosmic neutrino background allowed by the measured cosmological red shift.

Opher, R.

1974-01-01

188

Inverse Neutrino-less Double Beta Decay Revisited: Neutrinos, Higgs Triplets and a Muon Collider  

E-print Network

We revisit the process of inverse neutrino-less double beta decay (e e -> W W) at future linear colliders. The cases of Majorana neutrino and Higgs triplet exchange are considered. We also discuss the processes e mu -> W W and mu mu -> W W, which are motivated by the possibility of muon colliders. For heavy neutrino exchange and center-of-mass energies larger than 1 TeV, we show that masses up to 10^6 (10^5) GeV could be probed for e-e and e-mu machines, respectively. The stringent limits for mixing of heavy neutrinos with muons render mu mu -> W W less promising, even though this process is not constrained by limits from neutrino-less double beta decay. If Higgs triplets are responsible for inverse neutrino-less double beta decay, observable signals are only possible if a very narrow resonance is met. We also consider unitarity aspects of the process in case both Higgs triplets and neutrinos are exchanged. An exact see-saw relation connecting low energy data with heavy neutrino and triplet parameters is found.

Werner Rodejohann

2010-05-17

189

Neutrino Masses in E6 Unification  

NASA Astrophysics Data System (ADS)

We show that neutrino masses with large mixing between νμ and ντ are naturally reproduced in a supersymmetric E6 grand unification model with an anomalous U(1)X symmetry. We propose a simple scenario which incorporates a novel mechanism called `E-twisting' by which all the characteristic features of the fermion mass matrices, not only the quark/lepton Dirac masses but also the neutrino's Majorana masses, can be reproduced despite the fact that all the members in 27 of each generation are assigned a common U(1)X charge.

Bando, M.; Kugo, T.

1999-06-01

190

Neutrinoless double beta decay and neutrino masses  

SciTech Connect

Neutrinoless double beta decay (0{nu}{beta}{beta}) is a promising test for lepton number violating physics beyond the standard model (SM) of particle physics. There is a deep connection between this decay and the phenomenon of neutrino masses. In particular, we will discuss the relation between 0{nu}{beta}{beta} and Majorana neutrino masses provided by the so-called Schechter-Valle theorem in a quantitative way. Furthermore, we will present an experimental cross check to discriminate 0{nu}{beta}{beta} from unknown nuclear background using only one isotope, i.e., within one experiment.

Duerr, Michael [Max-Planck-Institut fuer Kernphysik, Saupfercheckweg 1, 69117 Heidelberg (Germany)

2012-07-27

191

Pseudo-Dirac neutrinos as a potential complete solution to the neutrino oscillation puzzle  

NASA Astrophysics Data System (ADS)

A solution for the neutrino mass and mixing pattern is proposed which is compatible with all available experimental data on neutrino oscillations. This solution involves Majorana neutrinos of the pseudo-Dirac type, i.e. mMajorana?mDirac. The solar and atmospheric neutrino observations are mainly explained as ?e-?eS and ??-??S oscillations, where S indicates the sterile (``righthanded'') partner of each neutrino generation, while the LSND result is interpreted in terms of standard ??-?e oscillations. The resulting constraints on ??-?? and ??-??S oscillations are also discussed. This solution leaves room for a hierarchical mass and mixing scheme with a ?? mass in the few eV range, as favoured by some dark matter scenarios. The apparent conflict with standard Big Bang nucleosynthesis is addressed and the implications for current and future experiments are discussed. It is argued that both short and long baseline accelerator neutrino experiments are needed in order to decide between this solution and other oscillation scenarios.

Geiser, A.

1998-12-01

192

Topics in neutrino astrophysics  

NASA Astrophysics Data System (ADS)

In this thesis, we investigate observable consequences of active and sterile neutrinos, in galactic, cluster, and cosmological scales. We assume that sterile neutrinos with masses of order 10's eV, 10's keV, and MeV were formed by oscillation of active neutrinos in the early universe. If sterile neutrinos with mass ~ 30 eV exist, they affect the structure of galaxies and explain the flatness of their rotation curves. Also, the existence of decaying sterile neutrinos with mass 16 -- 18 keV and decay rate G = (5 ± 1) × 10^-17 s -1 can simultaneously be the cause of heating at the Milky Way center, the supermassive blackhole mass and velocity dispersion relation, the lack of cooling flow in clusters, and reionization in the universe. Lastly, we make of the observed 511 keV annihilation flux line at the Milky Way center to constrain properties of sterile neutrinos of MeV mass scale. We also derive a relation among several cluster observables assuming the existence of an active neutrino halo, which agrees with the observational data in 103 clusters.

Chan, Man Ho

2009-06-01

193

Superheavy sterile neutrinos as dark matter  

E-print Network

neutrinos as a dark matter candidate, produced through MSW conversion of active neutrinos. Recently Allen proposed a different nonthermal mechanism for the production of superheavy sterile neutrinos. Such neutrinos are predicted by an SO(10) grand...

Tang, Yongjun

2012-06-07

194

Solar mass-varying neutrino oscillations  

E-print Network

We propose that the solar neutrino deficit may be due to oscillations of mass-varying neutrinos (MaVaNs). This scenario elucidates solar neutrino data beautifully while remaining comfortably compatible with atmospheric neutrino and K2K data...

Marfatia, Danny; Huber, P.; Barger, V.

2005-11-18

195

Neutrinos from neutron stars  

NASA Technical Reports Server (NTRS)

A calculation of the flux of ultra-high energy neutrinos from galactic neutron stars is presented. The calculation is used to determine the number of point sources detectable at the sensitivity threshold of a proposed deep underwater muon and neutrino detector array. The detector array would have a point source detection threshold of about 100 eV/sq cm-sec. Analysis of neutrino luminosities and the number of detectable sources suggests that the deep underwater detector may make a few discoveries. In particular, a suspected neutron star in the Cyg X-3 source seems a promising target for the deep underwater array.

Helfand, D. J.

1979-01-01

196

Neutrinos: Nature's Identity Thieves?  

SciTech Connect

The oscillation of neutrinos from one variety to another has long been suspected, but was confirmed only about 15 years ago. In order for these oscillations to occur, neutrinos must have a mass, no matter how slight. Since neutrinos have long been thought to be massless, in a very real way, this phenomena is a clear signal of physics beyond the known. In this video, Fermilab's Dr Don Lincoln explains how we know it occurs and hints at the rich experimental program at several international laboratories designed to understand this complex mystery.

Lincoln, Don

2013-07-11

197

Submarine neutrino communication  

E-print Network

We discuss the possibility to use a high energy neutrino beam from a muon storage ring to provide one way communication with a submerged submarine. Neutrino interactions produce muons which can be detected either, directly when they pass through the submarine or by their emission of Cerenkov light in sea water, which, in turn, can be exploited with sensitive photo detectors. Due to the very high neutrino flux from a muon storage ring, it is sufficient to mount either detection system directly onto the hull of the submersible. The achievable data transfer rates compare favorable with existing technologies and do allow for a communication at the usual speed and depth of submarines.

Patrick Huber

2010-08-20

198

Submarine neutrino communication  

E-print Network

We discuss the possibility to use a high energy neutrino beam from a muon storage ring to provide one way communication with a submerged submarine. Neutrino interactions produce muons which can be detected either, directly when they pass through the submarine or by their emission of Cerenkov light in sea water, which, in turn, can be exploited with sensitive photo detectors. Due to the very high neutrino flux from a muon storage ring, it is sufficient to mount either detection system directly onto the hull of the submersible. The achievable data transfer rates compare favorable with existing technologies and do allow for a communication at the usual speed and depth of submarines.

Huber, Patrick

2009-01-01

199

Neutrinos: Nature's Identity Thieves?  

ScienceCinema

The oscillation of neutrinos from one variety to another has long been suspected, but was confirmed only about 15 years ago. In order for these oscillations to occur, neutrinos must have a mass, no matter how slight. Since neutrinos have long been thought to be massless, in a very real way, this phenomena is a clear signal of physics beyond the known. In this video, Fermilab's Dr Don Lincoln explains how we know it occurs and hints at the rich experimental program at several international laboratories designed to understand this complex mystery.

Lincoln, Don

2014-08-07

200

Formation of neutrino halos  

NASA Astrophysics Data System (ADS)

A fully general relativistic nonlinear model of the formation of massive neutrino halos in an Einstein-Straus universe was given by Fabbri, Jantzen and Ruffini (1982). The paper considers the role which a nonvanishing, repulsive cosmological constant Lambda greater than 0, admissible by observational limits, can have in the FJR model. The main conclusion is that the influence of Lambda is negligible in the FJR model for massive neutrinos with mass of about 10 eV, indicated by recent observations of SN 1987a. On the other hand, the cosmological constant is relevant in the model, if neutrinos have low mass, less than 0.2 eV.

Stuchlik, Zdenek

201

Neutrinos: Nature's Identity Thieves?  

ScienceCinema

The oscillation of neutrinos from one variety to another has long been suspected, but was confirmed only about 15 years ago. In order for these oscillations to occur, neutrinos must have a mass, no matter how slight. Since neutrinos have long been thought to be massless, in a very real way, this phenomena is a clear signal of physics beyond the known. In this video, Fermilab's Dr Don Lincoln explains how we know it occurs and hints at the rich experimental program at several international laboratories designed to understand this complex mystery.

Dr. Don Lincoln

2013-07-22

202

Solar-neutrino oscillations  

NASA Technical Reports Server (NTRS)

The theory of oscillations of solar neutrinos is developed as it applies to the electron-recoil spectrum in neutrino-electron scattering. The spectral information obtained by such measurements (as opposed to counting total event rates) is crucial for allowing observation of neutrino oscillations for masses down to 500 neV. In this regard, the effects of different masses and mixing angles, as well as such subtleties as thermal and pressure broadening, finite solar-core size, and variable indices of refraction are investigated.

Krauss, L.; Wilczek, F.

1985-01-01

203

Neutrino time travel  

E-print Network

We discuss causality properties of extra-dimensional theories allowing for effectively superluminal bulk shortcuts. Such shortcuts for sterile neutrinos have been discussed as a solution to the puzzling LSND and MiniBooNE neutrino oscillation results. We focus here on the sub-category of asymmetrically warped brane spacetimes and argue that scenarios with two extra dimensions may allow for timelike curves which can be closed via paths in the extra-dimensional bulk. In principle sterile neutrinos propagating in the extra dimension may be manipulated in a way to test the chronology protection conjecture experimentally.

James Dent; Heinrich Päs; Sandip Pakvasa; Thomas J. Weiler

2007-10-12

204

Atmospheric neutrino oscillations and tau neutrinos in ice  

SciTech Connect

The main goal of the IceCube Deep Core Array is to search for neutrinos of astrophysical origins. Atmospheric neutrinos are commonly considered as a background for these searches. We show here that cascade measurements in the Ice Cube Deep Core Array can provide strong evidence for tau neutrino appearance in atmospheric neutrino oscillations. Controlling systematic uncertainties will be the limiting factor in the analysis. A careful study of these tau neutrinos is crucial, since they constitute an irreducible background for astrophysical neutrino detection.

Giordano, Gerardo; Mocioiu, Irina [Department of Physics, Pennsylvania State University, University Park, Pennsylvania 16802 (United States); Mena, Olga [Instituto de Fisica Corpuscular, IFIC, CSIC and Universidad de Valencia (Spain)

2010-06-01

205

Sterile neutrinos: Phenomenology and theory  

NASA Astrophysics Data System (ADS)

A simultaneous understanding of the results of the LSND experiment indicating ??-?e oscillation together with other evidences for neutrino oscillations from solar and atmospheric neutrino data seems to require the existence of at least one sterile neutrino. One can also give other plausible astrophysical arguments that seem to require light sterile neutrinos. If such sterile neutrinos exist, a major theoretical challenge is to understand why they are so light. A scenario for the light sterile neutrino is presented where one assumes a parity doubling of the standard model with identical matter and gauge content. The neutrinos of the parity doubled (mirror) sector are light for the same reason that the known neutrinos are light and since they do not couple to the known W and Z bosons, they can be identified with the sterile neutrinos. Some of the implications and possible tests of this hypothesis are mentioned.

Mohapatra, Rabindra N.

1999-07-01

206

Leptoquarks: Neutrino masses and related accelerator signals  

SciTech Connect

Leptoquark-Higgs interactions induce mixing between leptoquark (LQ) states with different chiralities once the electroweak symmetry is broken. In such LQ models Majorana neutrino masses are generated at 1-loop order. Here we calculate the neutrino mass matrix and explore the constraints on the parameter space enforced by the assumption that LQ-loops explain current neutrino oscillation data. LQs will be produced at the CERN LHC, if their masses are at or below the TeV scale. Since the fermionic decays of LQs are governed by the same Yukawa couplings, which are responsible for the nontrivial neutrino mass matrix, several decay branching ratios of LQ states can be predicted from measured neutrino data. Especially interesting is that large lepton flavor violating rates in muon and tau final states are expected. In addition, the model predicts that, if kinematically possible, heavier LQs decay into lighter ones plus either a standard model Higgs boson or a Z{sup 0}/W{sup {+-}} gauge boson. Thus, experiments at the LHC might be able to exclude the LQ mechanism as an explanation of neutrino data.

Aristizabal Sierra, D.; Hirsch, M.; Kovalenko, S. G. [AHEP Group, Instituto de Fisica Corpuscular-C.S.I.C./Universitat de Valencia Edificio de Institutos de Paterna, Apartado 22085, E-46071 Valencia (Spain); Centro de Estudios Subatomicos (CES), Universidad Tecnica Federico Santa Maria, Casilla 110-V, Valparaiso (Chile)

2008-03-01

207

The Science of NOA Neutrinos are everywhere!  

E-print Network

The Science of NOA Neutrinos are everywhere! Neutrinos are among the most abundant particles. Unimaginably large numbers of neutrinos from the first moments of the universe are still present today. Neutrinos help to shape our universe Nuclear reactions make the sun shine, producing neutrinos. Neutrinos

Quigg, Chris

208

Detecting the Neutrino  

NASA Astrophysics Data System (ADS)

In 1930 Wolfgang Pauli suggested that a new particle might be required to make sense of the radioactive-disintegration mode known as beta decay. This conjecture initially seemed impossible to verify since the new particle, which became known as the neutrino, was uncharged, had zero or small mass, and interacted only insignificantly with other matter. In 1951 Frederick Reines and Clyde L. Cowan, Jr., of the Los Alamos Scientific Laboratory undertook the difficult task of detecting the free neutrino by observing its inverse beta-decay interaction with matter. They succeeded in 1956. The neutrino was accepted rapidly as a fundamental particle despite discrepancies in reported details of the experiments and despite the absence of independent verification of the result. This paper describes the experiments, examines the nature of the discrepancies, and discusses the circumstances of the acceptance of the neutrino's detection by the physics community.

Arns, Robert G.

209

Phenomenology of Neutrino Oscillations  

E-print Network

The phenomenology of solar, atmospheric, supernova and laboratory neutrino oscillations is described. Analytical formulae for matter effects are reviewed. The results from oscillations are confronted with neutrinoless double beta decay.

G. Rajasekaran

2000-04-17

210

Electromagnetic properties of massive neutrinos  

SciTech Connect

The vertex function for a virtual massive neutrino is calculated in the limit of soft real photons. A method based on employing the neutrino self-energy operator in a weak external electromagnetic field in the approximation linear in the field is developed in order to render this calculation of the vertex function convenient. It is shown that the electric charge and the electric dipole moment of the real neutrino are zero; only the magnetic moment is nonzero for massive neutrinos. A fourth-generation heavy neutrino of mass not less than half of the Z-boson mass is considered as a massive neutrino.

Dobrynina, A. A., E-mail: aleksandradobrynina@rambler.ru; Mikheev, N. V.; Narynskaya, E. N. [Demidov Yaroslavl State University (Russian Federation)] [Demidov Yaroslavl State University (Russian Federation)

2013-10-15

211

Recent advances in neutrino astrophysics  

E-print Network

Neutrinos are produced by a variety of sources that comprise our Sun, explosive environments such as core-collapse supernovae, the Earth and the Early Universe. The precise origin of the recently discovered ultra-high energy neutrinos is to be determined yet. These weakly interacting particles give us information on their sources, although the neutrino fluxes can be modified when neutrinos traverse an astrophysical environment. Here we highlight recent advances in neutrino astrophysics and emphasise the important progress in our understanding of neutrino flavour conversion in media.

Cristina Volpe

2014-11-24

212

Experimental High Energy Neutrino Astrophysics  

SciTech Connect

Neutrinos are considered promising probes for high energy astrophysics. More than four decades after deep water Cerenkov technique was proposed to detect high energy neutrinos. Two detectors of this type are successfully taking data: BAIKAL and AMANDA. They have demonstrated the feasibility of the high energy neutrino detection and have set first constraints on TeV neutrino production astrophysical models. The quest for the construction of km3 size detectors have already started: in the South Pole, the IceCube neutrino telescope is under construction; the ANTARES, NEMO and NESTOR Collaborations are working towards the installation of a neutrino telescope in the Mediterranean Sea.

Distefano, Carla [Laboratori Nazionali del Sud, Catania (Italy)

2005-10-12

213

Neutrino Detectors: Challenges and Opportunities  

SciTech Connect

This paper covers possible detector options suitable at future neutrino facilities, such as Neutrino Factories, Super Beams and Beta Beams. The Magnetised Iron Neutrino Detector (MIND), which is the baseline detector at a Neutrino Factory, will be described and a new analysis which improves the efficiency of this detector at low energies will be shown. Other detectors covered include the Totally Active Scintillating Detectors (TASD), particularly relevant for a low energy Neutrino Factory, emulsion detectors for tau detection, liquid argon detectors and megaton scale water Cherenkov detectors. Finally the requirements of near detectors for long-baseline neutrino experiments will be demonstrated.

Soler, F. J. P. [School of Physics and Astronomy, University of Glasgow, Glasgow G12 8QQ (United Kingdom)

2011-10-06

214

Neutrinos beyond the Standard Model  

SciTech Connect

I review some basic aspects of neutrino physics beyond the Standard Model such as neutrino mixing and neutrino non-orthogonality, universality and CP violation in the lepton sector, total lepton number and lepton flavor violation, etc.. These may lead to neutrino decays and oscillations, exotic weak decay processes, neutrinoless double /beta/ decay, etc.. Particle physics models are discussed where some of these processes can be sizable even in the absence of measurable neutrino masses. These may also substantially affect the propagation properties of solar and astrophysical neutrinos. 39 refs., 4 figs.

Valle, J.W.F.

1989-08-01

215

Helicity of Neutrinos  

Microsoft Academic Search

A combined analysis of circular polarization and resonant scattering of ; gamma rays following orbital electron capture measures the helicity of the ; neutrino. A measurement was carried out with Eu¹⁵² which decays by orbital ; electron capture. Assuming the most plausible spin-parity for this isomer ; compatible with its decay scheme, 0-1, it was found that the neutrino was

M. Goldhaber; L. Grodzins; A. W. Sunyar

1958-01-01

216

The Sudbury Neutrino Observatory  

Microsoft Academic Search

Two experiments now in progress have reported measurements of the flux of high energy neutrinos from the Sun. Since about 1970, Davis and his co-workers have been using a [sup 37]Cl-based detector to measure the [sup 7]Be and [sup 8]B solar neutrino flux and have found it to be at least a factor of three lower than that predicted by

E. B. Norman; Y. D. Chan; A. Garcia; K. T. Lesko; A. R. Smith; R. G. Stokstad; I. Zlimen; H. C. Evans; G. T. Ewan; A. Hallin; H. W. Lee; J. R. Leslie; J. D. MacArthur; H. B. Mak; A. B. McDonald; W. McLatchie; B. C. Robertson; P. Skensved; B. Sur; E. Bonvin; E. D. Earle; D. Hepburn; G. M. Milton

1992-01-01

217

Supernova neutrino detection  

E-print Network

The gravitational core collapse of a star produces a huge burst of neutrinos of all flavors. A number of detectors worldwide are sensitive to such a burst; its detection would yield information about both particle physics and astrophysics. Sensitivity to all flavors, and ability to tag different interactions, will be key for extraction of information. Here I will survey the capabilities of current and future detectors for detection of supernova neutrinos from the Milky Way and beyond.

K. Scholberg

2007-01-04

218

The Highest Energy Neutrinos  

E-print Network

Measurements of the arrival directions of cosmic rays have not revealed their sources. High energy neutrino telescopes attempt to resolve the problem by detecting neutrinos whose directions are not scrambled by magnetic fields. The key issue is whether the neutrino flux produced in cosmic ray accelerators is detectable. It is believed that the answer is affirmative, both for the galactic and extragalactic sources, provided the detector has kilometer-scale dimensions. We revisit the case for kilometer-scale neutrino detectors in a model-independent way by focussing on the energetics of the sources. The real breakthrough though has not been on the theory but on the technology front: the considerable technical hurdles to build such detectors have been overcome. Where extragalactic cosmic rays are concerned an alternative method to probe the accelerators consists in studying the arrival directions of neutrinos produced in interactions with the microwave background near the source, i.e. within a GZK radius. Their flux is calculable within large ambiguities but, in any case, low. It is therefore likely that detectors that are larger yet by several orders of magnitudes are required. These exploit novel techniques, such as detecting the secondary radiation at radio wavelengths emitted by neutrino induced showers.

Francis Halzen

2007-10-22

219

Small Neutrino Masses from Supersymmetry Breaking  

SciTech Connect

An alternative to the conventional see-saw mechanism is proposed to explain the origin of small neutrino masses in supersymmetric theories. The masses and couplings of the right-handed neutrino field are suppressed by supersymmetry breaking, in a way similar to the suppression of the Higgs doublet mass, $\\mu$. New mechanisms for light Majorana, Dirac and sterile neutrinos arise, depending on the degree of suppression. Superpartner phenomenology is greatly altered by the presence of weak scale right-handed sneutrinos, which may have a coupling to a Higgs boson and a left-handed sneutrino. The sneutrino spectrum and couplings are quite unlike the conventional case - the lightest sneutrino can be the dark matter and predictions are given for event rates at upcoming halo dark matter direct detection experiments. Higgs decays and search strategies are changed. Copious Higgs production at hadron colliders can result from cascade decays of squarks and gluinos.

Arkani-Hamed, Nima; Hall, Lawrence; Murayama, Hitoshi; Smith, David; Weiner, Neal

2000-06-27

220

Measurement of Atmospheric Neutrinos at the Sudbury Neutrino Observatory  

E-print Network

The Sudbury Neutrino Observatory consists of a 1 kiloton heavy water Cherenkov detector able to detect and reconstruct high-energy muons created from cosmic ray showers and atmospheric neutrino interactions. By measuring ...

Formaggio, Joseph A.

221

Sterile Neutrino Fits to Short-Baseline Neutrino Oscillation Measurements  

E-print Network

This paper reviews short-baseline oscillation experiments as interpreted within the context of one, two, and three sterile neutrino models associated with additional neutrino mass states in the ~1?eV range. Appearance and ...

Conrad, J. M.

2013-01-01

222

Core-collapse supernova neutrinos and neutrino properties  

E-print Network

Core-collapse supernovae are powerful neutrino sources. The observation of a future (extra-)galactic supernova explosion or of the relic supernova neutrinos might provide important information on the supernova dynamics, on the supernova formation rate and on neutrino properties. One might learn more about unknown neutrino properties either from indirect effects in the supernova (e.g. on the explosion or on in the r-process) or from modifications of the neutrino time or energy distributions in a detector on Earth. Here we will discuss in particular possible effects of CP violation in the lepton sector. We will also mention the interest of future neutrino-nucleus interaction measurements for the precise knowledge of supernova neutrino detector response to electron neutrinos.

J. Gava; C. Volpe

2008-05-18

223

Probing leptogenesis with GeV-scale sterile neutrinos at LHCb and Belle II  

NASA Astrophysics Data System (ADS)

We show that existing laboratory experiments have the potential to unveil the origin of matter by probing leptogenesis in the type-I seesaw model with three right-handed neutrinos and Majorana masses in the GeV range. The baryon asymmetry is generated by C P -violating flavor oscillations during the production of the right-handed neutrinos. In contrast to the case with only two right-handed neutrinos, no degeneracy in the Majorana masses is required. The right-handed neutrinos can be found in meson decays at Belle II and LHCb.

Canetti, Laurent; Drewes, Marco; Garbrecht, Björn

2014-12-01

224

Electrophobic Lorentz invariance violation for neutrinos and the see-saw mechanism  

E-print Network

In this talk we show how Lorentz invariance violation (LIV) can occur for Majorana neutrinos, without inducing LIV in the charged leptons via radiative corrections. Such ``electrophobic'' LIV is due to the Majorana nature of the LIV operator together with electric charge conservation. Being free from the strong constraints coming from the charged lepton sector, electrophobic LIV can in principle be as large as current neutrino experiments permit. On the other hand electrophobic LIV could be naturally small if it originates from LIV in some singlet ``right-handed neutrino'' sector, and is felt in the physical left-handed neutrinos via a see-saw mechanism.

S. F. King

2004-09-28

225

Physics and Astrophysics of Neutrinos  

NASA Astrophysics Data System (ADS)

Observations of neutrinos being emitted by the supernova SN1987A, star neutrinos, and atmospheric neutrinos by means of underground detectors have provided new insights into astronomy. These observations have brought to light new unresolved phenomena such as the solar neutrino problem, spurring investigative studies among particle physicists and astrophysicists. Today, intense interaction and continual cooperation between specialists in the field of particle physics and astronomy/cosmology are a pre-requisite for conducting further studies. This book provides detailed elaborations on selected topics. One of the most important features of this book is its enumeration of a number of basic properties of neutrinos and their relationship to Grand Unified Theories. It does not cover all aspects of neutrino theory, but rather focuses on the origin of the neutrino's mass and the generation mixing of neutrinos. The neutrino experiments described were carried out mainly by Japanese researchers. All the kamiokande results, detector performances, and complete references are included. Experiments regarding the neutrino's mass are represented in the direct mass measurement, the double beta-decay experiment, and the neutrino oscillation experiment. The detection of low-energy astrophysical neutrinos is discussed. Particle acceleration mechanisms in astrophysics and the detection of high-energy gamma-rays and neutrinos are also represented.

Fukugita, Masataka; Suzuki, Atsuto

1994-01-01

226

Prospect for Relic Neutrino Searches  

NASA Astrophysics Data System (ADS)

Neutrinos from the Big Bang are theoretically expected to be the most abundant particles in the Universe after the photons of the Cosmic Microwave Background (CMB). Unlike the relic photons, relic neutrinos have not so far been observed. The Cosmic Neutrino Background (C?B) is the oldest relic from the Big Bang, produced a few seconds after the Bang itself. Due to their impact in cosmology, relic neutrinos may be revealed indirectly in the near future through cosmological observations. In this talk we concentrate on other proposals, made in the last 30 years, to try to detect the C?B directly, either in laboratory searches (through tiny accelerations they produce on macroscopic targets) or through astrophysical observations (looking for absorption dips in the flux of Ultra-High Energy (UHE) neutrinos, due to the annihilation of these neutrinos with relic neutrinos at the Z-resonance). We concentrate mainly on the first possibility. We show that, given present bounds on neutrino masses, lepton number in the Universe and gravitational clustering of neutrinos, all expected laboratory effects of relic neutrinos are far from observability, awaiting future technological advances to reach the necessary sensitivity. The problem for astrophysical searches is that sources of UHE neutrinos at the extreme energies required may not exist. If they do exist, we could reveal the existence, and possibly the mass spectrum, of relic neutrinos, with detectors of UHE neutrinos (such as ANITA, Auger, EUSO, OWL, RICE and SalSA).

Gelmini, Graciela B.

2005-01-01

227

Prospect for Relic Neutrino Searches  

NASA Astrophysics Data System (ADS)

Neutrinos from the Big Bang are theoretically expected to be the most abundant particles in the Universe after the photons of the Cosmic Microwave Background (CMB). Unlike the relic photons, relic neutrinos have not so far been observed. The Cosmic Neutrino Background (C?B) is the oldest relic from the Big Bang, produced a few seconds after the Bang itself. Due to their impact in cosmology, relic neutrinos may be revealed indirectly in the near future through cosmological observations. In this talk we concentrate on other proposals, made in the last 30 years, to try to detect the C?B directly, either in laboratory searches (through tiny accelerations they produce on macroscopic targets) or through astrophysical observations (looking for absorption dips in the flux of Ultra-High Energy (UHE) neutrinos, due to the annihilation of these neutrinos with relic neutrinos at the Z-resonance). We concentrate mainly on the first possibility. We show that, given present bounds on neutrino masses, lepton number in the Universe and gravitational clustering of neutrinos, all expected laboratory effects of relic neutrinos are far from observability, awaiting future technological advances to reach the necessary sensitivity. The problem for astrophysical searches is that sources of UHE neutrinos at the extreme energies required may not exist. If they do exist, we could reveal the existence, and possibly the mass spectrum, of relic neutrinos, with detectors of UHE neutrinos (such as ANITA, Auger, EUSO, OWL, RICE and SalSA).

Gelmini, Graciela B.

2006-03-01

228

Formation of Neutrino Stars from Cosmological Background Neutrinos  

E-print Network

We study hydrodynamic evolution of cosmological background neutrinos. By using a spherically symmetric Newtonian hydrodynamic code, we calculate the time evolution of the density profiles of neutrino matter in cluster and galactic scales. We discuss the possible observational consequences of such evolution and the resulting density profiles of the degenerate neutrino `stars' in galaxies and clusters.

M. H. Chan; M. -C. Chu

2006-09-20

229

Vetoing atmospheric neutrinos in a high energy neutrino telescope  

E-print Network

We discuss the possibility to suppress downward atmospheric neutrinos in a high energy neutrino telescope. This can be achieved by vetoing the muon which is produced by the same parent meson decaying in the atmosphere. In principle, atmospheric neutrinos with energies $E_\

Stefan Schönert; Thomas K. Gaisser; Elisa Resconi; Olaf Schulz

2008-12-22

230

First neutrino observations from the Sudbury Neutrino Observatory  

Microsoft Academic Search

The first neutrino observations from the Sudbury Neutrino Observatory are presented from preliminary analyses. Based on energy, direction and location, the data in the region of interest appear to be dominated by 8B solar neutrinos, detected by the charged current reaction on deuterium and elastic scattering from electrons, with very little background. Measurements of radioactive backgrounds indicate that the measurement

R. G. Allen; G. Buhler; H. H. Chen; 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; J. Cameron; Y. D. Chan; 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. A. Dunmore; E. D. Earle; S. R. Elliott; H. C. Evans; G. T. Ewan; J. Farine; H. Fergani; A. P. Ferraris; R. J. Ford; J. A. Formaggio; M. M. Fowler; K. Frame; E. D. Frank; W. Frati; N. Gagnon; J. V. Germani; S. Gil; K. Graham; D. R. Grant; R. L. Hahn; A. L. Hallin; E. D. Hallman; A. S. Hamer; A. A. Hamian; W. B. Handler; R. U. 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; J. Hewett; A. Hime; J. G. Hykawy; M. C. P. Isaac; P. Jagam; N. A. Jelley; C. Jillings; G. Jonkmans; K. Kazkaz; P. T. Keener; J. R. Klein; A. B. Knox; R. J. Komar; R. Kouzes; T. Kutter; C. C. M. Kyba; J. Law; I. T. Lawson; M. Lay; H. W. Lee; K. T. Lesko; J. R. Leslie; I. Levine; W. Locke; S. Luoma; J. Lyon; S. Majerus; H. B. Mak; J. Maneira; J. Manor; A. D. Marino; N. McCauley; D. S. McDonald; A. B. McDonald; K. McFarlane; G. McGregor; R. Meijer; C. Mifflin; G. G. Miller; G. Milton; B. A. Moffat; M. Moorhead; C. W. Nally; M. S. Neubauer; F. M. Newcomer; H. S. Ng; A. J. Noble; E. B. Norman; V. M. Novikov; M. ONeill; C. E. Okada; R. W. Ollerhead; M. Omori; J. L. Orrell; S. M. Oser; A. W. P. Poon; T. J. Radcliffe; A. Roberge; B. C. Robertson; R. G. H. Robertson; S. S. E. Rosendahl; J. K. Rowley; V. L. Rusu; E. Saettler; K. K. Schaffer; M. H. Schwendener; A. Schulke; H. Seifert; M. Shatkay; J. J. Simpson; C. J. Sims

2001-01-01

231

Local demands on sterile neutrinos  

E-print Network

In a model independent manner, we explore the local implications of a single neutrino oscillation measurement which cannot be reconciled within a three-neutrino theory. We examine this inconsistency for a single region of baseline to neutrino energy $L/E$. Assuming that sterile neutrinos account for the anomaly, we find that the {\\it local} demands of this datum can require the addition to the theory of one to three sterile neutrinos. We examine the constraints which can be used to determine when more than one neutrino would be required. The results apply only to a given region of $L/E$. The question of the adequacy of the sterile neutrinos to satisfy a global analysis is not addressed here. Finally, using the results of a 3+2 analysis, we indicate values for unknown mixing matrix elements which would require two sterile neutrinos due to local demands only.

David C. Latimer; David J. Ernst

2005-09-23

232

Simulating nonlinear neutrino flavor evolution  

E-print Network

We discuss a new kind of astrophysical transport problem: the coherent evolution of neutrino flavor in core collapse supernovae. Solution of this problem requires a numerical approach which can simulate accurately the quantum mechanical coupling of intersecting neutrino trajectories and the associated nonlinearity which characterizes neutrino flavor conversion. We describe here the two codes developed to attack this problem. We also describe the surprising phenomena revealed by these numerical calculations. Chief among these is that the nonlinearities in the problem can engineer neutrino flavor transformation which is dramatically different than in standard Mikheyev-Smirnov-Wolfenstein treatments. This happens even though the neutrino mass-squared differences are measured to be small, and even when neutrino self-coupling is sub-dominant. Our numerical work has revealed potential signatures which, if detected in the neutrino burst from a Galactic core collapse event, could reveal heretofore unmeasurable properties of the neutrinos, such as the mass hierarchy and vacuum mixing angle theta_13.

Huaiyu Duan; George M. Fuller; J. Carlson

2008-03-26

233

Effects of Spin-Flavor Conversion in Supernova Neutrino Signal  

SciTech Connect

Majorana neutrinos with a finite transition magnetic moment are expected to convert their flavors by spin precession in a strong magnetic field of a supernova. We investigate detailed dependence of the resonant spin-flavor conversions on electron fraction Y{sub e} in the innermost region of the supernova assuming the inverted mass hierarchy. The observed supernova v-bar{sub e} spectrum is expected to be larger in Y{sub e}>0.5 than that in Y{sub e}<0.5. Therefore, the time variation of supernova v-bar{sub e} signal would indicate Majorana neutrinos with a finite transition magnetic moment.

Yoshida, Takashi [Division of Theoretical Astronomy, National Astronomical Observatory of Japan (Japan); Takamura, Akira [Department of Mathematics, Toyota National College of Technology (Japan); Kimura, Keiichi; Yokomakura, Hidekazu [Department of Physics, Graduate School of Science, Nagoya University (Japan); Kawagoe, Shiou [Department of Astronomy, Graduate School of Science, University of Tokyo (Japan); Kajino, Toshitaka [Division of Theoretical Astronomy, National Astronomical Observatory of Japan (Japan); Department of Astronomy, Graduate School of Science, University of Tokyo (Japan)

2009-05-04

234

Neutrino oscillation constraints on neutrinoless double-beta decay  

NASA Astrophysics Data System (ADS)

We have studied the constraints imposed by the results of neutrino oscillation experiments on the effective Majorana mass \\|\\| that characterizes the contribution of Majorana neutrino masses to the matrix element of neutrinoless double-beta decay. We have shown that in a general scheme with three Majorana neutrinos and a hierarchy of neutrino masses (which corresponds to the standard seesaw mechanism) the results of neutrino oscillation experiments imply rather strong constraints on the parameter \\|\\|. From the results of the first reactor long-baseline experiment CHOOZ and the Bugey experiment it follows that \\|\\|<~3×10-2 eV if ?m2<~2 eV2 (?m2 is the largest mass-squared difference). Hence, we conclude that the observation of neutrinoless double-beta decay with a probability that corresponds to \\|\\|>~10-1 eV would be a signal for a nonhierarchical neutrino mass spectrum and/or nonstandard mechanisms of lepton number violation.

Bilenky, S. M.; Giunti, C.; Kim, C. W.; Monteno, M.

1998-06-01

235

Physics in Action: Neutrino Astrophysics  

NSDL National Science Digital Library

This site provides information about the importance of neutrinos in stellar astronomy. It uses the famous supernova 1987A as an example of the energy carried by neutrinos. More information on supernovae and the solar neutrino question are provided, along with links to research.

Central, Physics

2004-04-08

236

Where are the beryllium neutrinos?  

E-print Network

We show that present experiments imply that neutrinos are nonstandard at the 87\\% C.L., independently of solar or nuclear physics. Moreover, if neutrinos are standard, the $^7$Be flux must be almost zero. Even if we arbitrarily disregard one of the experiments, the neutrino flux must still be less than half of the value predicted by standard solar models.

S. Degl'Innocenti; G. Fiorentini; M. Lissia

1994-08-30

237

Electromagnetic neutrino: a short review  

E-print Network

A short review on selected issues related to the problem of neutrino electromagnetic properties is given. After a flash look at the theoretical basis of neutrino electromagnetic form factors, constraints on neutrino magnetic moments and electric millicharge from terrestrial experiments and astrophysical observations are discussed. We also focus on some recent studies of the problem and on perspectives.

Alexander I. Studenikin

2014-11-09

238

Electromagnetic neutrino: a short review  

E-print Network

A short review on selected issues related to the problem of neutrino electromagnetic properties is given. After a flash look at the theoretical basis of neutrino electromagnetic form factors, constraints on neutrino magnetic moments and electric millicharge from terrestrial experiments and astrophysical observations are discussed. We also focus on some recent studies of the problem and on perspectives.

Studenikin, Alexander I

2014-01-01

239

Supernova Neutrinos Detection On Earth  

E-print Network

In this paper, we first discuss the detection of supernova neutrino on Earth. Then we propose a possible method to acquire information about $\\theta_{13}$ smaller than $1.5^\\circ$ by detecting the ratio of the event numbers of different flavor supernova neutrinos. Such an sensitivity cannot yet be achieved by the Daya Bay reactor neutrino experiment.

Xin-Heng Guo; Ming-Yang Huang; Bing-Lin Young

2009-05-11

240

Relic neutrinos: Physically consistent treatment of effective number of neutrinos and neutrino mass  

NASA Astrophysics Data System (ADS)

We perform a model independent study of the neutrino momentum distribution at freeze-out, treating the freeze-out temperature as a free parameter. Our results imply that measurement of neutrino reheating, as characterized by the measurement of the effective number of neutrinos N?, amounts to the determination of the neutrino kinetic freeze-out temperature within the context of the standard model of particle physics where the number of neutrino flavors is fixed and no other massless (fractional) particles arise. At temperatures on the order of the neutrino mass, we show how cosmic background neutrino properties, i.e., energy density, pressure, and particle density, are modified in a physically consistent way as a function of neutrino mass and N?.

Birrell, Jeremiah; Yang, Cheng-Tao; Chen, Pisin; Rafelski, Johann

2014-01-01

241

Extraterrestrial Solar Neutrino Physics  

E-print Network

We advocate the extraterrestrial solar neutrino physics (etSNP) as a means of investigating solar neutrino physics (SNP). As we already know, the dominant and subdominant (vacuum) oscillation lengths would be approximately one kilometer and one hundred kilometers. On the other hand, we know so far that the matter-enhanced oscillations take place only in the core of the Sun. Thus, the etSNP, i.e. solar neutrino physics that could be extracted outside the Earth, would assume a special unique role. The etSNP experiments include (1) a satellite (detector) around the Earth or around the Jupiter or others (to provide the shadow, for the matter-enhanced neutrino oscillations), (2) during the Sun-Venus-Earth eclipse or similar, and (3) the chemical compositions of the geology type (as in the Jupiter or in the Venus, to study the origins of these planets). To be specific, we note that the reactions induced by the ^8B solar neutrinos, in view of the sole high energy nature (E_\

W-Y. Pauchy Hwang; Jen-Chieh Peng

2010-03-23

242

Neutrino oscillations: brief history and present status  

E-print Network

A brief review of the problem of neutrino masses and oscillations is given. In the beginning we present an early history of neutrino masses, mixing and oscillations. Then we discuss all possibilities of neutrino masses and mixing (neutrino mass terms). The phenomenology of neutrino oscillations in vacuum is considered in some details. We present also the neutrino oscillation data and the seesaw mechanism of the neutrino mass generation.

S. M. Bilenky

2014-08-12

243

KATRIN: an experiment to measure the neutrino mass  

E-print Network

KATRIN is a very large scale tritium-beta-decay experiment to determine the mass of the neutrino. It is presently under construction at the Forschungszentrum Karlsruhe, and makes use of the Tritium Laboratory built there for the ITER project. The combination of a very large retarding-potential electrostatic-magnetic spectrometer and an intense gaseous molecular tritium source makes possible a sensitivity to neutrino mass of 0.2 eV, about an order of magnitude below present laboratory limits. The measurement is kinematic and independent of whether the neutrino is Dirac or Majorana. The status of the project is summarized briefly in this report.

R. G. H. Robertson; for the KATRIN Collaboration

2007-12-23

244

Limits on neutrino-neutrino scattering in the early Universe  

NASA Astrophysics Data System (ADS)

In the standard model neutrinos are assumed to have streamed across the Universe since they last scattered when the standard-model plasma temperature was ˜MeV . The shear stress of free-streaming neutrinos imprints itself gravitationally on the cosmic microwave background (CMB) and makes the CMB a sensitive probe of neutrino scattering. Yet, the presence of nonstandard physics in the neutrino sector may alter this standard chronology and delay neutrino free streaming until a much later epoch. We use observations of the CMB to constrain the strength of neutrino self interactions Geff and put limits on new physics in the neutrino sector from the early Universe. Within the context of conventional ? CDM parameters cosmological data are compatible with Geff?1 /(56 MeV )2 and neutrino free streaming might be delayed until their temperature has cooled to as low as ˜25 eV . Intriguingly, we also find an alternative cosmology compatible with cosmological data in which neutrinos scatter off each other until z ˜1 04 with a preferred interaction strength in a narrow region around Geff?1 /(10 MeV )2?8.6 ×1 08GF , where GF is the Fermi constant. This distinct self-interacting neutrino cosmology is characterized by somewhat lower values of both the scalar spectral index and the amplitude of primordial fluctuations. While we phrase our discussion here in terms of a specific scenario, our constraints on the neutrino visibility function are very general.

Cyr-Racine, Francis-Yan; Sigurdson, Kris

2014-12-01

245

Signatures of the neutrino mass hierarchy in supernova neutrinos  

E-print Network

The undetermined neutrino mass hierarchy may leave observable imprint on the neutrino fluxes from the core-collpse supernova (SN). The interpretation of the observables, however, is subject to the uncertain SN models and the flavor conversion mechanism of neutrinos in a SN. We attempt to propose a qualitative and model-independent interpretation of the expected neutrino events at terrestrial detectors, focusing on the accretion phase of the neutrino burst. The flavor conversions due to the neutrino self-interaction, the MSW effect, and the Earth regeneration effect are incorporated in the calculation. It leads to several distinct scenarios that are identified by the neutrino mass hierarchies and the collective flavor transitions. Consequences resulting from the variation of incident angles and SN models are also discussed.

S. H. Chiu; Chu-Ching Huang; Kwang-Chang Lai

2014-04-07

246

Plasmon decay to a neutrino pair via neutrino electromagnetic moments in a strongly magnetized medium  

E-print Network

We calculate the neutrino luminosity of a degenerate electron gas in a strong magnetic field via plasmon decay to a neutrino pair due to neutrino electromagnetic moments and obtain the relative upper bounds on the effective neutrino magnetic moment.

A. V. Borisov; P. E. Sizin

2014-06-12

247

Neutrinoless Double Beta Decay - and the Neutrino Mass Matrix  

NASA Astrophysics Data System (ADS)

Double beta decay is indispensable to solve the question of the neutrino mass matrix together with ? oscillation experiments. Recent analysis of the most sensitive experiment since eight years - the HEIDELBERG-MOSCOW experiment in Gran-Sasso - yields evidence for the neutrinoless decay mode. This result is the first evidence for lepton number violation and proves the neutrino to be a Majorana particle. We give the present status of the analysis in these Proceedings. It excludes several of the neutrino mass scenarios allowed from present neutrino oscillation experiments - essentially only degenerate and partially degenerate mass scenarios survive. This result allows neutrinos to still play an important role as dark matter in the Universe. To improve the present result, considerably enlarged experiments are required, such as GENIUS. A GENIUS Test Facility has just been funded and will come into operation by end of 2002.

Klapdor-Kleingrothaus, H. V.

2002-04-01

248

Enhanced solar anti-neutrino flux in random magnetic fields  

E-print Network

We discuss the impact of the recent KamLAND constraint on the solar anti-neutrino flux on the analysis of solar neutrino data in the presence of Majorana neutrino transition magnetic moments and solar magnetic fields. We consider different stationary solar magnetic field models, both regular and random, highlighting the strong enhancement in the anti-neutrino production rates that characterize turbulent solar magnetic field models. Moreover, we show that for such magnetic fields inside the Sun, one can constrain the intrinsic neutrino magnetic moment down to the level of mu_nu lessthan few times 10^-12 x mu_B irrespective of details of the underlying turbulence model. This limit is more stringent than all current experimental sensitivities, and similar to the most stringent bounds obtained from stellar cooling. We also comment on the robustness of this limit and show that at most it might be weakened by one order of magnitude, under very unlikely circumstances.

O. G. Miranda; T. I. Rashba; A. I. Rez; J. W. F. Valle

2004-10-13

249

A Mechanism for Ordinary-Sterile Neutrino Mixing  

E-print Network

Efficient oscillations between ordinary (active) and sterile neutrinos can occur only if Dirac and Majorana mass terms exist which are both small and comparable. It is shown that this can occur naturally in a class of string models, in which higher-dimensional operators in the superpotential lead to an intermediate scale expectation value for a scalar field and to suppressed Dirac and Majorana fermion masses.

Paul Langacker

1998-07-24

250

The neutrino signal at HALO: learning about the primary supernova neutrino fluxes and neutrino properties  

SciTech Connect

Core-collapse supernova neutrinos undergo a variety of phenomena when they travel from the high neutrino density region and large matter densities to the Earth. We perform analytical calculations of the supernova neutrino fluxes including collective effects due to the neutrino-neutrino interactions, the Mikheev-Smirnov-Wolfenstein (MSW) effect due to the neutrino interactions with the background matter and decoherence of the wave packets as they propagate in space. We predict the numbers of one- and two-neutron charged and neutral-current electron-neutrino scattering on lead events. We show that, due to the energy thresholds, the ratios of one- to two-neutron events are sensitive to the pinching parameters of neutrino fluxes at the neutrinosphere, almost independently of the presently unknown neutrino properties. Besides, such events have an interesting sensitivity to the spectral split features that depend upon the presence/absence of energy equipartition among neutrino flavors. Our calculations show that a lead-based observatory like the Helium And Lead Observatory (HALO) has the potential to pin down important characteristics of the neutrino fluxes at the neutrinosphere, and provide us with information on the neutrino transport in the supernova core.

Väänänen, Daavid; Volpe, Cristina, E-mail: vaananen@ipno.in2p3.fr, E-mail: volpe@ipno.in2p3.fr [Institut de Physique Nucléaire, F-91406 Orsay cedex, CNRS/IN2P3 and University of Paris-XI (France)

2011-10-01

251

Popcorn Neutrino Lab  

NSDL National Science Digital Library

Students will participate in a modeling activity that simulates the cyclical role of experimental and theoretical science. Initially, the students will measure the mass of popcorn kernels. While the mass of the kernels are determined, students will also make predictions of the mass of the kernels after they are popped. After the popcorn is popped, the mass of the popcorn is measured. Data is shared and students articulate theories that explain why the masses do not agree. After the experiment, the topic of neutrinos is introduced. Essentially, the unpopped kernels represent neutrons and the popped kernels represent protons, electrons, and neutrinos. As students relate the experiment to the theoretical discovery of the neutrino, dialogue can follow discussing the strengths and weaknesses of the model.

Petula, Jason

252

Entanglement in neutrino oscillations  

E-print Network

Flavor oscillations in elementary particle physics are related to multi-mode entanglement of single-particle states. We show that mode entanglement can be expressed in terms of flavor transition probabilities, and therefore that single-particle entangled states acquire a precise operational characterization in the context of particle mixing. We treat in detail the physically relevant cases of two- and three-flavor neutrino oscillations, including the effective measure of CP violation. We discuss experimental schemes for the transfer of the quantum information encoded in single-neutrino states to spatially delocalized two-flavor charged lepton states, thus showing, at least in principle, that single-particle entangled states of neutrino mixing are legitimate physical resources for quantum information tasks.

Massimo Blasone; Fabio Dell'Anno; Silvio De Siena; Fabrizio Illuminati

2009-04-17

253

Neutrino physics: Summary talk  

SciTech Connect

This paper is organized as follows: First, I describe the state of neutrino phenomenology. Emphasis is placed on sin/sup 2/ /theta//sub W/, its present status and future prospects. In addition, some signatures of ''new physics'' are described. Then, kaon physics at Fermilab is briefly discussed. I concentrate on the interesting rare decay K/sub L/ /yields/ /pi//sup 0/e/sup +/e/sup /minus// which may be a clean probe direct CP violation. Neutrino mass, mixing, and electromagnetic moments are surveyed. There, I describe the present state and future direction of accelerator based experiments. Finally, I conclude with an outlook on the future. Throughout this summary, I have drawn from and incorporated ideas discussed by other speakers at this workshop. However, I have tried to combine their ideas with my own perspective on neutrino physics and where it is headed. 49 refs., 3 figs., 4 tabs.

Marciano, W.J.

1989-04-01

254

Tritium neutrino mass experiments  

SciTech Connect

The current status of the experimental search for neutrino mass is reviewed, with emphasis on direct kinematic methods, such as the beta decay of tritium. The situation concerning the electron neutrino mass as measured in tritium beta decay is essentially unchanged from a year ago, although a great deal of experimental work is in progress. The ITEP group continues to find evidence for a nonzero mass, now slightly revised to 26(5) eV. After correcting for recently discovered errors in the energy loss distribution and source thickness, however, the Z/umlt u/rich group still claims and upper limit of 18 eV. There may be evidence for neutrino mass and mixing in the SN1987a data, in the same range suggested by the ITEP experiment. 42 refs., 3 figs.

Robertson, R.G.H.

1988-01-01

255

Resonant solar neutrino oscillation experiments  

SciTech Connect

The results of a detailed calculation of the effects of resonant neutrino oscillations in the sun on the current and proposed solar neutrino experiments are presented. Analytic results are used for the electron-neutrino survival probability so that a sophisticated model for both the production distribution of the solar neutrino sources and the solar electron-number density can be employed. Contour plots for the electron-neutrino capture rate, in the mass-difference-squared versus vacuum-mixing-angle plane, are given for the current /sup 37/Cl experiment and the proposed /sup 71/Ga detector.

Parke, S.J.; Walker, T.P.

1986-11-03

256

Solar neutrino experiments  

Microsoft Academic Search

New results are presented for absorption cross sections of nine possible detectors of solar neutrinos (⁷Li, ³⁷Cl, ⁵¹V, ⁵⁵Mn, ⁷¹Ga, ⁸¹Br, ⁸⁷Rb, ¹¹⁵In, and ²°⁵Tl). Special attention is given to nuclear physics uncertainties. The calculated cross sections are used (with the aid of illustrative solar models and ad hoc assumptions about neutrino propagation) to discuss what can be learned about

John Bahcall

1978-01-01

257

Neutrinos from Auger Sources  

E-print Network

The Pierre Auger observatory has presented evidence that the arrival directions of cosmic rays with energies in excess of 6x10^7 TeV may be correlated with nearby active galactic nuclei (AGN). In this context we revisit a suggestion based on gamma ray observations that nearby Fanaroff-Riley I galaxies such as Cen A and M87 are the sources of the local cosmic rays. We compute the accompanying neutrino flux and find a flux within reach of second-generation kilometer-scale neutrino telescopes.

Francis Halzen; Aongus O'Murchadha

2008-02-28

258

Neutrino Telescopes in Antarctica  

NASA Astrophysics Data System (ADS)

It is hoped that in the near future neutrino astronomy will reach throughout and beyond our galaxy and make measurements relevant to cosmology, astrophysics, cosmic-ray and particle physics. The construction of a high-energy neutrino telescope requires a huge volume of very transparent, deeply buried material such as ocean water or ice, which acts as the medium for detecting the particles. I will describe two experiments using Antarctic ice as this medium: the AMANDA experiment employing photomultiplier tubes and RICE utilising radio receivers.

Adams, Jenni

2000-04-01

259

Neutrinos Have Mass - So What?  

E-print Network

In this brief review, I discuss the new physics unveiled by neutrino oscillation experiments over the past several years, and discuss several attempts at understanding the mechanism behind neutrino masses and lepton mixing. It is fair to say that, while significant theoretical progress has been made, we are yet to construct a coherent picture that naturally explains non-zero, yet tiny, neutrino masses and the newly revealed, puzzling patterns of lepton mixing. I discuss what the challenges are, and point to the fact that more experimental input (from both neutrino and non-neutrino experiments) is dearly required - and that new data is expected to reveal, in the next several years, new information. Finally, I draw attention to the fact that neutrinos may have only just begun to reshape fundamental physics, given the fact that we are still to explain the LSND anomaly and because the neutrino oscillation phenomenon is ultimately sensitive to very small new-physics effects.

Andre de Gouvea

2005-03-09

260

ccsd-00016511,version1-5Jan2006 Neutrino Physics/Physique des neutrinos  

E-print Network

ccsd-00016511,version1-5Jan2006 Neutrino Physics/Physique des neutrinos Reactor Neutrinos Thierry Abstract We review the status and the results of reactor neutrino experiments, that toe the cutting edge of neutrino research. Short baseline experiments have provided the measurement of the reactor neutrino

Boyer, Edmond

261

The JHF-Kamioka neutrino project  

Microsoft Academic Search

The JHF-Kamioka neutrino project is a second generation long base line neutrino oscillation experiment that probes physics beyond the Standard Model by high precision measurements of the neutrino masses and mixing. A high intensity narrow band neutrino beam is produced by secondary pions created by a high intensity proton synchrotron at JHF (JAERI). The neutrino energy is tuned to the

Y. Itow; T. Kajita; K. Kaneyuki; M. Shiozawa; Y. Totsuka; Y. Hayato; T. Ishida; T. Ishii; T. Kobayashi; T. Maruyama; K. Nakamura; Y. Obayashi; Y. Oyama; M. Sakuda; M. Yoshida; S. Aoki; T. Hara; A. Suzuki; A. Ichikawa; T. Nakaya; K. Nishikawa; T. Hasegawa; K. Ishihara; A. Konaka

2001-01-01

262

Neutrinos from a core collapse supernova  

E-print Network

The neutrino burst from a galactic supernova can help determine the neutrino mass hierarchy and $\\theta_{13}$, and provide crucial information about supernova astrophysics. Here we review our current understanding of the neutrino burst, flavor conversions of these neutrinos, and model independent signatures of various neutrino mixing scenarios.

Amol Dighe

2007-12-28

263

Review of the physics of the neutrino  

SciTech Connect

The status of knowledge with respect to neutrinos is reviewed. Questions covered briefly include whether or not a neutrino is its own antiparticle and neutrino mass. Experimental studies are also considered, including neutrino oscillations, double beta decay, and direct neutrino mass measurements. (LEW)

Robertson, R.G.H.

1986-01-01

264

Probing Pseudo-Dirac Neutrino through Detection of Neutrino Induced Muons from GRB Neutrinos  

E-print Network

The possibility to verify the pseudo-Dirac nature of neutrinos is investigated here via the detection of ultra high energy neutrinos from distant cosmological objects like GRBs. The very long baseline and the energy range from $\\sim$ TeV to $\\sim$ EeV for such neutrinos invokes the likelihood to probe very small pseude-Dirac splittings. The expected secondary muons from such neutrinos that can be detected by a kilometer scale detector such as ICECUBE is calculated. The pseudo-Dirac nature, if exists, will show a considerable departure from flavour oscillation scenario in the total yield of the secondary muons induced by such neutrinos.

Debasish Majumdar

2006-07-31

265

Observables sensitive to absolute neutrino masses: Constraints and correlations from world neutrino data  

SciTech Connect

In the context of three-flavor neutrino mixing, we present a thorough study of the phenomenological constraints applicable to three observables sensitive to absolute neutrino masses: The effective neutrino mass in Tritium beta-decay (m{sub {beta}}); the effective Majorana neutrino mass in neutrinoless double beta-decay (m{sub {beta}}{sub {beta}}); and the sum of neutrino masses in cosmology ({sigma}). We discuss the correlations among these variables which arise from the combination of all the available neutrino oscillation data, in both normal and inverse neutrino mass hierarchy. We set upper limits on m{sub {beta}} by combining updated results from the Mainz and Troitsk experiments. We also consider the latest results on m{sub {beta}}{sub {beta}} from the Heidelberg-Moscow experiment, both with and without the lower bound claimed by such experiment. We derive upper limits on {sigma} from an updated combination of data from the Wilkinson Microwave Anisotropy Probe (WMAP) satellite and the two degrees Fields (2dF) Galaxy Redshifts Survey, with and without Lyman-{alpha} forest data from the Sloan Digital Sky Survey (SDSS), in models with a nonzero running of the spectral index of primordial inflationary perturbations. The results are discussed in terms of two-dimensional projections of the globally allowed region in the (m{sub {beta}},m{sub {beta}}{sub {beta}},{sigma}) parameter space, which neatly show the relative impact of each data set. In particular, the (in)compatibility between {sigma} and m{sub {beta}}{sub {beta}} constraints is highlighted for various combinations of data. We also briefly discuss how future neutrino data (both oscillatory and nonoscillatory) can further probe the currently allowed regions.

Fogli, G.L.; Lisi, E.; Marrone, A.; Palazzo, A. [Dipartimento di Fisica and Sezione INFN di Bari, Via Amendola 173, 70126, Bari (Italy); Melchiorri, A.; Serra, P. [Dipartimento di Fisica and Sezione INFN, Universita degli Studi di Roma 'La Sapienza', P.le Aldo Moro 5, 00185, Rome (Italy); Silk, J. [Astrophysics, Denys Wilkinson Building, Keble Road, OX13RH, Oxford (United Kingdom)

2004-12-01

266

Fireball Heated by Neutrinos  

E-print Network

The fireball, the promising model of the gamma-ray burst (GRB), is an opaque radiation plasma, whose energy is significantly greater than its rest mass. We numerically simulate the evolution of the fireball heated by the neutrino-antineutrino annihilation process for the spherically symmetric case. We also derive analytical energy and momentum deposition rates via neutrino scattering with thermalized electron-positron pairs in the fireball. In our simulation the matter is provided around the neutrinosphere before neutrinos start to be emitted, and the energy is injected during a finite period of time $t_{\\rm dur}$. In the acceleration regime the matter shell is pushed from behind by radiation pressure. The Lorentz factor of the shell reaches the maximum value $\\eta$ at $r \\simeq \\eta^2 c t_{\\rm dur}$. After the fireball enters the coasting regime, the velocity distribution in the shell becomes very flat. The shell expansion rate $d W/dr$ can be much smaller than $\\eta^{-2}$. The runaway of temperature of the fireball due to neutrino scattering with electron-positron pairs does not occur in most cases. The energy deposition due to scattering is not so significant.

Katsuaki Asano; Shizuo Iwamoto

2002-10-05

267

Neutrinos from Protoneutron Stars  

E-print Network

We study the diffusive transport of neutrinos in a newly born neutron star to explore its sensitivity to dense matter properties. Energy and lepton number which are trapped during the catastrophic implosion diffuse out on the time scale of a few tens of seconds. Results for different dense matter models are presented.

S. Reddy; J. Pons; M. Prakash; J. M. Lattimer

1998-02-24

268

Bounds on the tau and muon neutrino vector and axial vector charge radius  

E-print Network

A Majorana neutrino is characterized by just one flavor diagonal electromagnetic form factor: the anapole moment, that in the static limit corresponds to the axial vector charge radius . Experimental information on this quantity is scarce, especially in the case of the tau neutrino. We present a comprehensive analysis of the available data on the single photon production process $e^+ e^- -> \

Martin Hirsch; Enrico Nardi; Diego Restrepo

2002-10-09

269

A See-Saw Mechanism for Large Neutrino Mixing from Small Quark and Lepton Mixings  

E-print Network

I introduce and sketch the main features of those see-saw models where a large atmospheric mixing can be achieved starting from nearly diagonal matrices for charged leptons, Dirac neutrinos and Majorana right-handed neutrinos. It turns out that these models can be realized in Grand Unified Theories and they are well compatible with the related phenomenology of fermion masses and mixings.

Isabella Masina

2000-05-24

270

Neutrino Oscillations, SUSY See-Saw Mechanism and Charged Lepton Flavor Violation  

E-print Network

Neutrino oscillations give clear evidence for non-vanishing neutrino masses and lepton-flavor violation (LFV) in the neutrino sector. This provides strong motivation to search for signals of LFV also in the charged lepton sector, and to probe the SUSY see-saw mechanism. We compare the sensitivity of rare radiative decays on the right-handed Majorana mass scale M_R with the reach in slepton-pair production at a future linear collider.

F. Deppisch; H. Päs; A. Redelbach; R. Rückl; Y. Shimizu

2002-11-11

271

Z_3 Dark Matter and Two-Loop Neutrino Mass  

E-print Network

Dark matter is usually distinguished from ordinary matter by an odd-even parity, i.e. the discrete symmetry Z_2. The new idea of Z_3 dark matter is proposed with a special application to generating radiative Majorana neutrino masses in two-loop order.

Ernest Ma

2007-09-05

272

Measurement of Atmospheric Neutrino Oscillations with the ANTARES Neutrino Telescope  

E-print Network

The data taken with the ANTARES neutrino telescope from 2007 to 2010, a total live time of 863 days, are used to measure the oscillation parameters of atmospheric neutrinos. Muon tracks are reconstructed with energies as low as 20 GeV. Neutrino oscillations will cause a suppression of vertical upgoing muon neutrinos of such energies crossing the Earth. The parameters determining the oscillation of atmospheric neutrinos are extracted by fitting the event rate as a function of the ratio of the estimated neutrino energy and reconstructed flight path through the Earth. Measurement contours of the oscillation parameters in a two-flavour approximation are derived. Assuming maximum mixing, a mass difference of $\\Delta m_{32}^2=(3.1\\pm 0.9)\\cdot 10^{-3}$ eV$^2$ is obtained, in good agreement with the world average value.

ANTARES collaboration; S. Adrian-Martinez; I. Al Samarai; A. Albert; M. Andre; M. Anghinolfi; G. Anton; S. Anvar; M. Ardid; T. Astraatmadja; J. -J. Aubert; B. Baret; S. Basa; V. Bertin; S. Biagi; C. Bigongiari; C. Bogazzi; M. Bou-Cabo; B. Bouhou; M. C. Bouwhuis; J. Brunner; J. Busto; A. Capone; C. Carloganu; J. Carr; S. Cecchini; Z. Charif; Ph. Charvis; T. Chiarusi; M. Circella; R. Coniglione; L. Core; H. Costantini; P. Coyle; A. Creusot; C. Curtil; G. De Bonis; M. P. Decowski; I. Dekeyser; A. Deschamps; C. Distefano; C. Donzaud; D. Dornic; Q. Dorosti; D. Drouhin; T. Eberl; U. Emanuele; A. Enzenhoefer; J. -P. Ernenwein; S. Escoffier; K. Fehn; P. Fermani; M. Ferri; S. Ferry; V. Flaminio; F. Folger; U. Fritsch; J. -L. Fuda; S. Galata; P. Gay; K. Geyer; G. Giacomelli; V. Giordano; A. Gleixner; J. P. Gomez-Gonzalez; K. Graf; G. Guillard; G. Hallewell; M. Hamal; H. van Haren; A. J. Heijboer; Y. Hello; J. J. Hernandez-Rey; B. Herold; J. Hoessl; C. C. Hsu; M. de Jong; M. Kadler; O. Kalekin; A. Kappes; U. Katz; O. Kavatsyuk; P. Kooijman; C. Kopper; A. Kouchner; I. Kreykenbohm; V. Kulikovskiy; R. Lahmann; G. Lambard; G. Larosa; D. Lattuada; D. Lefevre; G. Lim; D. Lo Presti; H. Loehner; S. Loucatos; F. Louis; S. Mangano; M. Marcelin; A. Margiotta; J. A. Martinez-Mora; A. Meli; T. Montaruli; M. Morganti; L. Moscoso; H. Motz; M. Neff; E. Nezri; D. Palioselitis; G. E. Pavalas; K. Payet; J. Petrovic; P. Piattelli; V. Popa; T. Pradier; E. Presani; C. Racca; C. Reed; G. Riccobene; C. Richardt; R. Richter; C. Riviere; A. Robert; K. Roensch; A. Rostovtsev; J. Ruiz-Rivas; M. Rujoiu; G. V. Russo; D. F. E. Samtleben; A. Sanchez-Losa; P. Sapienza; J. Schmid; J. Schnabel; F. Schoeck; J. -P. Schuller; F. Schuessler; T. Seitz; R. Shanidze; F. Simeone; A. Spies; M. Spurio; J. J. M. Steijger; Th. Stolarczyk; M. Taiuti; C. Tamburini; A. Trovato; B. Vallage; C. Vallee; V. Van Elewyck; M. Vecchi; P. Vernin; E. Visser; S. Wagner; G. Wijnker; J. Wilms; E. de Wolf; H. Yepes; D. Zaborov; J. D. Zornoza; J. Zuniga

2012-07-02

273

Measurement of Atmospheric Neutrino Oscillations with the ANTARES Neutrino Telescope  

E-print Network

The data taken with the ANTARES neutrino telescope from 2007 to 2010, a total live time of 863 days, are used to measure the oscillation parameters of atmospheric neutrinos. Muon tracks are reconstructed with energies as low as 20 GeV. Neutrino oscillations will cause a suppression of vertical upgoing muon neutrinos of such energies crossing the Earth. The parameters determining the oscillation of atmospheric neutrinos are extracted by fitting the event rate as a function of the ratio of the estimated neutrino energy and reconstructed flight path through the Earth. Measurement contours of the oscillation parameters in a two-flavour approximation are derived. Assuming maximum mixing, a mass difference of $\\Delta m_{32}^2=(3.1\\pm 0.9)\\cdot 10^{-3}$ eV$^2$ is obtained, in good agreement with the world average value.

Adrian-Martinez, S; Albert, A; Andre, M; Anghinolfi, M; Anton, G; Anvar, S; Ardid, M; Astraatmadja, T; Aubert, J -J; Baret, B; Basa, S; Bertin, V; Biagi, S; Bigongiari, C; Bogazzi, C; Bou-Cabo, M; Bouhou, B; Bouwhuis, M C; Brunner, J; Busto, J; Capone, A; Carloganu, C; Carr, J; Cecchini, S; Charif, Z; Charvis, Ph; Chiarusi, T; Circella, M; Coniglione, R; Core, L; Costantini, H; Coyle, P; Creusot, A; Curtil, C; De Bonis, G; Decowski, M P; Dekeyser, I; Deschamps, A; Distefano, C; Donzaud, C; Dornic, D; Dorosti, Q; Drouhin, D; Eberl, T; Emanuele, U; Enzenhoefer, A; Ernenwein, J -P; Escoffier, S; Fehn, K; Fermani, P; Ferri, M; Ferry, S; Flaminio, V; Folger, F; Fritsch, U; Fuda, J -L; Galata, S; Gay, P; Geyer, K; Giacomelli, G; Giordano, V; Gleixner, A; Gomez-Gonzalez, J P; Graf, K; Guillard, G; Hallewell, G; Hamal, M; van Haren, H; Heijboer, A J; Hello, Y; Hernandez-Rey, J J; Herold, B; Hoessl, J; Hsu, C C; de Jong, M; Kadler, M; Kalekin, O; Kappes, A; Katz, U; Kavatsyuk, O; Kooijman, P; Kopper, C; Kouchner, A; Kreykenbohm, I; Kulikovskiy, V; Lahmann, R; Lambard, G; Larosa, G; Lattuada, D; Lefevre, D; Lim, G; Presti, D Lo; Loehner, H; Loucatos, S; Louis, F; Mangano, S; Marcelin, M; Margiotta, A; Martinez-Mora, J A; Meli, A; Montaruli, T; Morganti, M; Moscoso, L; Motz, H; Neff, M; Nezri, E; Palioselitis, D; Pavalas, G E; Payet, K; Petrovic, J; Piattelli, P; Popa, V; Pradier, T; Presani, E; Racca, C; Reed, C; Riccobene, G; Richardt, C; Richter, R; Riviere, C; Robert, A; Roensch, K; Rostovtsev, A; Ruiz-Rivas, J; Rujoiu, M; Russo, G V; Samtleben, D F E; Sanchez-Losa, A; Sapienza, P; Schmid, J; Schnabel, J; Schoeck, F; Schuller, J -P; Schuessler, F; Seitz, T; Shanidze, R; Simeone, F; Spies, A; Spurio, M; Steijger, J J M; Stolarczyk, Th; Taiuti, M; Tamburini, C; Trovato, A; Vallage, B; Vallee, C; Van Elewyck, V; Vecchi, M; Vernin, P; Visser, E; Wagner, S; Wijnker, G; Wilms, J; de Wolf, E; Yepes, H; Zaborov, D; Zornoza, J D; Zuniga, J

2012-01-01

274

Flavour-dependent radiative correction to neutrino-neutrino refraction  

E-print Network

In the framework of the Standard Model we calculate the flavour non-universal correction for neutrino refraction in a neutrino background and verify a similar previous result for the case of ordinary-matter background. The dominant term arises at loop level and involves tau leptons circulating in the loop. These O(G_F m_tau^2) corrections to the tree-level potential provide the dominant refractive difference between nu_mu and nu_tau unless the medium contains mu or tau leptons. Our results affect the flavour evolution of dense neutrino gases and may be of interest for collective three-flavour oscillations of supernova neutrinos. We spell out explicitly how these non-universal neutrino-neutrino interactions enter the flavour oscillation equations.

Alessandro Mirizzi; Stefano Pozzorini; Georg G. Raffelt; Pasquale D. Serpico

2009-10-08

275

High Energy Neutrinos: Sources and Fluxes  

E-print Network

We discuss briefly the potential sources of high energy astrophysical neutrinos and show estimates of the neutrino fluxes that they can produce. A special attention is paid to the connection between the highest energy cosmic rays and astrophysical neutrinos.

Todor Stanev

2005-11-22

276

Status of global fits to neutrino oscillations  

Microsoft Academic Search

We review the present status of global analyses of neutrino oscillations, taking into account the most recent neutrino data including the latest KamLAND and K2K updates presented at Neutrino 2004, as well as state-of-the-art solar and atmospheric neutrino flux calculations. We give the two-neutrino solar + KamLAND results, and the two-neutrino atmospheric + K2K oscillation regions, discussing in each case

Michele Maltoni; Thomas Schwetz; Mariam Tórtola; José W. F. Valle

2004-01-01

277

Heavy sterile neutrinos and supernova explosions  

E-print Network

We consider sterile neutrinos with rest masses ~0.2 GeV. Such sterile neutrinos could augment core collapse supernova shock energies by enhancing energy transport from the core to the vicinity of the shock front. The decay of these neutrinos could produce a flux of very energetic active neutrinos, detectable by future neutrino observations from a galactic supernova. The relevant range of sterile neutrino masses and mixing angles can be probed in future laboratory experiments.

George M. Fuller; Alexander Kusenko; Kalliopi Petraki

2008-06-26

278

Collective flavour transitions of supernova neutrinos  

E-print Network

When the neutrino density is very high, as in core-collapse supernovae, neutrino-neutrino interactions are not negligible and can appreciably affect the evolution of flavour. The physics of these phenomena is briefly highlighted, and their effects are shown on observable energy spectra from a future galactic supernova within two-neutrino and three-neutrino frameworks. Detection of such effects could provide a handle on two unknowns: the neutrino mass hierarchy, and the mixing angle theta(13).

Irene Tamborra

2009-05-15

279

Tau Neutrinos at EeV Energies  

NASA Astrophysics Data System (ADS)

Astrophysical sources of ultrahigh energy neutrinos yield tau neutrino fluxes due to neutrino oscillations. At neutrino energies in the EeV range, radio Cherenkov detection methods show promise for detecting these fluxes. We quantify the tau neutrino contributions to the signal in, for example, a detector like the Radio Ice Cherenkov experiment (RICE) for a Z -burst flux prediction. Tau neutrino regeneration in transit through the Earth, including energy loss, is evaluated.

Hall Reno, M.; Dutta, S. Iyer; Mocioiu, I.; Reno, M.H.; Sarcevic, I.

2003-07-01

280

Searching for hep Neutrinos using the Sudbury Neutrino Observatory  

E-print Network

The Sudbury Neutrino Observatory has recently finished its third and final phase, and has accumulated over 1082 days of neutrino data, spanning the energy range from approximately 5-20 MeV. Almost all the observed neutrinos are due to the 8B reaction in the Sun. The so-called hep process (3He + p -> 4He + e + nu_e) also occurs in the Sun, but has not yet been observed. hep neutrino energy endpoint extends above the 8B spectrum. This paper describes the three phase analysis that will ultimately be the most sensitive to this reaction.

Chris Howard; for the SNO Collaboration

2009-05-29

281

Solar neutrino experiments: An update  

SciTech Connect

The situation in solar neutrino physics has changed drastically in the past few years, so that now there are four neutrino experiments in operation, using different methods to look at different regions of the solar neutrino energy spectrum. These experiments are the radiochemical {sup 37}Cl Homestake detector, the realtime Kamiokande detector, and the different forms of radiochemical {sup 71}Ga detectors used in the GALLEX and SAGE projects. It is noteworthy that all of these experiments report a deficit of observed neutrinos relative to the predictions of standard solar models (although in the case of the gallium detectors, the statistical errors are still relatively large). This paper reviews the basic principles of operation of these neutrino detectors, reports their latest results and discusses some theoretical interpretations. The progress of three realtime neutrino detectors that are currently under construction, SuperKamiok, SNO and Borexino, is also discussed.

Hahn, R.L.

1993-12-31

282

Burst Neutrinos from Nitrogen Flash  

E-print Network

Neutrinos give a novel probe to explore deep interior of astrophysical objects, which otherwise is not accessible with optical observations; among notable examples are solar and supernova neutrinos. We show that there is a new class of strong neutrino emission from helium burning, N + alpha --> 18F gamma followed by beta decay 18F --> 18O + e+ + nu_e, that gives a maximum neutrino luminosity of 10^8 times the solar bolometric luminosity at the helium-core flash of a 1 M_sun star, whereas the flash is not observable by optical means. This means that the neutrino flux, of average energy of 0.382 MeV, will be 10% the solar CNO neutrino flux on Earth if the star is located at 10pc.

A. M. Serenelli; M. Fukugita

2005-09-07

283

Probing Superluminal Neutrinos Via Refraction  

E-print Network

One phenomenological explanation of superluminal propagation of neutrinos, which may have been observed by OPERA and MINOS, is that neutrinos travel faster inside of matter than in vacuum. If so neutrinos exhibit refraction inside matter and should exhibit other manifestations of refraction, such as deflection and reflection. Such refraction would be easily detectable through the momentum imparted to appropriately shaped refractive material inserted into the neutrino beam. For NuMI this could be as large as ~10g cm/s. If these effect were found, they would provide new ways of manipulating and detecting neutrinos. Reasons why this scenario seems implausible are given, however it is still worthwhile to conduct simple searches for differential refraction of neutrinos.

Albert Stebbins

2011-10-12

284

Phases of flavor neutrino masses and CP-violation  

NASA Astrophysics Data System (ADS)

For flavor neutrino masses MijPDG (i,j=e,?,?) compatible with the phase convention defined by Particle Data Group (PDG), if neutrino mixings are controlled by small corrections to those with sin ?13=0 denoted by sin ?13?Me?PDG and sin ?13?M??PDG, CP-violating Dirac phase ?CP is calculated to be ?CP?arg[(M??PDG*/tan ?23+M??PDG*)?Me?PDG+MeePDG?Me?PDG*-tan?23Me?PDG?M??PDG*] (mod ?), where ? (i,j=1,2,3) denotes an i-j neutrino mixing angle. If possible neutrino mass hierarchies are taken into account, the main source of ?CP turns out to be ?Me?PDG except for the inverted mass hierarchy with m?-m, where m=mie (i=1,2) stands for a neutrino mass mi accompanied by a Majorana phase ?i for ? giving two CP-violating Majorana phases. We can further derive that ?CP?arg(Me?PDG)-arg(M??PDG) with arg(Me?PDG)?arg(Me?PDG) for the normal mass hierarchy and ?CP?arg(MeePDG)-arg(Me?PDG)+? for the inverted mass hierarchy with m?m. For specific flavor neutrino masses M whose phases arise from M, these phases can be connected with arg(MijPDG) (i,j=e,?,?). As a result, numerical analysis suggests that Dirac CP-violation becomes maximal as |arg(M)| approaches to ?/2 for the inverted mass hierarchy with m?m and for the degenerate mass pattern satisfying the inverted mass ordering and that Majorana CP-violation becomes maximal as |arg(M)| approaches to its maximal value around 0.5 for the normal mass hierarchy. Alternative CP-violation induced by three CP-violating Dirac phases is compared with the conventional one induced by ?CP and two CP-violating Majorana phases.

Yasuè, Masaki

2012-11-01

285

Small neutrino mass from large compactification volumes.  

PubMed

We present an argument in which the scale approximately 0.1 eV associated with neutrino masses naturally appears in a class of (very) large volume compactifications, being tied to a supersymmetry scale of 10(3) GeV and a string scale of 10(11) GeV. The masses are of the Majorana type, and there is no right-handed neutrino within the low-energy field theory. The suppression scale 10(14) GeV is independent of the masses of the heavy states that are integrated out. These kinds of constructions appear naturally in type IIB flux compactifications. However, the arguments that lead to this result rely only on a few geometrical features of the compactification manifold and, hence, can be used independently of string theory. PMID:17678352

Conlon, Joseph P; Cremades, Daniel

2007-07-27

286

Astrophysical and cosmological constraints to neutrino properties  

NASA Technical Reports Server (NTRS)

The astrophysical and cosmological constraints on neutrino properties (masses, lifetimes, numbers of flavors, etc.) are reviewed. The freeze out of neutrinos in the early Universe are discussed and then the cosmological limits on masses for stable neutrinos are derived. The freeze out argument coupled with observational limits is then used to constrain decaying neutrinos as well. The limits to neutrino properties which follow from SN1987A are then reviewed. The constraint from the big bang nucleosynthesis on the number of neutrino flavors is also considered. Astrophysical constraints on neutrino-mixing as well as future observations of relevance to neutrino physics are briefly discussed.

Kolb, Edward W.; Schramm, David N.; Turner, Michael S.

1989-01-01

287

Muon colliders and neutrino factories  

SciTech Connect

Over the last decade there has been significant progress in developing the concepts and technologies needed to produce, capture and accelerate {Omicron}(10{sup 21}) muons/year. This development prepares the way for a new type of neutrino source (Neutrino Factory) and a new type of very high energy lepton-antilepton collider (Muon Collider). This article reviews the motivation, design and R&D for Neutrino Factories and Muon Colliders.

Geer, S.; /Fermilab

2010-09-01

288

Neutrino Opacities in Nuclear Matter  

E-print Network

Neutrino-matter cross sections and interaction rates are central to the core-collapse supernova phenomenon and, very likely, to the viability of the explosion mechanism itself. In this paper, we describe the major neutrino scattering, absorption, and production processes that together influence the outcome of core collapse and the cooling of protoneutron stars. One focus is on energy redistribution and many-body physics, but our major goal is to provide a useful resource for those interested in supernova neutrino microphysics.

Adam Burrows; Sanjay Reddy; Todd A. Thompson

2004-04-21

289

MINOS Search for Sterile Neutrinos  

E-print Network

Using a NuMI beam exposure of 7.1 /times 10^20 protons-on-target, the MINOS long-baseline experiment has performed a search for active to sterile neutrino mixing over a distance of 735 km. Details of the analysis are provided, along with results from comparisons with standard three neutrino oscillations and fits to a 3+1 model including oscillations into one sterile neutrino. An outlook on the future sterile neutrino related contributions from MINOS and the proposed MINOS+ project is also presented.

Alexandre Sousa; on behalf of the MINOS Collaboration

2011-10-16

290

50 Years of Neutrino Physics  

E-print Network

Some important topics from history of neutrino physics over the last fifty years are discussed. History of neutrinos is older, at 4th December 2010 it will be eightieth anniversary of the "neutrino birth". In that day W. Pauli wrote the famous letter to participants of the physics conference at Tubingen with the suggestion that "there could exist in the nuclei electrically neutral particle". We will concentrate mostly on the 50 years of neutrino history just to show the long tradition of the Zakopane Theoretical School.

Marek Zralek

2010-12-10

291

Neutrino helicity asymmetries in leptogenesis  

E-print Network

It is pointed out that the heavy singlet neutrinos characteristic of leptogenesis develop asymmetries in the abundances of the two helicity states as a result of the same mechanism that generates asymmetries in the standard lepton sector. Neutrinos and standard leptons interchange asymmetries in collisions with each other. It is shown that an appropriate quantum number, B-L', combining baryon, lepton and neutrino asymmetries, is not violated as fast as the standard B-L. This suppresses the washout effects relevant for the derivation of the final baryon asymmetry. One presents detailed calculations for the period of neutrino thermal production in the framework of the singlet seesaw mechanism.

Luis Bento; Francisco C. Santos

2005-06-18

292

Neutrino helicity asymmetries in leptogenesis  

SciTech Connect

It is pointed out that the heavy singlet neutrinos characteristic of leptogenesis develop asymmetries in the abundances of the two helicity states as a result of the same mechanism that generates asymmetries in the standard lepton sector. Neutrinos and standard leptons interchange asymmetries in collisions with each other. It is shown that an appropriate quantum number, B-L{sup '}, combining baryon, lepton and neutrino asymmetries, is not violated as fast as the standard B-L. This suppresses the washout effects relevant for the derivation of the final baryon asymmetry. One presents detailed calculations for the period of neutrino thermal production in the framework of the singlet seesaw mechanism.

Bento, Luis; Santos, Francisco C. [Universidade de Lisboa, Faculdade de Ciencias, Centro de Fisica Nuclear da Universidade de Lisboa, Avenida Prof. Gama Pinto 2, 1649-003 Lisbon (Portugal)

2005-05-01

293

Proton and Neutrino Extragalactic Astronomy  

E-print Network

The study of extragalactic sources of high energy radiation via the direct measurement of the proton and neutrino fluxes that they are likely to emit is one of the main goals for the future observations of the recently developed air showers detectors and neutrino telescopes. In this work we discuss the relation between the inclusive proton and neutrino signals from the ensemble of all sources in the universe, and the resolved signals from the closest and brightest objects. We also compare the sensitivities of proton and neutrino telescopes and comment on the relation between these two new astronomies.

Paolo Lipari

2008-08-04

294

Supernova neutrinos and explosive nucleosynthesis  

SciTech Connect

Core-collapse supernovae eject huge amount of flux of energetic neutrinos. We studied the explosive nucleosyn-thesis in supernovae and found that several isotopes {sup 7}Li, {sup 11}B, {sup 92}Nb, {sup 138}La and {sup 180}Ta as well as r-process nuclei are affected by the neutrino interactions. The abundance of these isotopes therefore depends strongly on the neutrino flavor oscillation due to the Mikheyev-Smirnov-Wolfenstein (MSW) effect. We discuss first how to determine the neutrino temperatures in order to explain the observed solar system abundances of these isotopes, combined with Galactic chemical evolution of the light nuclei and the heavy r-process elements. We then study the effects of neutrino oscillation on their abundances, and propose a novel method to determine the still unknown neutrino oscillation parameters, mass hierarchy and ?{sub 13}, simultaneously. There is recent evidence that SiC X grains from the Murchison meteorite may contain supernova-produced light elements {sup 11}B and {sup 7}Li encapsulated in the presolar grains. Combining the recent experimental constraints on ?{sub 13}, we show that our method sug-gests at a marginal preference for an inverted neutrino mass hierarchy. Finally, we discuss supernova relic neutrinos that may indicate the softness of the equation of state (EoS) of nuclear matter as well as adiabatic conditions of the neutrino oscillation.

Kajino, T. [National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan and Department of Astronomy, Graduate School of Science, The University of Tokyo, Hongo 7-3-1, Bunkyo-ku, Tokyo 113-0033 (Japan); Aoki, W. [National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan); Cheoun, M.-K. [Department of Physics, Soongsil University, Seoul 156-743 (Korea, Republic of); Hayakawa, T. [Japan Atomic Energy Agency, Shirakara-Shirane 2-4, Tokai-mura, Ibaraki 319-1195 (Japan); Hidaka, J.; Hirai, Y.; Shibagaki, S. [National Astronomical Observatory, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan); Mathews, G. J. [Center for Astrophysics, Department of Physics, University of Notre Dame, Notre Dame, IN 46556 (United States); Nakamura, K. [Faculty of Science and Engineering, Waseda University, Ohkubo 3-4-1, Shinjuku, Tokyo 169-8555 (Japan); Suzuki, T. [Department of Physics, College of Humanities and Sciences, Nihon University, Sakurajosui 3-25-40, Setagaya-ku, Tokyo 156-8550 (Japan)

2014-05-09

295

Neutrino clouds and dark matter  

SciTech Connect

We have examined the consequences of assuming the existence of a light scalar boson, weakly coupled to neutrinos, and not coupled to any other light fermions. For a range of parameters, we find that this hypothesis leads to the development of neutrino clusters which form in the early Universe and which provide gravitational fluctuations on scales small compared to a parsec (i.e., the scale of solar systems). Under some conditions, this can produce anomalous gravitational acceleration within solar systems and lead to a vanishing of neutrino mass-squared differences, giving rise to strong neutrino oscillation effects.

Goldman, T. [Los Alamos National Lab., NM (United States); McKellar, B.H.J. [Melbourne Univ., Parkville, VIC (Australia); Stephenson, G.J. Jr. [New Mexico Univ., Albuquerque, NM (United States)

1996-12-31

296

Helioseismology and Beryllium neutrino  

E-print Network

We derive a lower limit on the Beryllium neutrino flux on earth, $\\Phi(Be)_{min} = 1\\cdot 10^9 cm^{-2} s^{-1}$, in the absence of oscillations, by using helioseismic data, the B-neutrino flux measured by Superkamiokande and the hydrogen abundance at the solar center predicted by Standard Solar Model (SSM) calculations. We emphasize that this abundance is the only result of SSMs needed for getting $\\Phi(Be)_{min}$. We also derive lower bounds for the Gallium signal, $G_{min}=(91 \\pm 3) $ SNU, and for the Chlorine signal, $C_{min}=(3.24\\pm 0.14)$ SNU, which are about $3\\sigma$ above their corresponding experimental values, $G_{exp}= (72\\pm 6)$ SNU and $C_{exp}= (2.56\\pm 0.22) $ SNU.

B. Ricci; F. L. Villante; M. Lissia

1999-04-06

297

Neutrinos in the Electron  

E-print Network

We will show that one half of the rest mass of the electron is equal to the sum of the rest masses of electron neutrinos and that the other half of the rest mass of the electron is given by the energy in the sum of electric oscillations. With this composition we can explain the rest mass, the electric charge, the spin and the magnetic moment of the electron.

E. L. Koschmieder

2005-03-28

298

Natural Neutrino Dark Energy  

SciTech Connect

1 construct a general description for neutrino dark energy models, that do not require exotic particles or strange couplings. With the help of the above, this class of models is reduced to a single function with several constraints. It is shown that these models lead to some concrete predictions that can be verified (or disproved) within the next decade, using results from PLANK, EUCLID and JDEM.

Gurwich, Ilya [Physics Department, Ben-Gurion University, Beer-Sheva 84105 (Israel)

2010-06-23

299

Birth of Neutrino Astrophysics  

ScienceCinema

Based mainly on the results of two experiments, KamiokaNDE and Super-KamiokaNDE, the birth of neutrino astrophysics will be described. At the end, the result of the third generation Kamioka experiment, KamLAND, will be discussed together with the future possibilities.Organiser(s): Daniel Treille / EP DivisionNote: * Tea & coffee will be served at 16:00 hrs. Please note unusual day.

None

2011-10-06

300

Birth of Neutrino Astrophysics  

SciTech Connect

Based mainly on the results of two experiments, KamiokaNDE and Super-KamiokaNDE, the birth of neutrino astrophysics will be described. At the end, the result of the third generation Kamioka experiment, KamLAND, will be discussed together with the future possibilities.Organiser(s): Daniel Treille / EP DivisionNote: * Tea & coffee will be served at 16:00 hrs. Please note unusual day.

None

2010-05-07

301

Sneutrino dark matter in gauged inverse seesaw models for neutrinos.  

PubMed

Extending the minimal supersymmetric standard model to explain small neutrino masses via the inverse seesaw mechanism can lead to a new light supersymmetric scalar partner which can play the role of inelastic dark matter (IDM). It is a linear combination of the superpartners of the neutral fermions in the theory (the light left-handed neutrino and two heavy standard model singlet neutrinos) which can be very light with mass in ~5-20 GeV range, as suggested by some current direct detection experiments. The IDM in this class of models has keV-scale mass splitting, which is intimately connected to the small Majorana masses of neutrinos. We predict the differential scattering rate and annual modulation of the IDM signal which can be testable at future germanium- and xenon-based detectors. PMID:22463522

An, Haipeng; Dev, P S Bhupal; Cai, Yi; Mohapatra, R N

2012-02-24

302

Renormalization of a two-loop neutrino mass model  

SciTech Connect

We analyze the renormalization group structure of a radiative neutrino mass model consisting of a singly charged and a doubly charged scalar fields. Small Majorana neutrino masses are generated by the exchange of these scalars via two-loop diagrams. We derive boundedness conditions for the Higgs potential and show how they can be satisfied to energies up to the Planck scale. Combining boundedness and perturbativity constraints with neutrino oscillation phenomenology, new limits on the masses and couplings of the charged scalars are derived. These in turn lead to lower limits on the branching ratios for certain lepton flavor violating (LFV) processes such as ??e?, ??3e and ? ? e conversion in nuclei. Improved LFV measurements could test the model, especially in the case of inverted neutrino mass hierarchy where these are more prominent.

Babu, K. S. [Department of Physics, Oklahoma State University, Stillwater, Oklahoma 74078 (United States); Julio, J. [Fisika LIPI, Kompleks Puspiptek Serpong, Tangerang 15310, Indonesia and Jožef Stefan Institute, Jamova Cesta 39, 1001 Ljubljana (Slovenia)

2014-06-24

303

Neutrino-less Double Beta Decay and Particle Physics  

E-print Network

We review the particle physics aspects of neutrino-less double beta decay. This process can be mediated by light massive Majorana neutrinos (standard interpretation) or by something else (non-standard interpretations). The physics potential of both interpretations is summarized and the consequences of future measurements or improved limits on the half-life of neutrino-less double beta decay are discussed. We try to cover all proposed alternative realizations of the decay, including light sterile neutrinos, supersymmetric or left-right symmetric theories, Majorons, and other exotic possibilities. Ways to distinguish the mechanisms from one another are discussed. Experimental and nuclear physics aspects are also briefly touched, alternative processes to double beta decay are discussed, and an extensive list of references is provided.

Werner Rodejohann

2011-10-17

304

Probing neutrino mass hierarchies and $?_{13}$ with supernova neutrinos  

E-print Network

We investigate the feasibility of probing the neutrino mass hierarchy and the mixing angle $\\phi_{13}$ with the neutrino burst from a future supernova. An inverse power-law density $\\rho \\sim r^{n} $ with varying $n$ is adopted in the analysis as the density profile of a typical core-collapse supernova. The survival probabilities of $\

Shao-Hsuan Chiu; T. K. Kuo

2006-02-27

305

ON SOLAR NEUTRINO PROBLEM TIAN MA AND SHOUHONG WANG  

E-print Network

ON SOLAR NEUTRINO PROBLEM TIAN MA AND SHOUHONG WANG Abstract. The current neutrino oscillation an alternative resolution to the solar neutrino loss problem. Contents 1. Introduction 1 2. Discrepancy of Solar, there are three flavors of neutrinos: the electron neutrino e, the tau neutrino and the mu neutrino µ. The solar

306

Evidence of Electron Neutrino Appearance in a Muon Neutrino Beam  

E-print Network

The T2K collaboration reports evidence for electron neutrino appearance at the atmospheric mass splitting, |\\Delta m_{32}^2|=2.4x10^{-3} eV^2. An excess of electron neutrino interactions over background is observed from a muon neutrino beam with a peak energy of 0.6 GeV at the Super-Kamiokande (SK) detector 295 km from the beam's origin. Signal and background predictions are constrained by data from near detectors located 280 m from the neutrino production target. We observe 11 electron neutrino candidate events at the SK detector when a background of 3.3\\pm0.4(syst.) events is expected. The background-only hypothesis is rejected with a p-value of 0.0009 (3.1\\sigma), and a fit assuming \

Abgrall, N; Akiri, T; Albert, J B; 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; Beznosko, D; Bhadra, S; Blaszczyk, F d M; Blondel, A; Bojechko, C; Boyd, S; Brailsford, D; Bravar, A; Bronner, C; Brook-Roberge, D G; Buchanan, N; Calland, R G; Rodriguez, J Caravaca; 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; Day, M; de Andre, J P A M; de Perio, P; De Rosa, G; Dealtry, T; Dennis, S; Densham, C; Di Lodovico, F; Di Luise, S; Dobson, J; Drapier, O; Duboyski, T; Dufour, F; Dumarchez, J; Dytman, S; Dziewiecki, M; Dziomba, M; Emery, S; Ereditato, A; Escudero, L; Finch, A J; Frank, E; Friend, M; Fujii, Y; Fukuda, Y; Furmanski, A; 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; Kaji, H; Kajita, T; Kakuno, H; Kameda, J; Kanazawa, Y; Karlen, D; Karpikov, I; Kearns, E; Khabibullin, M; Khanam, F; Khotjantsev, A; Kielczewska, D; Kikawa, T; Kilinski, A; Kim, J Y; Kim, J; Kim, S B; Kirby, B; Kisiel, J; Kitching, P; Kobayashi, T; Kogan, G; Kolaceke, A; Konaka, A; Kormos, L L; Korzenev, A; Koseki, K; Koshio, Y; Kowalik, K; Kreslo, I; Kropp, W; Kubo, H; Kudenko, Y; Kumaratunga, S; Kurjata, R; Kutter, T; Lagoda, J; Laihem, K; Laing, A; 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; Marchionni, A; Marino, A D; Marteau, J; Martin, J F; Maruyama, T; Marzec, J; Masliah, P; Mathie, E L; Matveev, V; Mavrokoridis, K; Mazzucato, E; McCauley, N; McFarland, K S; McGrew, C; McLachlan, T; Messina, M; Metelko, C; Mezzetto, M; 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; Nakajima, K; Nakamura, K; Nakayama, S; Nakaya, T; Nakayoshi, K; Naples, D; Nicholls, T C; Nielsen, C; Nirkko, M; Nishikawa, K; Nishimura, Y; O'Keeffe, H M; Obayashi, Y; 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; Guerra, E S Pinzon; 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; Reeves, M; Reinherz-Aronis, E; Retiere, F; Robert, A; Rodrigues, P A; Rondio, E; Roth, S; Rubbia, A; Ruterbories, D; Sacco, R; Sakashita, K; Sanchez, F; Scantamburlo, E; Scholberg, K; Schwehr, J; Scott, M; Scully, D I; Seiya, Y; Sekiguchi, T; Sekiya, H; Sgalaberna, D; Shibata, M; 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; Suzuki, A; Suzuki, K; Suzuki, S Y; Suzuki, Y; Szeglowski, T; Szeptycka, M; Tacik, R; Tada, M; Takahashi, S; Takeda, A; Takeuchi, Y; Tanaka, H A; Tanaka, M M; Tanaka, 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; Zambelli, L; Zaremba, K; Ziembicki, M; Zimmerman, E D; Zito, M; Zmuda, J

2013-01-01

307

Detecting non-relativistic cosmic neutrinos by capture on tritium: phenomenology and physics potential  

NASA Astrophysics Data System (ADS)

We study the physics potential of the detection of the Cosmic Neutrino Background via neutrino capture on tritium, taking the proposed PTOLEMY experiment as a case study. With the projected energy resolution of ? ~ 0.15 eV, the experiment will be sensitive to neutrino masses with degenerate spectrum, m1 simeq m2 simeq m3 = m? gtrsim 0.1 eV. These neutrinos are non-relativistic today; detecting them would be a unique opportunity to probe this unexplored kinematical regime. The signature of neutrino capture is a peak in the electron spectrum that is displaced by 2 m? above the beta decay endpoint. The signal would exceed the background from beta decay if the energy resolution is ? lesssim 0.7 m? . Interestingly, the total capture rate depends on the origin of the neutrino mass, being ?D simeq 4 and ?M simeq 8 events per year (for a 100 g tritium target) for unclustered Dirac and Majorana neutrinos, respectively. An enhancement of the rate of up to Script O(1) is expected due to gravitational clustering, with the unique potential to probe the local overdensity of neutrinos. Turning to more exotic neutrino physics, PTOLEMY could be sensitive to a lepton asymmetry, and reveal the eV-scale sterile neutrino that is favored by short baseline oscillation searches. The experiment would also be sensitive to a neutrino lifetime on the order of the age of the universe and break the degeneracy between neutrino mass and lifetime which affects existing bounds.

Long, Andrew J.; Lunardini, Cecilia; Sabancilar, Eray

2014-08-01

308

Neutrino mass spectrum and future beta decay experiments  

NASA Astrophysics Data System (ADS)

We study the discovery potential of future beta decay experiments on searches for the neutrino mass in the sub-eV range, and, in particular, KATRIN experiment with sensitivity m>0.3 eV. Effects of neutrino mass and mixing on the beta decay spectrum in the neutrino schemes which explain the solar and atmospheric neutrino data are discussed. The schemes which lead to observable effects contain one or two sets of quasi-degenerate states. Future beta decay measurements will allow to check the three-neutrino scheme with mass degeneracy, moreover, the possibility appears to measure the CP-violating Majorana phase. Effects in the four-neutrino schemes which can also explain the LSND data are strongly restricted by the results of Bugey and CHOOZ oscillation experiments: apart from bending of the spectrum and the shift of the end point one expects appearance of small kink of (<2%) size or suppressed tail after bending of the spectrum with rate below 2% of the expected rate for zero neutrino mass. We consider possible implications of future beta decay experiments for the neutrino mass spectrum, the determination of the absolute scale of neutrino mass and for establishing the nature of neutrinos. We show that beta decay measurements in combination with data from the oscillation and double beta decay experiments will allow to establish the structure of the scheme (hierarchical or non-hierarchical), the type of the hierarchy or ordering of states (normal or inverted) and to measure the relative CP-violating phase in the solar pair of states.

Farzan, Y.; Peres, O. L. G.; Smirnov, A. Yu.

2001-09-01

309

On the Neutrino Mass Spectrum and Neutrinoless Double-Beta Decay  

E-print Network

Assuming 3-neutrino mixing, neutrino oscillation explanation of the solar and atmospheric neutrino data, massive Majorana neutrinos and neutrinoless double beta-decay generated only by the (V-A) charged current weak interaction via the exchange of the three Majorana neutrinos, we analyze in detail the possibility of determining the type of the neutrino mass spectrum by measuring of the effective Majorana mass || in neutrinoless double-beta decay. The three possible types of neutrino mass spectrum are considered: i) with normal hierarchy (NH) m1 | due to the imprecise knowledge of the relevant nuclear matrix elements. We derive the ranges of values of the mixing angle which controls the solar neutrino oscillations for which the measurement of || would allow one to discriminate between the NH and IH, NH and QD and IH and QD spectra. The requirements which the possibility of distinguishing between the three types of spectra imposes on the uncertainty in the values of the neutrinoless double beta-decay nuclear ma...

Pascoli, S; Rodejohann, W

2003-01-01

310

Is There a Massive Neutrino?  

ERIC Educational Resources Information Center

Discussed is the question of whether "heavy" neutrinos really do exist based on the evidence supplied by four research groups. The implications of its existence on the disciplines of particle physics, astrophsyics, and cosmology are discussed. Background information on the different types of neutrinos is provided. (KR)

Selvin, Paul

1991-01-01

311

The Mass of the Neutrinos  

E-print Network

In the theory of the Dirac equation and in the standard model, the neutrino is massless. Both these theories use Lorentz invariance. In modern approaches however, spacetime is no longer smooth, and this modifies special relativity. We show how such a modification throws up the mass of the neutrino.

Burra G. Sidharth

2009-04-23

312

Neutrino astronomy and lepton charge  

Microsoft Academic Search

It is shown that lepton nonconservation might lead to a decrease in the number of detectable solar neutrinos at the earth surface, because of nue<--numu oscillations, similar to Ko<--K~o oscillations. Equations are presented describing such oscillations for the case when there exist only four neutrino states.

V. Gribov; B. Pontecorvo

1969-01-01

313

Observation of Geo-Neutrinos  

E-print Network

Geo-neutrinos, electron anti-neutrinos produced in beta decays of naturally occurring radioactive isotopes in the Earth, are a unique direct probe of our planet's interior. We report the first observation at more than 3$\\sigma$ C.L. of geo-neutrinos, performed with the Borexino detector at Laboratori Nazionali del Gran Sasso. Anti-neutrinos are detected through the neutron inverse beta decay reaction. With a 252.6 ton-yr fiducial exposure after all selection cuts, we detected 9.9^{+4.1}_{-3.4}(^{+14.6}_{-8.2}) geo-neutrino events, with errors corresponding to a 68.3%(99.73%) C.L. From the $\\ln{\\cal{L}}$ profile, the statistical significance of the Borexino geo-neutrino observation corresponds to a 99.997% C.L. Our measurement of the geo-neutrinos rate is 3.9^{+1.6}_{-1.3}(^{+5.8}_{-3.2}) events/(100ton-yr). This measurement rejects the hypothesis of an active geo-reactor in the Earth's core with a power above 3 TW at 95% C.L. The observed prompt positron spectrum above 2.6 MeV is compatible with that expected from european nuclear reactors (mean base line of approximately 1000 km). Our measurement of reactor anti-neutrinos excludes the non-oscillation hypothesis at 99.60% C.L.

Borexino Collaboration

2010-03-01

314

Beta Beams for Neutrino Production  

Microsoft Academic Search

This paper gives an overview of the work done so far to produce sufficient neutrino fluxes for neutrino oscillation physics using beta beams. The design study on a beta beam scenario, the EURISOL (European Isotope Separation On-Line Radioactive Ion Beam Facility) Design Study, a project funded by the European Commission (EC), is now ready to be published. The study is

Elena Wildner; Elena

2010-01-01

315

Neutrino exploration of the earth  

NASA Astrophysics Data System (ADS)

We show how the neutrinos produced by a multi-TeV proton synchotron may be used for purposes of geological research. Project GENIUS (geological exploration by neutrino-induced underground sound) is designed to search for deposits of oil and gas at large distances from the accelerator. It depends upon the coherent sound signal produced at depth by millions of neutrino interactions along the underground neutrino beam. Surface measurements of the acoustic pulse provide a remote underground probe. Project GEMINI (geological exploration with muons induced by neutrino interactions) is designed to search for distant deposits of high- Z ores. It depends upon the surface measurement of neutrino-induced muons which were produced in the last few kilometers of the neutrinos' underground voyage. Project GEOSCAN is a flux-independent procedure to determine the vertical density profile of the Earth, and especially its core. It depends upon the angle and energy dependence of the attenuation as the neutrino beam traverses the whole Earth.

De Rújula, A.; Glashow, S. L.; Wilson, R. R.; Charpak, G.

1983-10-01

316

High energy neutrinos from quasars  

Microsoft Academic Search

We review and clarify the assumptions of our basic model for neutrino production in the cores of quasars, as well as those modifications to the model made subsequently by other workers. We also present a revised estimate of the neutrino background flux and spectrum obtained using more recent empirical studies of quasars and their evolution. We compare our results with

F. W. Stecker; M. H. Salamon

1996-01-01

317

India-based Neutrino Observatory  

NASA Astrophysics Data System (ADS)

An introduction to India-based Neutrino Observatory and a brief status report are presented.The two possible sites are described along with their special advantages.The proposed detector and its physics capabilities for atmospheric neutrinos and long-base-line experiments are discussed.

Rajasekaran, G.

2004-10-01

318

Enhanced sensitivities for the searches of neutrino magnetic moments through atomic ionization.  

PubMed

A new detection channel on atomic ionization for possible neutrino electromagnetic interactions is identified and studied. Significant sensitivity enhancement is demonstrated when the energy transfer to the target is of the atomic-transition scale. The interaction cross section induced by neutrino magnetic moments (?(?)) is evaluated with the equivalent photon method. A new limit of ?(?)(?[over ¯](e))<1.3×10(-11) ?(B) at 90% confidence level is derived by using current reactor neutrino data. Potential reaches for future experiments are explored. Experiments with sub-keV sensitivities can probe ?(?) to 10(-13) ?(B). Positive observations of ?(?) in this range would imply that neutrinos are Majorana particles. PMID:20867973

Wong, Henry T; Li, Hau-Bin; Lin, Shin-Ted

2010-08-01

319

Big World of Small Neutrinos Hitoshi Murayama  

E-print Network

Big World of Small Neutrinos Hitoshi Murayama UC Berkeley / LBNL Harvard, Dec 9, 2002 #12;Harvard colloquium 2 Neutrinos are Everywhere #12;Harvard colloquium 3 "Wimpy and Abundant" Neutrinos are Everywhere · They come from the Big Bang: ­ When the Universe was hot, neutrinos were created equally with any other

Murayama, Hitoshi

320

Theory of neutrinos: a white paper  

Microsoft Academic Search

This paper is a review of the present status of neutrino mass physics, which grew out of an APS sponsored study of neutrinos in 2004. After a discussion of the present knowledge of neutrino masses and mixing and some popular ways to probe the new physics implied by recent data, it summarizes what can be learned about neutrino interactions as

R. N. Mohapatra; S. Antusch; K. S. Babu; G. Barenboim; M.-C. Chen; A. de Gouvêa; P. de Holanda; B. Dutta; Y. Grossman; A. Joshipura; B. Kayser; J. Kersten; Y. Y. Keum; S. F. King; P. Langacker; M. Lindner; W. Loinaz; I. Masina; I. Mocioiu; S. Mohanty; H. Murayama; S. Pascoli; S. T. Petcov; A. Pilaftsis; P. Ramond; M. Ratz; W. Rodejohann; R. Shrock; T. Takeuchi; T. Underwood; L. Wolfenstein

2007-01-01

321

Thermodynamic Laws of Neutrino and Photon Emission.  

ERIC Educational Resources Information Center

Compares neutrino and photon emissions, develops the thermodynamic blackbody laws of neutrino emission analogous to laws governing photon emission, points out that combined radiation from a "true blackbody" consists of both photon and neutrino emissions of comparable magnitude, and speculates upon the existence of blackbody neutrino emitters in…

Walsh, P. J.; Gallo, C. F.

1980-01-01

322

Ultra- and extremely high energy neutrino astronomy  

E-print Network

Scientific motivations for ultra- and extremely high energy neutrino astronomy are considered. Sources and expected fluxes of EHE/UHE neutrinos are briefly discussed. Operating and planned experiments on astrophysical neutrino detection are reviewed focusing on deep underwater/ice Cherenkov neutrino telescopes.

I. Sokalski

2005-01-05

323

Search for excited neutrinos in Z decay  

Microsoft Academic Search

Excited neutrinos decaying into a neutrino and a photon are searched for in the ALEPH detector at LEP. No evidence is found for Z decay into v¯v* or v¯*v* final states. Upper limits are derived on excited neutrino couplings up to excited neutrino masses close to the Z mass. Lower limits on the v* mass, independent of the v* decay

D. Decamp; B. Deschizeaux; C. Goy; J.-P. Lees; M.-N. Minard; R. Alemany; J. M. Crespo; M C Delfino; E. Fernandez; V. Gaitan; Ll. Garrido; P. Mato; R. Miguel; Ll. M. Mir; S. Orteu; A. Pacheco; J. A. Perlas; E. Tubau; M. G. Catanesi; D. Creanza; M. de Palma; A. Farilla; G. Iaselli; G. Maggi; M. Maggi; S. Natali; S. Nuzzo; M. Quattromini; A. Ranieri; G. Raso; F Ruggieri; G. Selvaggi; L. Silvestris; P. Tempesta; G. Zito; Y. S. Gao; H. Hu; D. Huang; S. Jin; J. Lin; T. Ruan; T. Wang; W. Wu; Y. Xie; D. Xu; R. Xu; J. Zhang; W. Zhao; W. B. Atwood; F. Bird; E. Blucher; G. Bonvicini; F. Bossi; J. Bourotte; D. Brown; T. H. Burnett; H. Drevermann; Friedrich Dydak; R. W. Forty; C. Grab; R. Hagelberg; S. Haywood; B. Jost; M. Kasemann; G. Kellner; J. Knobloch; A. Lacourt; I. Lehraus; T. Lohse; A. Marchioro; M. Martinez; S. Menary; A. Minten; A. Miotto; J. Nash; P. Palazzi; F. Ranjard; G. Redlinger; A. Roth; J. Rothberg; H. Rotscheidt; W. von Rüden; R. St. Denis; D. Schlatter; M. Takashima; M. Talby; H. Taureg; W. Tejessy; H. Wachsmuth; S. Wasserbaech; S. Wheeler; W. Wiedenmann; W. Witzeling; J. Wotschack; Z. Ajaltouni; M. Bardadin-Otwinowska; A. Falvard; R. El Fellous; P. Gay; P. Henrard; J. Jousset; B. Michel; J.-C. Montret; D. Pallin; P. Perret; J. Proriol; F. Prulhière; J. D. Hansen; J. R. Hansen; P. H. Hansen; R. Møllerud; B. S. Nilsson; G. Petersen; I. Efthymiopoulos; E. Simopoulou; A. Vayaki; J. Badier; A. Blondel; G. Bonneaud; F. Braems; J. C. Brient; G. Fouque; A. Gamess; R. Guirlet; A. Rosowsky; A. Rougé; M. Rumpf; R. Tanaka; H. Videau; I. Videau; D. J. Candlin; G. Parrini; M. Corden; C. Georgiopoulos; M. Ikeda; J. Lannutti; D. Levinthal; M. Mermikides; L. Sawyer; G. Stimpfl; A. Antonelli; R. Baldini; G. Bencivenni; G. Bologna; P. Campana; G. Capon; V. Chiarella; B. D'Ettorre-Piazzoli; G. Felici; P. Laurelli; G. Mannocchi; F. Massimo-Brancacci; F. Murtas; G. P. Murtas; G. Nicoletti; M. Pepe-Altarelli; P. Picchi; P. Zografou; B. Altoon; O. Boyle; A. W. Halley; I. Ten Have; J. L. Hearns; J. G. Lynch; W. T. Morton; C. Raine; J. M. Scarr; K. Smith; A. S. Thompson; B. Brandl; O. Braun; R. Geiges; C. Geweniger; P. Hanke; V. Hepp; E. E. Kluge; Y. Maumary; A. Putzer; B. Rensch; A. Stahl; K. Tittel; M. Wunsch; A. T. Belk; R. Beuselinck; D. M. Binnie; W. Cameron; M. Cattaneo; P. J. Dornan; S. Dugeay; A. M. Greene; J. F. Hassard; S. J. Patton; J. K. Sedgbeer; G. Taylor; I. R. Tomalin; A. G. Wright; P. Girtler; D. Kuhn; G. Rudolph; C. K. Bowdery; T. J. Brodbeck; A. J. Finch; F. Foster; G. Hughes; N. R. Keemer; M. Nuttall; B. S. Rowlingson; T. Sloan; S. W. Snow; T. Barczewski; L. A. T. Bauerdick; K. Kleinknecht; B. Renk; S. Roehn; H.-G. Sander; M. Schmelling; F. Steeg; J.-P. Albanese; J.-J. Aubert; C. Benchouk; V. Bernard; A. Bonissent; D. Courvoisier; F. Etienne; S. Papalexiou; P. Payre; B. Pietrzyk; Z. Qian; W. Blum; P. Cattaneo; G. Cowan; B. Dehning; H. Dietl; M. Fernandez-Bosman; A. Jahn; E. Lange; G. Lütjens; G. Lutz; W. Männer; H.-G. Moser; Y. Pan; R. Richter; A. S. Schwarz; R. Settles; U. Stiegler; U. Stierlin; J. Thomas; V. Bertin; G. de Bouard; J. Boucrot; O. Callot; X. Chen; A. Cordier; M. Davier; G. Ganis; J.-F. Grivaz; Ph. Heusse; P. Janot; V. Journé; D. W. Kim; J. Lefrançois; A.-M. Lutz; J.-J. Veillet; Z. Zhang; F. Zomer; S. R. Amendolia; G. Bagliesi; G. Batignani; L. Bosisio; U. Bottigli; C. Bradaschia; M. A. Ciocci; I. Ferrante; F. Fidecaro; L. Foà; E. Focardi; F. Forti; A. Giassi; M. A. Giorgi; F. Ligabue; A. Lusiani; E. B. Mannelli; P. S. Marrocchesi; A. Messineo; F. Palla; G. Sanguinetti; J. Steinberger; R. Tenchini; G Triggiani; J. M. Carter; M. G. Green; P. V. March; T. Medcalf; M. R. Saich; J. A. Strong; R. M. Thomas; T. Wildish; D. R. Botterill; R. W. Clifft; T. R. Edgecock; M. Edwards; S. M. Fisher; J. Harvey; T. J. Jones; P. R. Norton; D. P. Salmon; J. C. Thompson; B. Bloch-Devaux; P. Colas; C. Klopfenstein; E. Lançon; E. Locci; S. Loucatos; L. Mirabito; E. Monnier; P. Perez; F. Perrier; J. Rander; J.-F. Renardy; A. Roussarie; J.-P. Schuller; J. G. Ashman; C. N. Booth; F. Combley; M. Dinsdale; J. Martin; D. Parker; L. F. Thompson; S. Brandt; H. Burkhardt; C. Grupen; H. Meinhard; E. Neugebauer; U. Schäfer; H. Seywerd; G. Apollinari; G. Giannini; B. Gobbo; F. Liello; E. Milotti; L. Rolandi; L. Bellantoni; J. F. Boudreau; D. Cinabro; J. S. Conway; D. F. Cowen; A. J. Deweerd; Z. Feng; D. P. S. Ferguson; J. L. Harton; J. Hilgart; J. E. Jacobsen; R. C. Jared; R. P. Johnson; B. W. Leclaire; T. Parker; J. R. Pater; Y. Saadi; V. Sharma; J. A. Wear; F. V. Weber; Sau Lan Wu; G. Zobernig

1990-01-01

324

An Anatomy of Neutrino Oscillations  

E-print Network

To understand neutrino oscillations with neutrinos treated as point-like Dirac particles, we describe how to use an off-diagonal (cross-generation) neutrino-Higgs (mass) interaction to simulate oscillations in a natural way. This results in an extra orthogonal $SU_f(3)$ family gauge theory, which cooperates with the Minimal Standard Model to form a unique extended Standard Model (i.e., our Standard Mode). Altogether, it helps us to resolve a few outstanding puzzles - the question of why there are only three generations, the question of why the masses of neutrinos are so tiny, the question of why neutrinos oscillate, and the question of why the dark-matter world is so huge (25%) as compared to the visible ordinary-matter world (5%).

W-Y. Pauchy Hwang

2014-11-03

325

Geo-neutrinos: recent developments  

E-print Network

Radiogenic heating is a key component of the energy balance and thermal evolution of the Earth. It contributes to mantle convection, plate tectonics, volcanoes, and mountain building. Geo-neutrino observations estimate the present radiogenic power of our planet. This estimate depends on the quantity and distribution of heat-producing elements in various Earth reservoirs. Of particular geological importance is radiogenic heating in the mantle. This quantity informs the origin and thermal evolution of our planet. Here we present: currently reported geo-neutrino observations; estimates of the mantle geo-neutrino signal, mantle radiogenic heating, and mantle cooling; a comparison of chemical Earth model predictions of the mantle geo-neutrino signal and mantle radiogenic heating; a brief discussion of radiogenic heating in the core, including calculations of geo-neutrino signals per pW/kg; and finally a discussion of observational strategy.

Dye, Steve

2014-01-01

326

Neutrinos Get Under Your Skin  

SciTech Connect

The enigmatic neutrinos are among the most abundant of the tiny particles that make up our universe. They are a billion times more abundant than the particles of which the earth and we humans are made. Thus, to understand the universe, we must understand the neutrinos. Moving ghostlike, almost invisibly, through matter, these particles are very hard to pin down and study. However, dramatic progress has recently been made. In this lecture, the neutrinos will be introduced. Their behavior, so different from that of everyday objects, will be explained, and recent discoveries will be described. The open questions about neutrinos, forthcoming attempts to answer these questions, and the role of neutrinos in shaping the universe and making human life possible, will all be explained.

Kayser, Boris

2005-08-30

327

Supernova observations for neutrino mixing parameters  

SciTech Connect

The neutrino spectra from a future galactic core collapse supernova could reveal information on the neutrino mixing pattern, especially on {theta}{sub 13} and the mass hierarchy. I briefly outline our current understanding of neutrino flavor conversions inside a supernova, and point out possible signatures of various neutrino mixing scenarios that the neutrino detectors should look for. Supernova neutrinos provide a probe for {theta}{sub 13} and mass hierarchy that is complementary to, and sometimes even better than, the current and proposed terrestrial neutrino oscillation experiments.

Dighe, Amol [Department of Theoretical Physics, Tata Institute of Fundamental Research, 1, Homi Bhabha Road, Colaba, Mumbai 400005 (India)

2011-10-06

328

Low-Scale See-Saw Mechanisms for Light Neutrinos  

E-print Network

Alternatives to the see-saw mechanism are explored in supersymmetric models with three right-handed or sterile neutrinos. Tree-level Yukawa couplings can be drastically suppressed in a natural way to give sub-eV Dirac neutrino masses. If, in addition, a B-L gauge symmetry broken at a large scale M_G is introduced, a wider range of possibilities opens up. The value of the right-handed neutrino mass M_R can be easily disentangled from that of M_G. Dirac and Majorana neutrino masses at the eV scale can be generated radiatively through the exchange of sneutrinos and neutralinos. Dirac masses m_D owe their smallness to the pattern of light-heavy scales in the neutralino mass matrix. The smallness of the Majorana masses m_L is linked to a similar see-saw pattern in the sneutrino mass matrix. Two distinct scenarios emerge. In the first, with very small or vanishing M_R, the physical neutrino eigenstates are, for each generation, either two light Majorana states with mixing angle ranging from very small to maximal, depending on the ratio m_D/M_R, or one light Dirac state. In the second scenario, with a large value of M_R, the physical eigenstates are two nearly unmixed Majorana states with masses \\sim m_L and \\sim M_R. In both cases, the (B-L)-breaking scale M_G is, in general, much smaller than that in the traditional see-saw mechanism.

Francesca Borzumati; Yasunori Nomura

2000-07-03

329

Detecting the neutrino magnetic moment at hadron colliders  

NASA Astrophysics Data System (ADS)

We consider the model based on the S U (2 )R×S U (2 )L×U (1 )B -L gauge group with Majorana neutrinos. In this model the transit dipole magnetic moment (?? N)if which is associated with the Ni??f? transition may be as large as a few×1 0-8?B . The possible manifestations of the (?? N)if at hadron colliders are investigated. In doing so, we assume that one of the three heavy right-handed neutrinos Ne R is on the electroweak scale. The process of Ne R production p +p ?WR-?e-Ne R, with the subsequent Ne R decay through the channel Ne R??e L+? , is investigated. Problems caused by selecting the signal from background is examined. It is shown that the process in question is the most perspective one for detecting the (?? N)if, provided the condition mWR<6 TeV is realized. The cross section of N? R production under the collision of a high-energy light neutrino beam with the proton target ?? L+p ?? ?N? R+p +X is investigated. The produced N? R neutrino is identified through the decay channel N? R??±+2 j . Detection of both the positive and negative charged muons will point to the Majorana nature of the neutrino. On the other hand, detection of the right-handed polarized muons will be unambiguously indicative of a nonzero value of (?? N)if.

Boyarkin, O. M.; Boyarkina, G. G.

2014-11-01

330

Double neutrino production and detection in neutrino detectors  

NASA Astrophysics Data System (ADS)

Large, high-energy (E>100GeV) cosmic neutrino telescopes are now quite mature. IceCube, for example, observes about 50 000 well-reconstructed single atmospheric neutrino events/year, with energies above 100 GeV. Although the neutrino detection probability is small, current detectors are large enough so that it is possible to detect two neutrinos from the same cosmic-ray interaction. In this paper, we calculate the expected rate of double-neutrino interactions from a single cosmic-ray air shower. The rate is small, about 0.07events/year for a 1km3 detector like IceCube, with only a small dependence on the assumed cosmic-ray composition and hadronic interaction model. For a larger detector, like the proposed KM3Net, the rate is about 0.8events/year, high enough to be easily observable. These double neutrino interactions are the major irreducible background to searches for pairs of supersymmetric particles produced in neutrino or cosmic-ray air-shower interactions. Other standard model backgrounds are considered, and found to be small.

van der Drift, Don; Klein, Spencer R.

2013-08-01

331

Energy Dependence of Solar Neutrino Suppression and Bounds on the Neutrino Magnetic Moment  

E-print Network

An analysis of neutrino electron scattering as applied to the SuperKamiokande solar neutrino experiment with the data from the Homestake experiment leads to an upper bound on the neutrino magnetic moment in the range $\\mu_{\

Joao Pulido; Ana M. Mourao

1998-03-02

332

An angle to tackle the neutrinos  

E-print Network

A brief history of the discovery of neutrino oscillations and neutrino mass is presented highlighting the recent breakthrough in the determination of a crucial neutrino parameter by the Daya Bay and RENO reactor experiments. The importance of this parameter in the context of one of the goals of the India-based Neutrino Observatory (INO) project and also in advancing the frontier of neutrino physics is explained.

G. Rajasekaran

2012-06-01

333

What we can learn from atmospheric neutrinos  

E-print Network

Physics potential of future measurements of atmospheric neutrinos is explored. Observation of $\\Delta m^2_{21}$ driven sub-dominant effects and $\\theta_{13}$ driven large matter effects in atmospheric neutrinos can be used to study the deviation of $\\theta_{23}$ from maximality and its octant. Neutrino mass hierarchy can be determined extremely well due to the large matter effects. New physics can be constrained both in standard atmospheric neutrino experiments as well as in future neutrino telescopes.

Sandhya Choubey

2006-09-19

334

Theory Predictions for Inclusive atmospheric Neutrino flux  

NASA Astrophysics Data System (ADS)

We describe the history of theory prediction of inclusive atmospheric neutrino flux shortly, then the 3-dimensional calculation of atmospheric neutrino flux in some detail. With the calculated atmospheric neutrino flux for INO and South Pole, we discuss on the relation of atmospheric neutrino flux and geomagnetic field. We find the full 3-dimensional scheme calculation is necessary for the theory prediction of the atmospheric neutrino flux.

Honda, Morihiro

2013-06-01

335

Neutrino-induced muons observed with MINOS  

SciTech Connect

The Main Injector Neutrino Oscillation Search (MINOS) experiment's Far Detector has been operational since July 2003, taking cosmic ray and atmospheric neutrino data from its location in the Soudan Mine Underground Lab. Numerous neutrino-induced muons have been observed. The detector's magnetic field allows the first determination by a large underground detector of muon charge and thus neutrino versus anti-neutrino on an event by event basis.

Habig, A.; /Minnesota U., Duluth

2005-07-01

336

Neutrino properties deduced from the study of lepton number violating processes at low and high energies  

SciTech Connect

There is nowadays a significant progress in understanding the neutrino properties. The results of the neutrino oscillation experiments have convincingly showed that neutrinos have mass and oscillate, in contradiction with the Standard Model (SM) assumptions, and these are the first evidences of beyond SM physics. However, fundamental properties of the neutrinos like their absolute mass, their character (are they Dirac or Majorana particles?), their mass hierarchy, the number of neutrino flavors, etc., still remain unknown. In this context there is an increased interest in the study of the lepton number violating (LNV) processes, since they could complete our understanding on the neutrino properties. Since recently, the neutrinoless double beta decay was considered the only process able to distinguish between Dirac or Majorana neutrinos and to give a hint on the absolute mass of the electron neutrino. At present, the increased luminosity of the LHC experiments makes feasible the search of LNV processes at high energy as well. In this lecture I will make a brief review on our present knowledge of the neutrino properties, on the present status of the double-beta decay studies and on the first attempts to search LNV processes at LHC.

Stoica, Sabin [Horia Hulubei Foundation, P.O. Box MG-12, 077125 Magurele-Bucharest (Romania) and Horia Hulubei National Institute for Physics and Nuclear Engineering, P.O. Box MG-6, Magurele-Bucharest 077125 (Romania)

2012-11-20

337

Superluminal Neutrinos without Revolution  

E-print Network

The velocity anomaly recently reported by the OPERA collaboration appears strikingly at odds with the theory of special relativity. I offer a reinterpretation which removes this conflict, to wit that neutrinos yield a truer measurement of Einstein's limiting speed, and that light and indeed all other matter are retarded by additional interactions with the dark universe. I discuss existing experimental constraints and show that such a notion, considered cosmologically, can be subsumed in the dark-energy equation of state in an expanding Friedman-Robertson-Walker (FRW) universe. Planned measurements of the temporal variation in redshift have the potential to distinguish the possibilities.

Susan Gardner

2011-12-06

338

Geometry-free neutrino masses in curved spacetime  

E-print Network

The seesaw-induced neutrino mass is discussed in a generic class of curved spacetime, including the flat and warped extra dimensions. For Majorana masses in the bulk and on the boundary, the exact forms of seesaw-induced masses are derived by using the Kaluza-Klein mode expansion and the lepton number violating correlator for bulk fermion. It is found that the neutrino mass is determined without the knowledge of wave functions and whole background geometry when the metric factor is fixed on the boundary, e.g. by solving the hierarchy problem.

Atsushi Watanabe; Koichi Yoshioka

2009-10-05

339

Neutrino See-Saw Triviality And Lepton Flavour Violation  

E-print Network

For the D=5 Majorana neutrino mass operator to have a see-saw ultraviolet completion that is viable up to the Planck scale, the see-saw scale is bounded above due to triviality limits on the see-saw couplings. For supersymmetric see-saw models, with realistic neutrino mass textures, we compare constraints on the see-saw scale from triviality bounds, with those arising from experimental limits on induced charged-lepton flavour violation, for both the CMSSM and for models with split supersymmetry.

Bruce A. Campbell; David W. Maybury

2006-05-12

340

Neutrino mass, mixing and discrete symmetries  

NASA Astrophysics Data System (ADS)

Status of the discrete symmetry approach to explanation of the lepton masses and mixing is summarized in view of recent experimental results, in particular, establishing relatively large 1-3 mixing. The lepton mixing can originate from breaking of discrete flavor symmetry Gf to different residual symmetries Gl and Gv in the charged lepton and neutrino sectors. In this framework the symmetry group condition has been derived which allows to get relations between the lepton mixing elements immediately without explicit model building. The condition has been applied to different residual neutrino symmetries Gv. For generic (mass independent) Gv = Z2 the condition leads to two relations between the mixing parameters and fixes one column of the mixing matrix. In the case of Gv = Z2 × Z2 the condition fixes the mixing matrix completely. The non-generic (mass spectrum dependent) Gv lead to relations which include mixing angles, neutrino masses and Majorana phases. The symmetries Gl, Gv, Gf are identified which lead to the experimentally observed values of the mixing angles and allow to predict the CP phase.

Smirnov, Alexei Y.

2013-07-01

341

MUON STORAGE RINGS - NEUTRINO FACTORIES  

SciTech Connect

The concept of a muon storage ring based Neutrino Source (Neutrino Factory) has sparked considerable interest in the High Energy Physics community. Besides providing a first phase of a muon collider facility, it would generate more intense and well collimated neutrino beams than currently available. The BNL-AGS or some other proton driver would provide an intense proton beam that hits a target, produces pions that decay into muons. The muons must be cooled, accelerated and injected into a storage ring with a long straight section where they decay. The decays occurring in the straight sections of the ring would generate neutrino beams that could be directed to detectors located thousands of kilometers away, allowing studies of neutrino oscillations with precisions not currently accessible. For example, with the neutrino source at BNL, detectors at Soudan, Minnesota (1,715 km), and Gran Sasso, Italy (6,527 km) become very interesting possibilities. The feasibility of constructing and operating such a muon-storage-ring based Neutrino-Factory, including geotechnical questions related to building non-planar storage rings (e.g. at 8{degree} angle for BNL-Soudan, and 3{degree} angle for BNL-Gran Sasso) along with the design of the muon capture, cooling, acceleration, and storage ring for such a facility is being explored by the growing Neutrino Factory and Muon Collider Collaboration (NFMCC). The authors present overview of Neutrino Factory concept based on a muon storage ring, its components, physics opportunities, possible upgrade to a full muon collider, latest simulations of front-end, and a new bowtie-muon storage ring design.

PARSA,Z.

2000-05-30

342

Status of solar neutrino experiments  

SciTech Connect

A summary of the status of four solar neutrino experiments is presented. The Homestake {sup 37}Cl data are presented and the possible time dependence of the data is addressed. Data from 1040 days of operation of the Kamiokande II detector are presented next. The status of the {sup 71}Ga experiment in the Baksan Neutrino Observatory, which has operated for a short time, is discussed. The summary concludes with a discussion of the status of the Sudbury Neutrino Observatory, which has been under construction since the beginning of 1990. 7 refs., 6 figs.

Beier, E.W.; Davis, R. Jr.; Kim, S.B. (Pennsylvania Univ., Philadelphia, PA (USA). Dept. of Physics); Elliott, S.R. (Los Alamos National Lab., NM (USA)); Jelley, N. (Oxford Univ. (UK))

1990-01-01

343

Neutrino Leakage and Supernova Explosion  

NASA Astrophysics Data System (ADS)

In the process of supernova explosion, the neutrino leakage is very important. With different neutrino leakage schemes, the type II supernova explosions are simulated respectively for the stars with the mass of 12 M_{?}, 14 M_{?}, and 15 M_{?} by using a one-dimensional spherically symmetric model. The results show that the different neutrino leakage schemes have influence on the supernova collapse, shock wave propagation, and explosion. And the best values of corrective parameters which are propitious to the type II supernova explosions are given. In addition, the impacts of the equation of state and the compression modulus on the simulating results are discussed.

Liao, D. B.; Zhang, M. J.; Li, Y.; Pan, J. H.; Chen, X.

2014-09-01

344

An Anatomy of Neutrino Oscillations  

E-print Network

To understand neutrino oscillations in the sense of quantum mechanics or quantum field theory, we describe how to use an off-diagonal (cross-generation) neutrino-Higgs(mass) interaction to simulate oscillations in a natural way. This results in an extra orthogonal SU_f (3) family gauge theory, which may help us to resolve a few outstanding puzzles - the question of why there are only three generations, the question of why the masses of neutrinos are so tiny, and the question of why the dark-matter world is so huge (25%) as compared to the visible ordinary-matter world (5%).

Hwang, W-Y Pauchy

2012-01-01

345

Where do the Neutrinos go?  

NASA Astrophysics Data System (ADS)

Everybody knows that nuclear physics is the study the kind of matter found inside the atomic nucleus whether they it is at the center of atoms or the core of neutron stars. Nevertheless, nuclear physicists have made important discoveries about the neutrino. Figuring out where the neutrinos go in nuclear physics has challenged nuclear scientists, policy makers and those responsible for funding the enterprise. I will consider these and other challenges and how insightful scientific management has contributed the feast of wonderful discoveries about the neutrino.

Freedman, Stuart

2011-10-01

346

Neutrino interactions in neutron matter  

NASA Astrophysics Data System (ADS)

Neutrino flow is the dominant mechanism of energy transfer in the latest stages of supernovae explosions and in compact stars. The Standard Model of particle physics and accelerator data, provide a satisfactory description of neutrino physics in vacuum up to TeV scale. Nevertheless modeling the dynamics of neutrino interaction in the nuclear environment involves severe difficulties. This thesis in mainly aimed at obtaining the weak response of infinite matter, using both the Correlated Basis Function theory and Landau Theory of Fermi liquid to take into account properly nucleon-nucleon hard core potential and long range correlation (quasi-particle, collective modes, ecc.)

Cipollone, Andrea

2012-12-01

347

MOON for a next-generation neutrino-less double-beta decay experiment: Present status and perspective  

SciTech Connect

The performance of the MOON detector for a next-generation neutrino-less double-beta decay experiment was evaluated by means of the Monte Carlo method. The MOON detector was found to be a feasible solution for the future experiment to search for the Majorana neutrino mass in the range of 100-30 meV.

Shima, T.; /Osaka U., Res. Ctr. Nucl. Phys.; Doe, P.J.; /Washington U., Seattle; Ejiri, H.; /Osaka U., Res. Ctr. Nucl. Phys. /NIRS, Chiba /Prague, Tech. U.; Elliot, S.R.; /Washington U., Seattle /Los Alamos; Engel, J.; /North Carolina U.; Finger, M.; /Charles U.; Finger, M.; /Charles U.; Fushimi, K.; /Tokushima U.; Gehman, V.M.; /Washington U., Seattle /Los Alamos; Greenfield, M.B.; /Tokyo, Intl. Christian U.; Hazama, R.; /Hiroshima U. /NIRS, Chiba

2008-01-01

348

Supernova neutrino nucleosynthesis of light elements with neutrino oscillations.  

PubMed

Light element synthesis in supernovae through neutrino-nucleus interactions, i.e., the v process, is affected by neutrino oscillations in the supernova environment. There is a resonance of 13-mixing in the O/C layer, which increases the rates of charged-current -process reactions in the outer He-rich layer. The yields of 7Li and 11B increase by about a factor of 1.9 and 1.3, respectively, for a normal mass hierarchy and an adiabatic 13-mixing resonance, compared to those without neutrino oscillations. In the case of an inverted mass hierarchy and a nonadiabatic 13-mixing resonance, the increase in the 7Li and 11B yields is much smaller. Observations of the 7Li/11B ratio in stars showing signs of supernova enrichment could thus provide a unique test of neutrino oscillations and constrain their parameters and the mass hierarchy. PMID:16606251

Yoshida, Takashi; Kajino, Toshitaka; Yokomakura, Hidekazu; Kimura, Keiichi; Takamura, Akira; Hartmann, Dieter H

2006-03-10

349

Neutrino masses, leptogenesis, and sterile neutrino dark matter  

NASA Astrophysics Data System (ADS)

We analyze a scenario in which the lightest heavy neutrino N1 is a dark matter candidate and the second-heaviest neutrino N2 decays producing a lepton number. If N1 were in thermal equilibrium, its energy density today would be much larger than that of the observed dark matter, so we consider energy injection by the decay of N2. In this paper, we show the parameters of this scenario that give the correct abundances of dark matter and baryonic matter and also induce the observed neutrino masses. This model can explain a possible sterile neutrino dark matter signal of M1=7 keV in the x-ray observation of x-ray multi-mirror mission.

Tsuyuki, Takanao

2014-07-01

350

Neutrino mass and magnetic moment in supersymmetry without R-parity in the light of recent data  

NASA Astrophysics Data System (ADS)

We consider the generation of neutrino Majorana mass and transition magnetic moment by the lepton-number violating /? and/or /?' couplings in R-parity-violating supersymmetric models. We update (and improve) the existing upper limits on the relevant couplings using the most recent data on neutrino masses and mixings, indicating also the possible improvement by the GENIUS project. We study the implication of this update on the induced neutrino magnetic moment.

Bhattacharyya, G.; Klapdor-Kleingrothaus, H. V.; Päs, H.

1999-09-01

351

Evidence for neutrino oscillations in the Sudbury Neutrino Observatory  

SciTech Connect

The Sudbury Neutrino Observatory (SNO) is a large-volume heavy water Cerenkov detector designed to resolve the solar neutrino problem. SNO observes charged-current interactions with electron neutrinos, neutral-current interactions with all active neutrinos, and elastic-scattering interactions primarily with electron neutrinos with some sensitivity to other flavors. This dissertation presents an analysis of the solar neutrino flux observed in SNO in the second phase of operation, while {approx}2 tonnes of salt (NaCl) were dissolved in the heavy water. The dataset here represents 391 live days of data. Only the events above a visible energy threshold of 5.5 MeV and inside a fiducial volume within 550 cm of the center of the detector are studied. The neutrino flux observed via the charged-current interaction is [1.71 {+-} 0.065(stat.){+-}{sub 0.068}{sup 0.065}(sys.){+-}0.02(theor.)] x 10{sup 6}cm{sup -2}s{sup -1}, via the elastic-scattering interaction is [2.21{+-}0.22(stat.){+-}{sub 0.12}{sup 0.11}(sys.){+-}0.01(theor.)] x 10{sup 6}cm{sup -2}s{sup -1}, and via the neutral-current interaction is [5.05{+-}0.23(stat.){+-}{sub 0.37}{sup 0.31}(sys.){+-}0.06(theor.)] x 10{sup 6}cm{sup -2}s{sup -1}. The electron-only flux seen via the charged-current interaction is more than 7{sigma} below the total active flux seen via the neutral-current interaction, providing strong evidence that neutrinos are undergoing flavor transformation as they travel from the core of the Sun to the Earth. The most likely origin of the flavor transformation is matter-induced flavor oscillation.

Marino, Alysia Diane

2004-08-10

352

Sterile Neutrinos and IceCube  

E-print Network

Although the framework for oscillations of the three neutrino flavors in the Standard Model has been convincingly established, indications persist that it may be incomplete. Challenges are coming from the LSND and MiniBooNe short-baseline experiments, from the neutrino sources used in the Gallex and Sage solar neutrino experiments and, more recently,from an a-posteriori analysis of reactor neutrino experiments. One way to accommodate the reported "anomalies", if real, is to introduce one or more sterile neutrinos in the mass range $\\delta m^2 \\sim 1 eV^2$. TeV atmospheric neutrinos propagating through the Earth undergo resonant oscillations in the presence of sterile neutrinos; a clear signature in a neutrino telescope like IceCube is the the change in shape of the zenith-energy distribution of the atmospheric neutrinos.

Francis Halzen

2011-11-03

353

Neutrino propagation in nuclear medium and neutrinoless double-? decay.  

PubMed

We discuss a novel effect in neutrinoless double-? (0???) decay related with the fact that its underlying mechanisms take place in the nuclear matter environment. We study the neutrino exchange mechanism and demonstrate the possible impact of nuclear medium via lepton-number-violating (LNV) four-fermion interactions of neutrinos with quarks from a decaying nucleus. The net effect of these interactions is the generation of an effective in-medium Majorana neutrino mass matrix. The enhanced rate of the 0??? decay can lead to the apparent incompatibility of observations of the 0??? decay with the value of the neutrino mass determined or restricted by the ?-decay and cosmological data. The effective neutrino masses and mixing are calculated for the complete set of the relevant four-fermion neutrino-quark operators. Using experimental data on the 0??? decay in combination with the ?-decay and cosmological data, we evaluate the characteristic scales of these operators: ?LNV?2.4??TeV. PMID:24765948

Kovalenko, S; Krivoruchenko, M I; Simkovic, F

2014-04-11

354

First measurement of the flux of solar neutrinos from the sun at the Sudbury Neutrino Observatory  

NASA Astrophysics Data System (ADS)

The Sudbury Neutrino Observatory (SNO) is a second generation solar neutrino detector. SNO is the first experiment that is able to measure both the electron neutrino flux and a flavor-blind flux of all active neutrino types, allowing a model-independent determination if the deficit of solar neutrinos known as the solar neutrino problem is due to neutrino oscillation. The Sudbury Neutrino Observatory started taking production data in November, 1999. A measurement of the charged current rate will be the first indication if SNO too sees a suppression of the solar neutrino signal relative to the theoretical predictions. Such a confirmation is the first step in SNO's ambitious science program. In this thesis, we present evidence that SNO is seeing solar neutrinos and a preliminary ratio of the measured vs predicted rate of electrons as induced by 8B neutrinos in the ?e, + d --> p + p + e charged-current (CC) reaction.

Wittich, Peter

2000-12-01

355

Search for Possible Neutrino Decay During the 1999 Solar Eclipse  

Microsoft Academic Search

The solar neutrino problem could arise from the oscillation of one neutrino type into a second type. Neutrinos would have a mass and there could be the possibility of radiative neutrino decays. We discuss the search for neutrino decays during the 1999 total solar eclipse: it involves the emitted visible photons, while neutrinos travel from the Moon to the Earth.

S. Cecchini; G. Giacomelli; D. Hasegan; G. Mandrioli; O. Maris; L. Patrizii; V. Popa; L. Stefanov

1999-01-01

356

Primordial nucleosynthesis and neutrino physics.  

E-print Network

??We study primordial nucleosynthesis abundance yields for assumed ranges of cosmological lepton numbers, sterile neutrino mass-squared differences and active-sterile vacuum mixing angles. We fix the… (more)

Smith, Christel Johanna

2009-01-01

357

The Evolution of Neutrino Astronomy  

E-print Network

How did neutrino astronomy evolve? Are there any useful lessons for astronomers and physicists embarking on new observational ventures today? We answer the first question; the reader can can decide if there are any useful parallels for other fields.

John Bahcall; Raymond Davis, Jr

2000-04-08

358

Neutrinos and Nucleosynthesis in Supernova  

E-print Network

The type II supernova is considered as a candidate site for the production of heavy elements. The nucleosynthesis occurs in an intense neutrino flux, we calculate the electron fraction in this environment.

U. Solis; J. C. D'Olivo; L. G. Cabral-Rosetti

2005-11-12

359

High-Energy Neutrino Astronomy  

E-print Network

Kilometer-scale neutrino detectors such as IceCube are discovery instruments covering nuclear and particle physics, cosmology and astronomy. Examples of their multidisciplinary missions include the search for the particle nature of dark matter and for additional small dimensions of space. In the end, their conceptual design is very much anchored to the observational fact that Nature accelerates protons and photons to energies in excess of 10^{20} and 10^{13} eV, respectively. The cosmic ray connection sets the scale of cosmic neutrino fluxes. In this context, we discuss the first results of the completed AMANDA detector and the reach of its extension, IceCube. Similar experiments are under construction in the Mediterranean. Neutrino astronomy is also expanding in new directions with efforts to detect air showers, acoustic and radio signals initiated by neutrinos with energies similar to those of the highest energy cosmic rays.

F. Halzen

2005-01-26

360

Standard and non-standard primordial neutrinos  

E-print Network

The standard cosmological model predicts the existence of a cosmic neutrino background with a present density of about 110 cm^{-3} per flavour, which affects big-bang nucleosynthesis, cosmic microwave background anisotropies, and the evolution of large scale structures. We report on a precision calculation of the cosmic neutrino background properties including the modification introduced by neutrino oscillations. The role of a possible neutrino-antineutrino asymmetry and the impact of non-standard neutrino-electron interactions on the relic neutrinos are also briefly discussed.

P. D. Serpico

2006-06-02

361

Probing New Physics with Astrophysical Neutrinos  

E-print Network

We review the prospects for probing new physics with neutrino astrophysics. High energy neutrinos provide an important means of accessing physics beyond the electroweak scale. Neutrinos have a number of advantages over conventional astronomy and, in particular, carry information encoded in their flavor degree of freedom which could reveal a variety of exotic neutrino properties. We also outline ways in which neutrino astrophysics can be used to constrain dark matter properties, and explain how neutrino-based limits lead to a strong general bound on the dark matter total annihilation cross-section.

Nicole F. Bell

2008-11-06

362

Status of non-standard neutrino interactions.  

PubMed

The phenomenon of neutrino oscillations has been established as the leading mechanism behind neutrino flavor transitions, providing solid experimental evidence that neutrinos are massive and lepton flavors are mixed. Here we review sub-leading effects in neutrino flavor transitions known as non-standard neutrino interactions (NSIs), which is currently the most explored description for effects beyond the standard paradigm of neutrino oscillations. In particular, we report on the phenomenology of NSIs and their experimental and phenomenological bounds as well as an outlook for future sensitivity and discovery reach. PMID:23481442

Ohlsson, Tommy

2013-04-01

363

Plasma wave instabilities induced by neutrinos  

E-print Network

Quantum field theory is applied to study the interaction of an electron plasma with an intense neutrino flux. A connection is established between the field theory results and classical kinetic theory. The dispersion relation and damping rate of the plasma longitudinal waves are derived in the presence of neutrinos. It is shown that Supernova neutrinos are never collimated enough to cause non-linear effects associated with a neutrino resonance. They only induce neutrino Landau damping, linearly proportional to the neutrino flux and $G_{\\mathrm{F}}^{2}$.

Luis Bento

1999-12-29

364

Neutrino Oscillations: a source of Goldstone fields  

E-print Network

It is proved that true Goldstone bosons develop coherent fields whenever the associated charges of the matter particles are not conserved in a macroscopic scale. The sources of the Goldstone fields are the time rates of quantum number violation. The case of neutrino flavour oscillations is studied with application to Supernovae. It is shown that if the Lepton numbers break at the Fermi scale, the neutrino potentials and oscillation patterns change in the periods of largest neutrino fluxes. In this way, electron anti-neutrino to muon anti-neutrino oscillations may occur in the first instants of neutrino emission.

Luis Bento

1997-11-30

365

Neutrino scattering and flavor transformation in supernovae.  

PubMed

We argue that the small fraction of neutrinos that undergo direction-changing scattering outside of the neutrinosphere could have significant influence on neutrino flavor transformation in core-collapse supernova environments. We show that the standard treatment for collective neutrino flavor transformation is adequate at late times but could be inadequate in early epochs of core-collapse supernovae, where the potentials that govern neutrino flavor evolution are affected by the scattered neutrinos. Taking account of this effect, and the way it couples to entropy and composition, will require a new approach in neutrino flavor transformation modeling. PMID:23004955

Cherry, John F; Carlson, J; Friedland, Alexander; Fuller, George M; Vlasenko, Alexey

2012-06-29

366

40 years of neutrino physics  

NASA Astrophysics Data System (ADS)

Wolfgang Pauli and Enrico Fermi pioneered the hypothesis and characteristics of the weak interaction and the elementary particle called the neutrino. Since its discovery some forty years ago the neutrino has been shown to be a fundamental constituent of matter with a surprisingly rich, and in very many ways unexpected, set of characteristics ranging from basic roles in the generation of energy in the sun to supernovæ.

Reines, Frederick

367

One-loop contribution to the neutrino mass matrix in the next-to-minimal supersymmetric standard model with right-handed neutrinos and tribimaximal mixing  

NASA Astrophysics Data System (ADS)

Neutrino mass patterns and mixing have been studied in the context of the next-to-minimal supersymmetric standard model (NMSSM) with three gauge singlet neutrino superfields. We consider the case with the assumption of R-parity conservation. The vacuum expectation value of the singlet scalar field S of NMSSM induces the Majorana masses for the right-handed neutrinos as well as the usual ? term. The contributions to the light neutrino mass matrix at the tree level as well as one-loop level are considered, consistent with the tribimaximal pattern of neutrino mixing. Light neutrino masses arise at the tree level through a TeV-scale seesaw mechanism involving the right-handed neutrinos. Although all the three light neutrinos acquire nonzero masses at the tree level, we show that the one-loop contributions can be comparable in size under certain conditions. Possible signatures to probe this model at the LHC and its distinguishing features compared to other models of neutrino mass generation are briefly discussed.

Das, Debottam; Roy, Sourov

2010-08-01

368

MeV neutrinos in double {beta} decay  

SciTech Connect

The effect of Majorana neutrinos in the MeV mass range on the double {beta} decay of various isotopes is studied on pure phenomenological arguments. By using only experimental half-life data, limits on the mixing parameter U{sub eh}{sup 2} of the order 10{sup {minus}7} can be derived. Also the possible achievements of upcoming experiments and some consequences are outlined. {copyright} {ital 1997} {ital The American Physical Society}

Zuber, K. [Lehrstuhl fuer Experimentelle Physik IV, Universitaet Dortmund, Otto-Hahn-Strasse 4, D-44221 Dortmund (Germany)] [Lehrstuhl fuer Experimentelle Physik IV, Universitaet Dortmund, Otto-Hahn-Strasse 4, D-44221 Dortmund (Germany)

1997-08-01

369

On the Compound Structures of the Neutrino Mass and Charge  

E-print Network

The mass and charge of a particle correspond to the most diverse form of the same regularity of the nature of this field. As a consequence, each of all possible types of charges testifies in favor of the existence of a kind of inertial mass. Therefore, to investigate these features, we have established the compound structures of mass and charge. They can explain also the availability of fundamental differences in the masses as well as in the charges of Dirac and Majorana neutrinos.

Rasulkhozha S. Sarafiddinov

2010-12-07

370

Extraterrestrial high energy neutrino fluxes  

NASA Technical Reports Server (NTRS)

Using the most recent cosmic ray spectra up to 2x10 to the 20th power eV, production spectra of high energy neutrinos from cosmic ray interactions with interstellar gas and extragalactic interactions of ultrahigh energy cosmic rays with 3K universal background photons are presented and discussed. Estimates of the fluxes from cosmic diffuse sources and the nearby quasar 3C273 are made using the generic relationship between secondary neutrinos and gammas and using recent gamma ray satellite data. These gamma ray data provide important upper limits on cosmological neutrinos. Quantitative estimates of the observability of high energy neutrinos from the inner galaxy and 3C273 above atmospheric background for a DUMAND type detector are discussed in the context of the Weinberg-Salam model with sq sin theta omega = 0.2 and including the atmospheric background from the decay of charmed mesons. Constraints on cosmological high energy neutrino production models are also discussed. It appears that important high energy neutrino astronomy may be possible with DUMAND, but very long observing times are required.

Stecker, F. W.

1979-01-01

371

Neutrino Masses and Leptogenesis in Type I+II Seesaw Models  

E-print Network

The baryon to photon ratio in the present Universe is very accurately measured to be $(6.065 \\pm 0.090) \\times 10^{-10}$. We study the possible origin of this baryon asymmetry in the neutrino sector through the generic mechanism of baryogenesis through leptogenesis. We consider both type I and type II seesaw origin of neutrino masses within the framework of left right symmetric models (LRSM). Using the latest best fit global neutrino oscillation data of mass squared differences, mixing angles and Dirac CP phase, we compute the predictions for baryon to photon ratio keeping the Majorana CP phases as free parameters for two different choices of lightest neutrino mass eigenvalue for both normal and inverted hierarchical patterns of neutrino masses. We do our calculation with and without lepton flavor effects being taken into account. We choose different diagonal Dirac neutrino mass matrix for different flavor effects in such a way that the lightest right handed neutrino mass is in the appropriate range. We also study the predictions for baryon asymmetry when the neutrino masses arise from a combination of both type I and type II seesaw (with dominating type I term) and discriminate between several combinations of Dirac and Majorana CP phases by demanding successful predictions for baryon asymmetry.

Debasish Borah; Mrinal Kumar Das

2014-06-23

372

Strongly interacting astrophysical neutrinos  

NASA Astrophysics Data System (ADS)

The origin and chemical composition of ultrahigh energy cosmic rays is still an open question in astroparticle physics. The observed large-scale isotropy and also direct composition measurements can be interpreted as an extragalactic proton dominance above the ankle at about 1010 GeV. Photopion production of extragalactic protons in the cosmic microwave background predicts a cut-off at about 5×1010 GeV in conflict with excesses reported by some experiments. In this report we will outline a recent statistical analysis [M. Ahlers, A. Ringwald, H. Tu, Astropart. Phys. (in press). Preprint astro-ph/0506698] of cosmic ray data using strongly interacting neutrinos as primaries for these excesses.

Ahlers, Markus

2006-07-01

373

Loop-induced neutrino masses: A case study  

NASA Astrophysics Data System (ADS)

We study the cocktail model in which the Majorana neutrino masses are generated by the so-called "cocktail" three-loop diagrams with the dark matter particle running in the loops. In particular, we give the analytic expressions of the neutrino masses in the model by the detailed calculation of the cocktail diagrams. Based on the numerical calculation of the loop integrals, we explore the parameter space which can give the correct orders of neutrino masses while satisfying other experimental constraints, such as those from the neutrinoless double beta decay, low-energy lepton flavor violation processes, electroweak precision tests, and collider searches. As a result, the large couplings and the large mass difference between the two singly charged (neutral) scalars are required.

Geng, Chao-Qiang; Huang, Da; Tsai, Lu-Hsing

2014-12-01

374

Neutrino masses, grand unification, and baryon number violation  

NASA Astrophysics Data System (ADS)

If grand unification is real, searches for baryon-number violation should be included on the list of observables that may reveal information regarding the origin of neutrino masses. Making use of an effective-operator approach and assuming that nature is SU(5) invariant at very short distances, we estimate the consequences of different scenarios that lead to light Majorana neutrinos for low-energy phenomena that violate baryon number minus lepton number (B -L) by two (or more) units, including neutron-antineutron oscillations and B -L violating nucleon decays. We find that, among all possible effective theories of lepton-number violation that lead to nonzero neutrino masses, only a subset is, broadly speaking, consistent with grand unification.

de Gouvêa, André; Herrero-García, Juan; Kobach, Andrew

2014-07-01

375

Neutrino Masses, Grand Unification, and Baryon Number Violation  

E-print Network

If grand unification is real, searches for baryon-number violation should be included on the list of observables that may reveal information regarding the origin of neutrino masses. Making use of an effective-operator approach and assuming that nature is SU(5) invariant at very short distances, we estimate the consequences of different scenarios that lead to light Majorana neutrinos for low-energy phenomena that violate baryon number minus lepton number (B-L) by two (or more) units, including neutron-antineutron oscillations and B-L violating nucleon decays. We find that, among all possible effective theories of lepton-number violation that lead to nonzero neutrino masses, only a subset is, broadly speaking, consistent with grand unification.

Andre de Gouvea; Juan Herrero-Garcia; Andrew Kobach

2014-04-15

376

Neutrino factories: realization and physics potential  

SciTech Connect

Neutrino Factories offer an exciting option for the long-term neutrino physics program. This new type of neutrino facility will provide beams with unique properties. Low systematic uncertainties at a Neutrino Factory, together with a unique and precisely known neutrino flavor content, will enable neutrino oscillation measurements to be made with unprecedented sensitivity and precision. Over recent years, the resulting neutrino factory physics potential has been discussed extensively in the literature. In addition, over the last six years the R&D necessary to realize a Neutrino Factory has been progressing, and has developed into a significant international activity. It is expected that, within about five more years, the initial phase of this R&D program will be complete and, if the community chooses to build this new type of neutrino source within the following decade, neutrino factory technology will be ready for the final R&D phase prior to construction. In this paper (1) an overview is given of the technical ingredients needed for a Neutrino Factory, (2) beam properties are described, (3) the resulting neutrino oscillation physics potential is summarized, (4) a more detailed description is given for one representative Neutrino Factory design, and (5) the ongoing R&D program is summarized, and future plans briefly described.

Geer, S.; /Fermilab; Zisman, M.S.; /LBL, Berkeley

2006-12-01

377

Atmospheric Neutrinos in the MINOS Far Detector  

SciTech Connect

The phenomenon of flavour oscillations of neutrinos created in the atmosphere was first reported by the Super-Kamiokande collaboration in 1998 and since then has been confirmed by Soudan 2 and MACRO. The MINOS Far Detector is the first magnetized neutrino detector able to study atmospheric neutrino oscillations. Although it was designed to detect neutrinos from the NuMI beam, it provides a unique opportunity to measure the oscillation parameters for neutrinos and anti-neutrinos independently. The MINOS Far Detector was completed in August 2003 and since then has collected 2.52 kton-years of atmospheric data. Atmospheric neutrino interactions contained within the volume of the detector are separated from the dominant background from cosmic ray muons. Thirty seven events are selected with an estimated background contamination of less than 10%. Using the detector's magnetic field, 17 neutrino events and 6 anti-neutrino events are identified, 14 events have ambiguous charge. The neutrino oscillation parameters for {nu}{sub {mu}} and {bar {nu}}{sub {mu}} are studied using a maximum likelihood analysis. The measurement does not place constraining limits on the neutrino oscillation parameters due to the limited statistics of the data set analysed. However, this thesis represents the first observation of charge separated atmospheric neutrino interactions. It also details the techniques developed to perform atmospheric neutrino analyses in the MINOS Far Detector.

Howcroft, Caius L.F.; /Cambridge U.

2004-12-01

378

Neutrino dipole moments and charge radii in non-commutative space-time  

NASA Astrophysics Data System (ADS)

In this paper we obtain a bound ?_{NC}stackrel{ < }{˜} 150 TeV on the scale of space-time non-commutativity considering photon-neutrino interactions. We compute “*-dipole moments” and “*-charge radii” originating from space-time non-commutativity and compare them with the dipole moments calculated in the neutrino-mass extended standard model (SM). The computation depends on the nature of the neutrinos, Dirac versus Majorana, their mass and the energy scale. We focus on Majorana neutrinos. The “*-charge radius” is found to be r^* = sqrt{|< r^2_{?}rangle_{NC}|}=left|3sum_{i=1}^3 ({?}^{0i})^2right|^{1/4} stackrel{<}{˜} 1.6 × 10^{-19} {cm} at ?_{NC} = 150 TeV.

Minkowski, P.; Schupp, P.; Trampeti?, J.

2004-09-01

379

Neutrino Physics Neutrinos rarely interact despite their vast abundance in nature. To give a sense of  

E-print Network

Chapter 1 Neutrino Physics Neutrinos rarely interact despite their vast abundance in nature. To give a sense of scale, a person has roughly 1016 neutrinos passing through them each second, completely unnoticed. Nonetheless, neutrinos can still be used to probe the fundamental laws of na- ture

380

Neutrinos and Arms Control: Thinking Big about Detection of Neutrinos from  

E-print Network

Neutrinos and Arms Control: Thinking Big about Detection of Neutrinos from Reactors at Long for a world network of enormous neutrino detec- tors, which may be employed for monitoring the activity of allV, placed in the deep oceans (or possibly lakes) can record the electron anti-neutrino uxes from reactors

Learned, John

381

Reactor Monitoring Reactor Monitoring (near and far) with Neutrinos(near and far) with Neutrinos  

E-print Network

1 Reactor Monitoring Reactor Monitoring (near and far) with Neutrinos(near and far) with Neutrinos Neutrino Applications are on the horizon John G. LearnedJohn G. Learned Physics and Astronomy, University and astrophysics, initiator and participant in many neutrino experiments (IMB, DUMAND, SuperK, KamLAND, K2K

Learned, John

382

Neutrinos and Arms Control: Thinking Big about Detection of Neutrinos from  

E-print Network

Neutrinos and Arms Control: Thinking Big about Detection of Neutrinos from Reactors at Long for a world network of enormous neutrino detec­ tors, which may be employed for monitoring the activity of allV, placed in the deep oceans (or possibly lakes) can record the electron anti­neutrino fluxes from reactors

Learned, John

383

The solar neutrino problem in the presence of flavor-changing neutrino interactions  

NASA Astrophysics Data System (ADS)

We study the effects of flavor-changing neutrino interactions on the resonant conversion of solar neutrinos. In particular, we describe how the regions in the ?m2-sin 22? plane that are consistent with the four solar neutrino experiments are modified for different strengths of New Physics neutrino interactions.

Bergmann, Sven

1998-03-01

384

17 keV neutrino and large magnetic moment solution of the solar neutrino puzzle  

E-print Network

Zee-type models with Majorons naturally incorporate the 17 keV neutrino but in their minimal version fail to simultaneously solve the solar neutrino puzzle. If there is a sterile neutrino state, we find a particularly simple solution to the solar neutrino problem, which besides $\

Eugeni Akhmedov; Zurab Berezhiani; Goran Senjanovic; Zhijian Tao

1992-09-02

385

Solar neutrino oscillations and bounds on neutrino magnetic moment and solar magnetic field  

Microsoft Academic Search

If the observed deficit of solar neutrinos is due to neutrino oscillations, neutrino conversions caused by the interaction of their transition magnetic moments with the solar magnetic field (spin-flavour precession) can still be present at a subdominant level. In that case, the combined action of neutrino oscillations and spin-flavour precession can lead to a small but observable flux of electron

E. Kh. Akhmedov

2003-01-01

386

Solar neutrino oscillations and bounds on neutrino magnetic moment and solar magnetic field  

Microsoft Academic Search

If the observed deficit of solar neutrinos is due to neutrino oscillations, neutrino conversions caused by the interaction of their transition magnetic moments with the solar magnetic field (spin-flavour precession) can still be present at a subdominant level. In that case, the combined action of neutrino oscillations and spin-flavour pre- cession can lead to a small but observable flux of

E. Kh; Joao Pulido

387

A Search for Neutrinos from the Solar hep Reaction and the Diffuse Supernova Neutrino Background with the Sudbury Neutrino Observatory  

Microsoft Academic Search

A search has been made for neutrinos from the hep reaction in the Sun and from the diffuse supernova neutrino background (DSNB) using data collected during the first operational phase of the Sudbury Neutrino Observatory, with an exposure of 0.65 ktons yr. For the hep neutrino search, two events are observed in the effective electron energy range of 14.3 MeV

B. Aharmim; S. N. Ahmed; A. E. Anthony; E. W. Beier; A. Bellerive; M. Bergevin; S. D. Biller; M. G. Boulay; Y. D. Chan; M. Chen; X. Chen; B. T. Cleveland; G. A. Cox; C. A. Currat; X. Dai; F. Dalnoki-Veress; H. Deng; J. Detwiler; M. DiMarco; P. J. Doe; G. Doucas; P.-L. Drouin; F. A. Duncan; M. Dunford; J. A. Dunmore; E. D. Earle; H. C. Evans; G. T. Ewan; J. Farine; H. Fergani; F. Fleurot; R. J. Ford; J. A. Formaggio; N. Gagnon; J. Tm. Goon; K. Graham; E. Guillian; R. L. Hahn; A. L. Hallin; E. D. Hallman; P. J. Harvey; R. Hazama; K. M. Heeger; W. J. Heintzelman; J. Heise; R. L. Helmer; R. J. Hemingway; R. Henning; A. Hime; C. Howard; M. A. Howe; M. Huang; P. Jagam; N. A. Jelley; J. R. Klein; L. L. Kormos; M. Kos; A. Krüger; C. B. Krauss; T. Kutter; C. C. M. Kyba; H. Labranche; R. Lange; J. Law; I. T. Lawson; K. T. Lesko; J. R. Leslie; J. C. Loach; S. Luoma; R. MacLellan; S. Majerus; H. B. Mak; J. Maneira; A. D. Marino; R. Martin; N. McCauley; A. B. McDonald; S. McGee; C. Mifflin; K. K. S. Miknaitis; M. L. Miller; B. Monreal; B. G. Nickel; A. J. Noble; E. B. Norman; N. S. Oblath; C. E. Okada; H. M. O'Keeffe; G. D. Orebi Gann; S. M. Oser; R. Ott; S. J. M. Peeters; A. W. P. Poon; G. Prior; K. Rielage; B. C. Robertson; R. G. H. Robertson; E. Rollin; M. H. Schwendener; J. A. Secrest; S. R. Seibert; O. Simard; C. J. Sims; D. Sinclair; P. Skensved; R. G. Stokstad; L. C. Stonehill; G. Tesic; N. Tolich; T. Tsui; R. Van Berg; R. G. Van de Water; B. A. VanDevender; C. J. Virtue; T. J. Walker; B. L. Wall; D. Waller; H. Wan Chan Tseung; D. L. Wark; J. Wendland; J. F. Wilkerson; J. R. Wilson; J. M. Wouters; A. Wright; M. Yeh; F. Zhang; K. Zuber

2006-01-01

388

Long-range correlations of neutrinos in hadron reactions and neutrino diffraction II: neutrino  

E-print Network

In this II, a probability to detect the neutrino produced in a high-energy pion decay is shown to receive the large finite-size correction. The neutrino interacts extremely weakly with matters and is described with a many-body wave function together with the pion and charged lepton. This wave function slowly approaches to an asymptotic form, which is probed by the neutrino. The whole process is described by an S-matrix of a finite-time interval, which couples with states of non-conserving kinetic energy, and the final states of a broad spectrum specific to a relativistic invariant system contribute to the positive semi-definite correction similar to diffraction of waves through a hole. This diffraction component for the neutrino becomes long range and stable under changes of the pion's energy. Moreover, it has a universal form that depends on the absolute neutrino mass. Thus a new method of measuring the absolute neutrino mass is suggested.

Kenzo Ishikawa; Yutaka Tobita

2012-09-25

389

Supernova neutrino signals by liquid Argon detector and neutrino magnetic moment  

NASA Astrophysics Data System (ADS)

We study ? and ? signals from a supernova with strong magnetic field detected by a 100 kton liquid Ar detector. The change of neutrino flavors by resonant spin-flavor conversions, matter effects, and neutrino self-interactions are taken into account. Different neutrino signals, characterized by the total event numbers of ? and ? and neutronization burst event, are expected with different neutrino oscillation parameters and neutrino magnetic moment. Observations of supernova neutrino signals by a 100 kton liquid Ar detector would constrain oscillation parameters as well as neutrino magnetic moment in either normal and inverted mass hierarchies.

Yoshida, Takashi; Takamura, Akira; Kimura, Keiichi; Kawagoe, Shio; Kajino, Toshitaka; Yokomakura, Hidekazu

2011-10-01

390

One Right-handed Neutrino to Generate Complete Neutrino Mass Spectrum in the Framework of NMSSM  

E-print Network

The see-saw mechanism is usually applied to explain the lightness of neutrinos. The traditional see-saw mechanism introduces at least two right-handed neutrinos for the realistic neutrino spectrum. In the case of supersymmetry, loop corrections can also contribute to neutrino masses, which lead to the possibility to generate the neutrino spectrum by introducing just one right-handed neutrino. To be realistic, MSSM suffers from the mu problem and other phenomenological difficulties, so we extend NMSSM (the MSSM with a singlet S) by introducing one single right-handed neutrino superfield (N) and relevant phenomenology is discussed

Yi-Lei Tang

2014-11-07

391

One right-handed neutrino to generate complete neutrino mass spectrum in the framework of NMSSM  

NASA Astrophysics Data System (ADS)

The see-saw mechanism is usually applied to explain the lightness of neutrinos. The traditional see-saw mechanism introduces at least two right-handed neutrinos for the realistic neutrino spectrum. In the case of supersymmetry, loop corrections can also contribute to neutrino masses, which lead to the possibility to generate the neutrino spectrum by introducing just one right-handed neutrino. To be realistic, MSSM suffers from the ? problem and other phenomenological difficulties, so we extend NMSSM (the MSSM with a singlet S) by introducing one single right-handed neutrino superfield (N) and relevant phenomenology is discussed.

Tang, Yi-Lei

2015-01-01

392

Neutrino oscillations in the early universe with an inverted neutrino-mass hierarchy  

NASA Astrophysics Data System (ADS)

Nuclear simulations of neutrino oscillations in the early Universe are performed for a neutrino-mass hierarchy with the vacuum mass of the second neutrino exceeding that of the first. This situation is equivalent to a normal hierarchy with mixing angle greater than ?/4. We find that a large conversion of electron neutrinos to muon neutrinos occurs, independent of mixing angle. For certain parameter values, this is caused by the MSW effect. In the rest of the parameter region a new mechanism is operative, arising from nonlinear effects involving neutrino-neutrino forward scattering. This nonlinear conversion mechanism causes substantial flavor oscillation even for extremely small mixing angles.

Kostelecký, V. Alan; Samuel, Stuart

1993-11-01

393

Neutrino masses and mixings in gauge models with spontaneous parity violation  

Microsoft Academic Search

Unified electroweak gauge theories based on the gauge group SU(2)L×SU(2)R×U(1)B-L, in which the breakdown of parity invariance is spontaneous, lead most naturally to a massive neutrino. Assuming the neutrino to be a Majorana particle, we show that smallness of its mass can be understood as a result of the observed maximality of parity violation in low-energy weak interactions. This result

Rabindra N. Mohapatra; Goran Senjanovic

1981-01-01

394

Singlet Interacting Neutrinos in the Extended Zee Model and Solar Neutrino Transformation  

E-print Network

We study the impact of Standard Model singlet neutrinos on neutrino flavor transformation. We focus on an extension of the Zee model which includes singlet neutrinos, and find that the best limits on the interactions of the singlet neutrinos come from astrophysical phenomena. Singlet neutrino-electron scattering will impact both the mattter enhanced flavor transformation potential as well as detector cross sections. If electron neutrino - singlet neutrino oscillations are responsible for the solar neutrino anomaly, then the limit on the singlet neutrino interaction strength is of order of the weak interaction scale. Zee model modification of nu_tau - e scattering also impacts solar neutrino transformation, although this interaction is more tightly constrained.

G. C. McLaughlin; J. N. Ng

1999-07-21

395

Probing the absolute mass scale of neutrinos  

E-print Network

The Karlsruhe Tritium Neutrino (KATRIN) experiment is the next generation tritium beta decay experiment with sub-eV sensitivity to make a direct, model independent measurement of the neutrino mass. The principle of the ...

Formaggio, Joseph A.

396

Annual modulation of cosmic relic neutrinos  

E-print Network

The cosmic neutrino background (C?B), produced about one second after the big bang, permeates the Universe today. New technological advancements make neutrino capture on beta-decaying nuclei (NCB) a clear path forward ...

Safdi, Benjamin R.

397

Nucleosynthesis in neutrino-driven winds.  

E-print Network

??In this thesis the influence of neutrino-induced spallation rates on the nucleosynthesis is investigated. These neutrino-induced rates are studied in various nucleosynthesis processes such as… (more)

Huther, Lutz

2013-01-01

398

Neutrino mixing, flavor states and dark energy  

E-print Network

We shortly summarize the quantum field theory formalism for the neutrino mixing and report on recent results showing that the vacuum condensate induced by neutrino mixing can be interpreted as a dark energy component of the Universe.

M. Blasone; A. Capolupo; S. Capozziello; G. Vitiello

2007-11-06

399

Neutrino clustering around spherical dark matter halos  

E-print Network

Cold dark matter halos form within a smoothly distributed background of relic neutrinos -- at least some of which are massive and non-relativistic at late times. We calculate the accumulation of massive neutrinos around spherically collapsing cold dark matter halos in a cosmological background. We identify the physical extent of the "neutrino halo" in the spherical collapse model, which is large in comparison with the virial radius of the dark matter, and conditions under which neutrinos reaching the cold dark matter halo will remain bound to the halo at late times. We calculate the total neutrino mass and bound neutrino mass associated with isolated spherical halos for several neutrino mass hierarchies and provide fitting formulae for these quantities in terms of the cold dark matter halo mass and the masses of the individual neutrino species.

LoVerde, Marilena

2013-01-01

400

Neutrino physics: What makes the Sun shine  

NASA Astrophysics Data System (ADS)

Neutrinos produced in the nuclear reaction that triggers solar-energy generation have been detected. This milestone in the search for solar neutrinos required a deep underground detector of exceptional sensitivity. See Article p.383

Haxton, Wick

2014-08-01

401

Observation of electron neutrino appearance in a muon neutrino beam.  

PubMed

The T2K experiment has observed electron neutrino appearance in a muon neutrino beam produced 295 km from the Super-Kamiokande detector with a peak energy of 0.6 GeV. A total of 28 electron neutrino events were detected with an energy distribution consistent with an appearance signal, corresponding to a significance of 7.3? when compared to 4.92±0.55 expected background events. In the Pontecorvo-Maki-Nakagawa-Sakata mixing model, the electron neutrino appearance signal depends on several parameters including three mixing angles ?12, ?23, ?13, a mass difference ?m(32)(2) and a CP violating phase ?(CP). In this neutrino oscillation scenario, assuming |?m(32)(2)|=2.4×10(-3)??eV(2), sin(2)?(23)=0.5, and ?m322>0 (?m(32)(2)<0), a best-fit value of sin(2)2?(13)=0.140(-0.032)(+0.038) (0.170(-0.037)(+0.045)) is obtained at ?(CP)=0. When combining the result with the current best knowledge of oscillation parameters including the world average value of ?(13) from reactor experiments, some values of ?(CP) are disfavored at the 90% C.L. PMID:24580687

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; 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; Floetotto, L; Friend, M; Fujii, Y; Fukuda, Y; Furmanski, A P; Galymov, V; Gaudin, A; Giffin, S; Giganti, C; Gilje, K; Goeldi, D; 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; 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; Kisiel, J; Kitching, P; Kobayashi, T; Koch, L; 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; Lamont, I; Laveder, M; Lawe, M; Lazos, M; Lee, K P; Licciardi, C; Lindner, T; Lister, C; Litchfield, R P; Longhin, A; Ludovici, L; Macaire, M; Magaletti, L; Mahn, K; Malek, M; Manly, S; Marino, A D; Marteau, J; Martin, J F; Maruyama, T; Marzec, J; Mathie, E L; Matveev, V; Mavrokoridis, K; Mazzucato, E; McCarthy, M; McCauley, N; McFarland, K S; McGrew, C; Metelko, C; Mezzetto, M; 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; Owen, R A; Oyama, Y; Palladino, V; Paolone, V; Payne, D; Pearce, G F; Perevozchikov, O; Perkin, J D; Petrov, Y; Pickard, L J; 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; Rojas, P; 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; 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

2014-02-14

402

Observation of Electron Neutrino Appearance in a Muon Neutrino Beam  

E-print Network

The T2K experiment has observed electron neutrino appearance in a muon neutrino beam produced 295 km from the Super-Kamiokande detector with a peak energy of 0.6 GeV. A total of 28 electron neutrino events were detected with an energy distribution consistent with an appearance signal, corresponding to a significance of 7.3$\\sigma$ when compared to 4.92 $\\pm$ 0.55 expected background events. In the PMNS mixing model, the electron neutrino appearance signal depends on several parameters including three mixing angles $\\theta_{12}$, $\\theta_{23}$, $\\theta_{13}$, a mass difference $\\Delta m^2_{32}$ and a CP violating phase $\\delta_{\\mathrm{CP}}$. In this neutrino oscillation scenario, assuming $|\\Delta m^2_{32}| = 2.4 \\times 10^{-3}$ $\\rm eV^2$, $\\sin^2 \\theta_{23} = 0.5$, $\\delta_{\\mathrm{CP}}=0$, and $\\Delta m^2_{32} >0$ ($\\Delta m^2_{32} <0$), a best-fit value of $\\sin^2 2 \\theta_{13}$ = $0.140^{+0.038}_{-0.032}$ ($0.170^{+0.045}_{-0.037}$) is obtained.

Abe, K; 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; Rodríguez, J Caravaca; 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; 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; Floetotto, L; Friend, M; Fujii, Y; Fukuda, Y; Furmanski, A P; Galymov, V; Gaudin, A; Giffin, S; Giganti, C; Gilje, K; Goeldi, D; 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; 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; Kisiel, J; Kitching, P; Kobayashi, T; Koch, L; 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; Lamont, I; Laveder, M; Lawe, M; Lazos, M; Lee, K P; Licciardi, C; Lindner, T; Lister, C; Litchfield, R P; Longhin, A; Ludovici, L; Macaire, M; Magaletti, L; Mahn, K; Malek, M; Manly, S; Marino, A D; Marteau, J; Martin, J F; Maruyama, T; Marzec, J; 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; Owen, R A; Oyama, Y; Palladino, V; Paolone, V; Payne, D; Pearce, G F; Perevozchikov, O; Perkin, J D; Petrov, Y; Pickard, L J; Guerra, E S Pinzon; 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; 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; ?muda, J

2013-01-01

403

Neutrino-proton and anti-neutrino-proton elastic scattering  

SciTech Connect

An experiment performed at the Brookhaven National Laboratory Alternating Gradient Synchrotron observed the elastic scattering of neutrinos and anti-neutrinos from a nuclear target. The neutral current anti-neutrino to neutral current neutrino ratio is: sigma(anti ..nu..p ..-->.. anti ..nu..p)/sigma(..nu..p ..-->.. ..nu..p) = 0.45 +- 0.18 for 0.33 less than or equal to Q/sup 2/ less than or equal to 1.0 (GeV/c)/sup 2/, where Q/sup 2/ is the square of the momentum transfer to the nucleon. The neutrino neutral current to charged current ratio is: sigma(..nu..p ..-->.. ..nu..p)/sigma(..nu..n ..-->.. ..mu../sup -/p) = 0.13 +- 0.04 for 0.25 less than or equal to Q/sup 2/ less than or equal to 1.0 (GeV/c)/sup 2/. The ratios are consistent with a value of the Weinberg angle of sin/sup 2/theta/sub w/ = 0.26 +- 0.08.

Fuess, Stuart Charles

1981-01-01

404

Observation of Electron Neutrino Appearance in a Muon Neutrino Beam  

E-print Network

The T2K experiment has observed electron neutrino appearance in a muon neutrino beam produced 295 km from the Super-Kamiokande detector with a peak energy of 0.6 GeV. A total of 28 electron neutrino events were detected with an energy distribution consistent with an appearance signal, corresponding to a significance of 7.3$\\sigma$ when compared to 4.92 $\\pm$ 0.55 expected background events. In the PMNS mixing model, the electron neutrino appearance signal depends on several parameters including three mixing angles $\\theta_{12}$, $\\theta_{23}$, $\\theta_{13}$, a mass difference $\\Delta m^2_{32}$ and a CP violating phase $\\delta_{\\mathrm{CP}}$. In this neutrino oscillation scenario, assuming $|\\Delta m^2_{32}| = 2.4 \\times 10^{-3}$ $\\rm eV^2$, $\\sin^2 \\theta_{23} = 0.5$, and $\\Delta m^2_{32} >0$ ($\\Delta m^2_{32} <0$), a best-fit value of $\\sin^2 2 \\theta_{13}$ = $0.140^{+0.038}_{-0.032}$ ($0.170^{+0.045}_{-0.037}$) is obtained at $\\delta_{\\mathrm{CP}}=0$. When combining the result with the current best knowledge of oscillation parameters including the world average value of $\\theta_{13}$ from reactor experiments, some values of $\\delta_{\\mathrm{CP}}$ are disfavored at the 90% CL.

K. Abe; J. Adam; H. Aihara; T. Akiri; C. Andreopoulos; S. Aoki; A. Ariga; T. Ariga; S. Assylbekov; D. Autiero; M. Barbi; G. J. Barker; G. Barr; M. Bass; M. Batkiewicz; F. Bay; S. W. Bentham; V. Berardi; B. E. Berger; S. Berkman; I. Bertram; S. Bhadra; F. d. M. Blaszczyk; A. Blondel; C. Bojechko; S. Bordoni; S. B. Boyd; D. Brailsford; A. Bravar; C. Bronner; N. Buchanan; R. G. Calland; J. Caravaca Rodríguez; S. L. Cartwright; R. Castillo; M. G. Catanesi; A. Cervera; D. Cherdack; G. Christodoulou; A. Clifton; J. Coleman; S. J. Coleman; G. Collazuol; K. Connolly; L. Cremonesi; A. Dabrowska; I. Danko; R. Das; S. Davis; P. de Perio; G. De Rosa; T. Dealtry; S. R. Dennis; C. Densham; F. Di Lodovico; S. Di Luise; O. Drapier; T. Duboyski; K. Duffy; F. Dufour; J. Dumarchez; S. Dytman; M. Dziewiecki; S. Emery; A. Ereditato; L. Escudero; A. J. Finch; L. Floetotto; M. Friend; Y. Fujii; Y. Fukuda; A. P. Furmanski; V. Galymov; A. Gaudin; S. Giffin; C. Giganti; K. Gilje; D. Goeldi; T. Golan; J. J. Gomez-Cadenas; M. Gonin; N. Grant; D. Gudin; D. R. Hadley; A. Haesler; M. D. Haigh; P. Hamilton; D. Hansen; T. Hara; M. Hartz; T. Hasegawa; N. C. Hastings; Y. Hayato; C. Hearty; R. L. Helmer; M. Hierholzer; J. Hignight; A. Hillairet; A. Himmel; T. Hiraki; S. Hirota; J. Holeczek; S. Horikawa; K. Huang; A. K. Ichikawa; K. Ieki; M. Ieva; M. Ikeda; J. Imber; J. Insler; T. J. Irvine; T. Ishida; T. Ishii; S. J. Ives; K. Iyogi; A. Izmaylov; A. Jacob; B. Jamieson; R. A. Johnson; J. H. Jo; P. Jonsson; C. K. Jung; A. C. Kaboth; T. Kajita; H. Kakuno; J. Kameda; Y. Kanazawa; D. Karlen; I. Karpikov; E. Kearns; M. Khabibullin; A. Khotjantsev; D. Kielczewska; T. Kikawa; A. Kilinski; J. Kim; J. Kisiel; P. Kitching; T. Kobayashi; L. Koch; A. Kolaceke; A. Konaka; L. L. Kormos; A. Korzenev; K. Koseki; Y. Koshio; I. Kreslo; W. Kropp; H. Kubo; Y. Kudenko; S. Kumaratunga; R. Kurjata; T. Kutter; J. Lagoda; K. Laihem; I. Lamont; M. Laveder; M. Lawe; M. Lazos; K. P. Lee; C. Licciardi; T. Lindner; C. Lister; R. P. Litchfield; A. Longhin; L. Ludovici; M. Macaire; L. Magaletti; K. Mahn; M. Malek; S. Manly; A. D. Marino; J. Marteau; J. F. Martin; T. Maruyama; J. Marzec; E. L. Mathie; V. Matveev; K. Mavrokoridis; E. Mazzucato; M. McCarthy; N. McCauley; K. S. McFarland; C. McGrew; C. Metelko; M. Mezzetto; P. Mijakowski; C. A. Miller; A. Minamino; O. Mineev; S. Mine; A. Missert; M. Miura; L. Monfregola; S. Moriyama; Th. A. Mueller; A. Murakami; M. Murdoch; S. Murphy; J. Myslik; T. Nagasaki; T. Nakadaira; M. Nakahata; T. Nakai; K. Nakamura; S. Nakayama; T. Nakaya; K. Nakayoshi; D. Naples; C. Nielsen; M. Nirkko; K. Nishikawa; Y. Nishimura; H. M. O'Keeffe; R. Ohta; K. Okumura; T. Okusawa; W. Oryszczak; S. M. Oser; R. A. Owen; Y. Oyama; V. Palladino; V. Paolone; D. Payne; G. F. Pearce; O. Perevozchikov; J. D. Perkin; Y. Petrov; L. J. Pickard; E. S. Pinzon Guerra; C. Pistillo; P. Plonski; E. Poplawska; B. Popov; M. Posiadala; J. -M. Poutissou; R. Poutissou; P. Przewlocki; B. Quilain; E. Radicioni; P. N. Ratoff; M. Ravonel; M. A. M. Rayner; A. Redij; M. Reeves; E. Reinherz-Aronis; F. Retiere; A. Robert; P. A. Rodrigues; P. Rojas; E. Rondio; S. Roth; A. Rubbia; D. Ruterbories; R. Sacco; K. Sakashita; F. Sánchez; F. Sato; E. Scantamburlo; K. Scholberg; J. Schwehr; M. Scott; Y. Seiya; T. Sekiguchi; H. Sekiya; D. Sgalaberna; M. Shiozawa; S. Short; Y. Shustrov; P. Sinclair; B. Smith; R. J. Smith; M. Smy; J. T. Sobczyk; H. Sobel; M. Sorel; L. Southwell; P. Stamoulis; J. Steinmann; B. Still; Y. Suda; A. Suzuki; K. Suzuki; S. Y. Suzuki; Y. Suzuki; T. Szeglowski; R. Tacik; M. Tada; S. Takahashi; A. Takeda; Y. Takeuchi; H. K. Tanaka; H. A. Tanaka; M. M. Tanaka; D. Terhorst; R. Terri; L. F. Thompson; A. Thorley; S. Tobayama; W. Toki; T. Tomura; Y. Totsuka; C. Touramanis; T. Tsukamoto; M. Tzanov; Y. Uchida; K. Ueno; A. Vacheret; M. Vagins; G. Vasseur; T. Wachala; A. V. Waldron; C. W. Walter; D. Wark; M. O. Wascko; A. Weber; R. Wendell; R. J. Wilkes; M. J. Wilking; C. Wilkinson; Z. Williamson; J. R. Wilson; R. J. Wilson; T. Wongjirad; Y. Yamada; K. Yamamoto; C. Yanagisawa; S. Yen; N. Yershov; M. Yokoyama; T. Yuan; A. Zalewska; J. Zalipska; L. Zambelli; K. Zaremba; M. Ziembicki; E. D. Zimmerman; M. Zito; J. ?muda; for the T2K collaboration

2014-04-16

405

Neutrino properties and fundamental symmetries  

SciTech Connect

This is the final report of a three-year, Laboratory-Directed Research and Development (LDRD) project at the Los Alamos National Laboratory (LANL). There are two components to this work. The first is a development of a new detection scheme for neutrinos. The observed deficit of neutrinos from the Sun may be due to either a lack of understanding of physical processes in the Sun or may be due to neutrinos oscillating from one type to another during their transit from the Sun to the Earth. The Sudbury Neutrino Observatory (SNO) is designed to use a water Cerenkov detector employing one thousand tonnes of heavy water to resolve this question. The ability to distinguish muon and tau neutrinos from electron neutrinos is crucial in order to carry out a model-independent test of neutrino oscillations. We describe a developmental exploration of a novel technique to do this using {sup 3}He proportional counters. Such a method offers considerable advantages over the initially proposed method of using Cerenkov light from capture on NaCl in the SNO. The second component of this work is an exploration of optimal detector geometry for a time-reversal invariance experiment. The question of why time moves only in the forward direction is one of the most puzzling problems in modern physics. We know from particle physics measurements of the decay of kaons that there is a charge-parity symmetry that is violated in nature, implying time-reversal invariance violation. Yet, we do not understand the origin of the violation of this symmetry. To promote such an understanding, we are developing concepts and prototype apparatus for a new, highly sensitive technique to search for time-reversal-invariance violation in the beta decay of the free neutron. The optimized detector geometry is seven times more sensitive than that in previous experiments. 15 refs.

Bowles, T.J.

1996-07-01

406

Phenomenology of FourthPhenomenology of Fourth Generation NeutrinosGeneration Neutrinos  

E-print Network

Phenomenology of FourthPhenomenology of Fourth Generation NeutrinosGeneration Neutrinos LindaVGeV mdmd>268>268 GeVGeV LEP neutrinos 101, 102, 90LEP neutrinos 101, 102, 90 GeVGeV in e mu tau channel for Dirac neutrinosin e mu tau channel for Dirac neutrinos 90.7, 89.5, 80.590.7, 89.5, 80.5 GeVGeV forfor

California at Santa Cruz, University of

407

Supersymmetric Seesaw without Singlet Neutrinos: Neutrino Masses and Lepton-Flavour Violation  

Microsoft Academic Search

We consider the supersymmetric seesaw mechanism induced by the exchange of\\u000aheavy SU(2)_W triplet states, rather than `right-handed' neutrino singlets, to\\u000agenerate neutrino masses. We show that in this scenario the neutrino flavour\\u000astructure tested at low-energy in the atmospheric and solar neutrino\\u000aexperiments is directly inherited from the neutrino Yukawa couplings to the\\u000atriplets. This allows us to predict

Anna Rossi; G. Galilei

2002-01-01

408

Cosmological implications of a Relic Neutrino Asymmetry  

E-print Network

We consider some consequences of the presence of a cosmological lepton asymmetry in the form of neutrinos. Relic neutrino degeneracy enhances the contribution of massive neutrinos to the present energy density of the Universe, and modifies the power spectrum of radiation and matter. Comparing with current observations of cosmic microwave background anisotropies and large scale structure, we derive some constraints on the neutrino degeneracy and on the spectral index in the case of a flat Universe with a cosmological constant.

Julien Lesgourgues; Sergio Pastor

1999-04-20

409

Have massive cosmological neutrinos already been detected  

NASA Technical Reports Server (NTRS)

The possibility is investigated that the decay of massive cosmological neutrinos may have produced a spectral signature which has already been detected in observations of the ultraviolet background radiation. Various implications are discussed including a possible implied neutrino mass of 13.8-14.8 eV. A lower limit is also placed on the lifetime of heavy neutrinos with respect to decay into light neutrinos and gamma rays based on the cosmic UV observations.

Stecker, F. W.

1980-01-01

410

Evidence for Oscillation of Atmospheric Neutrinos  

Microsoft Academic Search

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

Henry Sobel; T. Hayakawa; E. Ichihara; K. Inoue; K. Ishihara; H. Ishino; Y. Itow; T. Kajita; J. Kameda; S. Kasuga; K. Kobayashi; Y. Kobayashi; Y. Koshio; M. Miura; M. Nakahata; S. Nakayama; A. 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. R. Sulak; C. W. Walter; M. Goldhaber; T. Barszczxak; D. Casper; W. Gajewski; P. G. Halverson; J. Hsu; W. R. Kropp; L. R. Price; F. Reines; M. Smy; M. R. Vagins; K. S. Ganezer; W. E. Keig; R. W. Ellsworth; S. Tasaka; J. W. 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; A. Sakai; M. Sakuda; O. Sasaki; S. Echigo; M. Kohama; A. 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; T. Yamaguchi; M. Yoshida; S. B. Kim; M. Etoh; K. Fujita; A. Hasegawa; T. Hasegawa; S. Hatakeyama; T. Iwamoto; M. Koga; T. Maruyama; H. Ogawa; J. Shirai; F. Tsushima; M. Koshiba; M. Nemoto; K. Nishijima; T. Futagami; Y. Hayato; Y. Kanaya; K. Kaneyuki; Y. Watanabe; D. Kielczewska; R. A. Doyle; J. S. George; A. L. Stachyra; L. L. Wai; R. J. Wilkes; K. K. Young

1998-01-01

411

Sterile neutrinos in the early universe  

SciTech Connect

We discuss the role played by right-handed sterile neutrinos in the early universe. We show how well known {sup 4}He constraint on the number of relativistic degrees of freedom at early times limits the equilibration of the right handed neutrino sea with the background plasma. We discuss how this allows interesting constraints to be placed on neutrino properties. In particular, a new limit on the Dirac mass of the neutrino is presented. 12 refs.

Malaney, R.A. (Lawrence Livermore National Lab., CA (USA)); Fuller, G.M. (California Univ., San Diego, La Jolla, CA (USA). Dept. of Physics)

1990-11-14

412

From Neutrino Factory to Muon Collider  

SciTech Connect

Both Muon Colliders and Neutrino Factories require a muon source capable of producing and capturing {Omicron}(10{sup 21}) muons/year. This paper reviews the similarities and differences between Neutrino Factory and Muon Collider accelerator complexes, the ongoing R&D needed for a Muon Collider that goes beyond Neutrino Factory R&D, and some thoughts about how a Neutrino Factory on the CERN site might eventually be upgraded to a Muon Collider.

Geer, S.; /Fermilab

2010-01-01

413

Instabilities in neutrino-plasma density waves  

E-print Network

One examines the interaction and possible resonances between supernova neutrinos and electron plasma waves. The neutrino phase space distribution and its boundary regions are analyzed in detail. It is shown that the boundary regions are too wide to produce non-linear resonant effects. The growth or damping rates induced by neutrinos are always proportional to the neutrino flux and $G_{{\\rm F}}^{2}$.

Luis Bento

2001-04-08

414

Earth Matter Effect on Democratic Neutrinos  

E-print Network

The neutrino propagation through the Earth is investigated in the framework of the democratic neutrino theory. In this theory the neutrino mixing angle theta-1-3 is approximately determined, which allows one to make a well defined neutrino oscillogram driven by the 1-3 mixing in the matter of the Earth. Significant differences in this oscillogram from the case of models with relatively small theta-1-3 are discussed.

Dmitry Zhuridov

2014-07-19

415

Neutrino magnetic moment in a magnetized plasma  

E-print Network

The contribution of a magnetized plasma to the neutrino magnetic moment is calculated. It is shown that only part of the additional neutrino energy in magnetized plasma connecting with its spin and magnetic field strength defines the neutrino magnetic moment. It is found that the presence of magnetized plasma does not lead to the considerable increase of the neutrino magnetic moment in contrast to the results presented in literature previously.

N. V. Mikheev; E. N. Narynskaya

2010-11-08

416

Results from Atmospheric Neutrinos J. G. Learned  

E-print Network

Results from Atmospheric Neutrinos J. G. Learned Department of Physics and Astronomy, University of Hawaii Honolulu, HI 96822 USA Abstract. With the announcement of new evidence for muon neutrino disappearance observed by the Super­ Kamiokande experiment, the more than a decade old atmospheric neutrino

Learned, John

417

The enigmatic neutrinos Syed Afsar Abbas  

E-print Network

The enigmatic neutrinos Syed Afsar Abbas Department of Physics Aligarh Muslim University, Aligarh di#erently for the neutrinos. Their corpuscular character demands that they have zero inertial mass it is a clear prediction of our model that neutrinos, in a pure oscillation mode, travel with velocites greater

418

Neutrinos and Non-proliferation in Europe  

E-print Network

Triggered by the demand of the IAEA, neutrino physicists in Europe involved with the Double Chooz experiment are studying the potential of neutrino detection to monitor nuclear reactors. In particular a new set of experiments at the ILL is planned to improve the knowledge of the neutrino spectrum emitted in the fission of 235U and 239Pu.

M. Cribier

2007-04-04

419

Chimie et Neutrinos Alain de Bellefon(1)  

E-print Network

Chimie et Neutrinos Alain de Bellefon(1) , Michel Cribier(1) et Jean-Claude Mialocq(2) Résumé Cet article illustre la synergie qui existe entre la chimie et la détection des neutrinos, ces particules'énigme des neutrinos solaires fut rendue possible entre autres par l'obtention d'une extrême pureté

Boyer, Edmond

420

Improved Theory of Neutrino Oscillations in Matter  

E-print Network

This is revision of the S-Matrix theory of neutrino oscillations used for many years. We evaluate the transition probability of a $\\mu$ to $e$ neutrino without an approximation used for many theoretical studies, and find important differences which could improve the extraction of neutrino parameters from experimental data in the future.

Leonard S. Kisslinger

2014-11-19

421

Neutrino oscillations at CERN-Pyhäsalmi baseline  

NASA Astrophysics Data System (ADS)

A neutrino factory at CERN could send a neutrino beam to the underground laboratory in the Pyhäsalmi mine in Finland. The 2288 km long baseline gives good physics reach, with a possibility to study mass hierarchy. We consider also other neutrino beams. The distance from JPARC, 7090 km, is interestingly close to magic baseline.

Peltoniemi, J. T.; Sarkamo, J.

2006-05-01

422

Recent Development on Collective Neutrino Interactions  

E-print Network

Quantum Field Theory is applied to study an electron plasma under an intense neutrino flux. The dispersion relation of the longitudinal waves is derived and the damping rate is calculated. It is shown that in the case of Supernova emission the neutrinos are not collimated enough to cause plasma instabilities associated to a strong neutrino resonance effect.

Luis Bento

1999-12-29

423

Short-BaseLine Electron Neutrino Disappearance  

NASA Astrophysics Data System (ADS)

We analyzed the electron neutrino data of the Gallium radioactive source experiments and the electron antineutrino data of the reactor Bugey and Chooz experiments in terms of neutrino oscillations. We found a hint of a CPT-violating asymmetry of the effective neutrino and antineutrino mixing angles.

Giunti, Carlo; Laveder, Marco

2011-08-01

424

ANTARES: The first undersea neutrino telescope  

Microsoft Academic Search

The ANTARES Neutrino Telescope was completed in May 2008 and is the first operational Neutrino Telescope in the Mediterranean Sea. The main purpose of the detector is to perform neutrino astronomy and the apparatus also offers facilities for marine and Earth sciences. This paper describes the design, the construction and the installation of the telescope in the deep sea, offshore

M. Ageron; J. A. Aguilar; I. Al Samarai; A. Albert; F. Ameli; M. André; M. Anghinolfi; G. Anton; S. Anvar; M. Ardid; K. Arnaud; E. Aslanides; A. C. Assis Jesus; T. Astraatmadja; J.-J. Aubert; R. Auer; E. Barbarito; B. Baret; S. Basa; M. Bazzotti; Y. Becherini; J. Beltramelli; A. Bersani; V. Bertin; S. Beurthey; S. Biagi; C. Bigongiari; M. Billault; R. Blaes; C. Bogazzi; N. de Botton; M. Bou-Cabo; B. Boudahef; M. C. Bouwhuis; A. M. Brown; J. Brunner; J. Busto; L. Caillat; A. Calzas; F. Camarena; A. Capone; L. Caponetto; C. Cârloganu; G. Carminati; E. Carmona; J. Carr; P. H. Carton; B. Cassano; E. Castorina; S. Cecchini; A. Ceres; Th. Chaleil; Ph. Charvis; P. Chauchot; T. Chiarusi; M. Circella; C. Compère; R. Coniglione; X. Coppolani; A. Cosquer; H. Costantini; N. Cottini; P. Coyle; S. Cuneo; C. Curtil; C. D'Amato; G. Damy; R. van Dantzig; G. De Bonis; G. Decock; M. P. Decowski; I. Dekeyser; E. Delagnes; F. Desages-Ardellier; A. Deschamps; J.-J. Destelle; F. Di Maria; B. Dinkespiler; C. Distefano; J.-L. Dominique; C. Donzaud; D. Dornic; Q. Dorosti; J.-F. Drogou; D. Drouhin; F. Druillole; D. Durand; R. Durand; T. Eberl; U. Emanuele; J. J. Engelen; J.-P. Ernenwein; S. Escoffier; E. Falchini; S. Favard; F. Fehr; F. Feinstein; M. Ferri; S. Ferry; C. Fiorello; V. Flaminio; F. Folger; U. Fritsch; J.-L. Fuda; S. Galatá; S. Galeotti; P. Gay; F. Gensolen; G. Giacomelli; C. Gojak; J. P. Gómez-González; Ph. Goret; K. Graf; G. Guillard; G. Halladjian; G. Hallewell; H. van Haren; B. Hartmann; A. J. Heijboer; E. Heine; Y. Hello; S. Henry; J. J. Hernández-Rey; B. Herold; J. Hößl; J. Hogenbirk; C. C. Hsu; J. R. Hubbard; M. Jaquet; M. Jaspers; M. de Jong; D. Jourde; M. Kadler; N. Kalantar-Nayestanaki; O. Kalekin; A. Kappes; T. Karg; S. Karkar; M. Karolak; U. Katz; P. Keller; P. Kestener; E. Kok; H. Kok; P. Kooijman; C. Kopper; A. Kouchner; W. Kretschmer; A. Kruijer; S. Kuch; V. Kulikovskiy; D. Lachartre; H. Lafoux; P. Lagier; R. Lahmann; C. Lahonde-Hamdoun; P. Lamare; G. Lambard; J.-C. Languillat; G. Larosa; J. Lavalle; Y. Le Guen; H. Le Provost; A. Levansuu; D. Lefèvre; T. Legou; G. Lelaizant; C. Lévéque; G. Lim; D. Lo Presti; H. Loehner; S. Loucatos; F. Louis; F. Lucarelli; V. Lyashuk; P. Magnier; S. Mangano; A. Marcel; M. Marcelin; A. Margiotta; J. A. Martinez-Mora; R. Masullo; F. Mazéas; A. Mazure; A. Meli; M. Melissas; E. Migneco; M. Mongelli; T. Montaruli; M. Morganti; L. Moscoso; H. Motz; M. Musumeci; C. Naumann; M. Naumann-Godo; M. Neff; V. Niess; G. J. L. Nooren; J. E. J. Oberski; C. Olivetto; N. Palanque-Delabrouille; D. Palioselitis; R. Papaleo; G. E. P?v?la?; K. Payet; P. Payre; H. Peek; J. Petrovic; P. Piattelli; N. Picot-Clemente; C. Picq; Y. Piret; J. Poinsignon; V. Popa; T. Pradier; E. Presani; G. Prono; C. Racca; G. Raia; J. van Randwijk; D. Real; C. Reed; F. Réthoré; P. Rewiersma; G. Riccobene; C. Richardt; R. Richter; J. S. Ricol; V. Rigaud; V. Roca; K. Roensch; J.-F. Rolin; A. Rostovtsev; A. Rottura; J. Roux; M. Rujoiu; M. Ruppi; G. V. Russo; F. Salesa; K. Salomon; P. Sapienza; F. Schmitt; F. Schöck; J.-P. Schuller; F. Schüssler; D. Sciliberto; R. Shanidze; E. Shirokov; F. Simeone; A. Sottoriva; A. Spies; T. Spona; M. Spurio; J. J. M. Steijger; Th. Stolarczyk; K. Streeb; L. Sulak; M. Taiuti; C. Tamburini; C. Tao; L. Tasca; G. Terreni; D. Tezier; S. Toscano; F. Urbano; P. Valdy; B. Vallage; V. van Elewyck; G. Vannoni; M. Vecchi; G. Venekamp; B. Verlaat; P. Vernin; E. Virique; G. de Vries; R. van Wijk; G. Wijnker; G. Wobbe; E. de Wolf; Y. Yakovenko; H. Yepes; D. Zaborov; H. Zaccone; J. D. Zornoza; J. Zúñiga

2011-01-01

425

Neutrino oscillations and consequences for coupling constants ?i33 (?) of the R?-Minimal Supersymmetric Standard Model  

NASA Astrophysics Data System (ADS)

In this article we discuss the different kinds of experiments which can be explained in terms of neutrino oscillations. As a consequence of this neutrinos have to massive. But the oscillation data cannot fix the ? mass matrix totally. By considering the neutrino as a Majorana particle and useing the information obtained the by search for 0???, we extracted upper limits on the elements of the ? mass matrix by using the upper limit of the averaged Majorana neutrino mass. To describe now massive neutrinos we considered the R? -MSSM. We constructed a mass matrix within this model where all three neutrinos can be massive. By comparing the so found theoretical mass matrix with the extracted phenomenological bounds we extracted stringent limits on the trilinear coupling constants ?i33 ?). By imposing an additional horizontal U(1) X flavor symmetry we were able to reduce the number of parameters in out model drastically. We could by comparing the theoretical and phenomenological mass matrix determine the scale on the phenomenological side and the remaining coupling constants on the theoretical side. This leads to a unique scenario for the neutrino masses within this framework. The averaged Majorana neutrino mass in this model was found to be ? 0.01-0.4 eV. This region will be explored in the near future by 0??? experiments (e.g. the GENIUS experiment).

Haug, O.; Vergados, J. D.; Faessler, A.; Kovalenko, S.; Vergados, J. D.; Kovalenko, S.

426

Neutrino mass hierarchy and octant determination with atmospheric neutrinos.  

PubMed

The recent discovery by the Daya-Bay and RENO experiments, that ?(13) is nonzero and relatively large, significantly impacts existing experiments and the planning of future facilities. In many scenarios, the nonzero value of ?(13) implies that ?(23) is likely to be different from ?/4. Additionally, large detectors will be sensitive to matter effects on the oscillations of atmospheric neutrinos, making it possible to determine the neutrino mass hierarchy and the octant of ?(23). We show that a 50 kT magnetized liquid argon neutrino detector can ascertain the mass hierarchy with a significance larger than 4? with moderate exposure times, and the octant at the level of 2-3? with greater exposure. PMID:23002822

Barger, Vernon; Gandhi, Raj; Ghoshal, Pomita; Goswami, Srubabati; Marfatia, Danny; Prakash, Suprabh; Raut, Sushant K; Sankar, S Uma

2012-08-31

427

Muon neutrino disappearance at MINOS  

SciTech Connect

A strong case has been made by several experiments that neutrinos oscillate, although important questions remain as to the mechanisms and precise values of the parameters. In the standard picture, two parameters describe the nature of how the neutrinos oscillate: the mass-squared difference between states and the mixing angle. The purpose of this thesis is to use data from the MINOS experiment to precisely measure the parameters associated with oscillations first observed in studies of atmospheric neutrinos. MINOS utilizes two similar detectors to observe the oscillatory nature of neutrinos. The Near Detector, located 1 km from the source, observes the unoscillated energy spectrum while the Far Detector, located 735 km away, is positioned to see the oscillation signal. Using the data in the Near Detector, a prediction of the expected neutrino spectrum at the Far Detector assuming no oscillations is made. By comparing this prediction with the MINOS data, the atmospheric mixing parameters are measured to be {Delta}m{sub 32}{sup 2} = 2.45{sub +0.12}{sup -0.12} x 10{sub -3} eV{sup 2} and sin{sup 2}(2{theta}{sub 32}) = 1.00{sub -0.04}{sup +0.00} (> 0.90 at 90% confidence level).

Armstrong, R.; /Indiana U.

2009-08-01

428

Ultrahigh-energy neutrino astronomy  

NASA Technical Reports Server (NTRS)

High-energy cosmic-ray interactions can produce neutrinos. The neutrino fluxes are calculated over a range of energies. The sources considered (and their ranges of importance) are cosmic-ray interactions in earth's atmosphere (neutrino energies less than 10,000 GeV), cosmic-ray interactions with ambient hydrogen in galaxies (neutrino energies between 10,000 and 1 million GeV), regions of cosmic-ray acceleration - e.g., pulsars - and cosmic-ray interactions with the microwave background radiation (neutrino energies greater than 100 million GeV). In addition, estimates of the flux from compact sources, such as active galaxies, are made. These flux levels, calculated conservatively, may be high enough for practical detection with a 1-cu km seawater detector; i.e., count rates greater than 1 per day. Such observations would provide information mainly about high-energy physics, but also (over long times) about cosmic-ray spectra, composition, and acceleration, as well as supernova and galactic-nucleus explosions.

Margolis, S. H.; Schramm, D. N.; Silberberg, R.

1978-01-01

429

Black holes at neutrino telescopes  

NASA Astrophysics Data System (ADS)

In scenarios with extra dimensions and TeV-scale quantum gravity, black holes are expected to be produced in the collision of light particles at center-of-mass energies above the fundamental Planck scale with small impact parameters. Black hole production and evaporation may thus be studied in detail at the Large Hadron Collider (LHC). But even before the LHC starts operating, neutrino telescopes such as AMANDA/IceCube, ANTARES, Baikal, and RICE have an opportunity to search for black hole signatures. Black hole production in the scattering of ultrahigh energy cosmic neutrinos on nucleons in the ice or water may initiate cascades and through-going muons with distinct characteristics above the Standard Model rate. In this Letter, we investigate the sensitivity of neutrino telescopes to black hole production and compare it to the one expected at the Pierre Auger Observatory, an air shower array currently under construction, and at the LHC. We find that, already with the currently available data, AMANDA and RICE should be able to place sensible constraints in black hole production parameter space, which are competitive with the present ones from the air shower facilities Fly's Eye and AGASA. In the optimistic case that a ultrahigh energy cosmic neutrino flux significantly higher than the one expected from cosmic ray interactions with the cosmic microwave background radiation is realized in nature, one even has discovery potential for black holes at neutrino telescopes beyond the reach of LHC.

Kowalski, M.; Ringwald, A.; Tu, H.

2002-03-01

430

GRB neutrino search with MAGIC  

SciTech Connect

The Major Atmospheric Gamma Imaging Cherenkov (MAGIC) telescope was designed for the detection of photon sources > or approx. 50 GeV. The measurement of highly-inclined air showers renders possible the search for high-energy neutrinos, too. Only neutrinos can traverse the Earth without interaction, and therefore, events close to the horizon can be identified as neutrino-induced rather than photon-induced or hadronic events. In this paper, Swift-XRT-detected GRBs with given spectral information are used in order to calculate the potential neutrino energy spectrum from prompt and afterglow emission for each individual GRB. The event rate in MAGIC is estimated assuming that the GRB happens within the field of view of MAGIC. A sample of 568 long GRBs as detected by BATSE is used to compare the detection rates with 163 Swift-detected bursts. BATSE has properties similar to the Gamma-ray Burst Monitor (GBM) on board of GLAST. Therefore the estimated rates give an estimate for the possibilities of neutrino detection with MAGIC from GLAST-triggered bursts.

Becker, Julia K.; Rhode, Wolfgang [Institut fuer Physik, TU Dortmund, 44221 Dortmund (Germany); Gaug, Markus [Instituto de Astrofisica de Canarias, C/Via Lactea s/n La Laguna, Tenerife (Spain); Hsu, C.-C. [Max-Planck-Institut fuer Physik, Foehringer Ring 6, Muenchen (Germany)

2008-05-22

431

Tracing very high energy neutrinos from cosmological distances in ice  

NASA Astrophysics Data System (ADS)

Astrophysical sources of ultrahigh energy neutrinos yield tau neutrino fluxes due to neutrino oscillations. We study in detail the contribution of tau neutrinos with energies above 106 GeV relative to the contribution of the other flavors. We consider several different initial neutrino fluxes and include tau neutrino regeneration in transit through the Earth and the energy loss of charged leptons. We discuss the signals of tau neutrinos in detectors such as IceCube, RICE, and ANITA.

Jones, J.; Mocioiu, I.; Reno, M. H.; Sarcevic, I.

2004-02-01

432

Expectation values of flavor-neutrino numbers with respect to neutrino-source hadron states --Neutrino oscillations and decay probabilities--  

E-print Network

On the basis of quantum field theory, we consider a unified description of various processes accompanied by neutrinos, namely weak decays and oscillation processes. The structures of the expectation values of flavor-neutrino numbers with respect to neutrino-source hadron state are investigated. Due to the smallness of neutrino masses, we naturally obtain the old (i.e. pre-mixing) formulas of decay probabilities. Together, it is shown that the oscillation formulas, similar to the usual ones, are applied irrespectively of the details of neutrino-producing processes. The derived oscillation formulas are the same in form as the usually used ones except for the oscillation length.

Kanji Fujii; Norihito Toyota

2014-08-09

433

A three-loop radiative neutrino mass model with dark matter  

E-print Network

We present a model that generates small neutrino masses at three-loop level due to the existence of Majorana fermionic dark matter, which is stabilized by a Z2 symmetry. The model predicts that the lightest neutrino is massless. We show a prototypical parameter choice allowed by relevant experimental data, which favors the case of normal neutrino mass spectrum and the dark matter with m \\sim 50-135 GeV and a sizable Yukawa coupling. It means that new particles can be searched for in future e+e- collisions.

Jin, Li-Gang; Zhang, Fei

2015-01-01

434

On the SUSY accompanied neutrino exchange mechanism of neutrinoless double beta decay  

NASA Astrophysics Data System (ADS)

The neutrinoless double beta decay (0???) induced by light Majorana neutrino exchange between decaying nucleons, accompanied by the squark exchange inside one nucleon, recently discussed by Babu and Mohapatra, is carefully analyzed both from the particle and nuclear physics sides. New nuclear matrix elements relevant to this mechanism are calculated. We extend the analysis to include mixing of light neutrinos with heavy and “sterile” neutrinos. It introduces another supersymmtric (SUSY) contribution to 0???. We discuss constraints on the RpMSSM parameters imposed by the current experimental limit on 0??? decay half-life of 76Ge.

Hirsch, M.; Klapdor-Kleingrothaus, H. V.; Kovalenko, S. G.

1996-02-01

435

Supernova neutrinos and nucleosynthesis  

E-print Network

Observations of metal-poor stars indicate that at least two different nucleosynthesis sites contribute to the production of r-process elements. One site is responsible for the production of light r-process elements Znucleosynthesis calculations based on long term Boltzmann neutrino transport simulations. They are based on an Equation of State that reproduces recent constrains on the nuclear symmetry energy. We predict that the early ejecta is neutron-rich with Ye ~ 0.48, it becomes proton rich around 4 s and reaches Ye = 0.586 at 9 s when our simulation stops. The nucleosynthesis in this model produces elements between Zn and Mo, including 92Mo. The elemental abundances are consistent with the observations of the metal-poor star HD 12263. For the elements between Ge and Mo, we produce mainly the neutron-deficient isotopes. This prediction can be confirmed by observations of isotopic abundances in metal-poor stars. No elements heavier than Mo (Z=42) and no heavy r-process elements are produced in our calculations.

G. Martínez-Pinedo; T. Fischer; L. Huther

2013-09-21

436

Measurable neutrino mass scale in A{sub 4}xSU(5)  

SciTech Connect

We propose a supersymmetric A{sub 4}xSU(5) model of quasidegenerate neutrinos which predicts the effective neutrino mass m{sub ee} relevant for neutrinoless double beta decay to be proportional to the neutrino mass scale, thereby allowing its determination approximately independently of unknown Majorana phases. Such a natural quasidegeneracy is achieved by using A{sub 4} family symmetry (as an example of a non-Abelian family symmetry with real triplet representations) to enforce a contribution to the neutrino mass matrix proportional to the identity. Tribimaximal neutrino mixing as well as quark CP violation with {alpha}{approx_equal}90 deg. d a leptonic CP phase {delta}{sub MNS{approx_equal}}90 deg. arise from the breaking of the A{sub 4} family symmetry by the vacuum expectation values of four 'flavon' fields pointing in specific postulated directions in flavor space.

Antusch, S.; Spinrath, M. [Max-Planck-Institut fuer Physik (Werner-Heisenberg-Institut), Foehringer Ring 6, D-80805 Muenchen (Germany); King, Stephen F. [School of Physics and Astronomy, University of Southampton, SO17 1BJ Southampton (United Kingdom)

2011-01-01

437

See-saw Enhancement of Neutrino Mixing due to the Right-handed Phases  

E-print Network

We study the see-saw enhancement mechanism in presence of the right-handed phases of the Dirac neutrino mass matrix and the Majorana mass matrix. The enhancement condition given by Smirnov is modified. We point out that the see-saw enhancement could be obtained due to the right-handed phases even if the Majorana matrix is proportional to the unit matrix. We show a realistic Dirac mass matrix which causes the see-saw enhancement.

Morimitsu Tanimoto

1995-03-14

438

An Axial Vector Nature of a Neutrino with an Electroweak Mass  

E-print Network

A classification of elementary particles with respect to C-operation admits the existence of truly neutral types of fermions. Among them one can find both a Dirac and a Majorana neutrinos of an electroweak nature. Their mass includes the electric and weak parts, in the presence of which a neutrino has the anapole charge, charge radius and electric dipole moment. They constitute the paraneutrino of true neutrality, for example, at the neutrino interaction with a spinless nucleus of an axial-vector current. We derive the united equations which relate the structural components of mass to anapole, charge radius and electric dipole of each truly neutral neutrino at the level of flavour symmetry. Such a principle can explain the C-noninvariant nature of neutrinos and fields in the framework of constancy law of the size implied from the multiplication of a weak mass of the C-odd neutrino by its electric mass. From this point of view, all neutrinos of C-antisymmetricality regardless of the difference in masses of an axial-vector character, possess the same anapole with his radius as well as the identical electric dipole. Their analysis together with earlier measurements of an electric dipole moment of neutrino gives the right to accept not only the existence of truly neutral types of Dirac neutrinos and fields but also the availability of mass structure in them as the one of experimentally established facts.

Rasulkhozha S. Sharafiddinov

2011-11-09

439

Spin flip of neutrinos with magnetic moment in core-collapse supernova  

SciTech Connect

Neutrinos with magnetic moment experience chirality flips while scattering off charged particles. It is known that if neutrino is a Dirac fermion, then such chirality flips lead to the production of sterile right-handed neutrinos inside the core of a star during the stellar collapse, which may facilitate the supernova explosion and modify the supernova neutrino signal. In the present paper we reexamine the production of right-handed neutrinos during the collapse using a dynamical model of the collapse. We refine the estimates of the values of the Dirac magnetic moment which are necessary to substantially alter the supernova dynamics and neutrno signal. It is argued in particular that Super-Kamiokande will be sensitive at least to {mu}{sub {nu}Dirac} = 10{sup -13{mu}}{sub B} in case of a galactic supernova explosion. Also we briefly discuss the case of Majorana neutrino magnetic moment. It is pointed out that in the inner supernova core spin flips may quickly equilibrate electron neutrinos with nonelectron antineutrinos if {mu}{sub {nu}Majorana} {>=} 10{sup -12{mu}}{sub B}. This may lead to various consequences for supernova physics.

Lychkovskiy, O. V., E-mail: lychkovskiy@itep.ru; Blinnikov, S. I. [Institute for Theoretical and Experimental Physics (Russian Federation)

2010-04-15

440

Decaying neutrinos in galaxy clusters  

NASA Technical Reports Server (NTRS)

Davidsen et al. (1991) have argued that the failure to detect UV photons from the dark matter (DM) in cluster A665 excludes the decaying neutrino hypothesis. Sciama et al. (1993) argued that because of high central concentration the DM in that cluster must be baryonic. We study the DM profile in clusters of galaxies simulated using the Harrison-Zel'dovich spectrum of density fluctuations, and an amplitude previously derived from numerical simulations (Melott 1984b; Anninos et al. 1991) and in agreement with microwave background fluctuations (Smoot et al. 1992). We find that with this amplitude normalization cluster neutrino DM densities are comparable to observed cluster DM values. We conclude that given this normalization, the cluster DM should be at least largely composed of neutrinos. The constraint of Davidsen et al. can be somewhat weakened by the presence of baryonic DM; but it cannot be eliminated given our assumptions.

Melott, Adrian L.; Splinter, Randall J.; Persic, Massimo; Salucci, Paolo

1994-01-01

441

Decaying neutrinos in galaxy clusters  

NASA Technical Reports Server (NTRS)

The DM profile in clusters of galaxies was studied and simulated using the Harrison-Zel'dovich spectrum of density fluctuations, and an amplitude previously derived from numerical simulations and in agreement with microwave background fluctuations. Neutrino DM densities, with this amplitude normalization cluster, are comparable to observed cluster DM values. It was concluded that given this normalization, the cluster DM should be al least largely composed of neutrinos. The constraint of Davidson et al., who argued that the failure to detect uv photons from the dark matter (DM) in cluster A665 excludes the decaying neutrino hypothesis, could be somewhat weakened by the presence of baryonic DM; but it cannot be eliminated given our assumptions.

Melott, Adrian L.; Splinter, Randall J.; Persic, Massimo; Salucci, Paolo

1993-01-01

442

Recent developments in neutrino physics  

SciTech Connect

I shall attempt to summarize recent developments in the experimental situation in neutrino physics. The paper will deal with recent results, drawing on either published work or research that has been presented in preprint form, as there is an adequate supply of interesting and controversial data restricting oneself to these generally more reliable sources. The discussion of the theoretical implication of these experimental results will be presented in the following paper by Boris Kayser. The topics to be covered in this presentation are: direct measurements of {bar {nu}}{sub e} mass via beta endpoint studies; status of solar neutrino observations; status of 17-keV neutrino'' reports; and the use of {nu}p elastic scattering to determine the strange quark'' content of the proton. 2 refs., 15 figs., 9 tabs.

Garvey, G.T.

1991-01-01

443

Stimulated neutrino transformation through turbulence  

NASA Astrophysics Data System (ADS)

We derive an analytical solution for the flavor evolution of a neutrino through a turbulent density profile which is found to accurately predict the amplitude and transition wavelength of numerical solutions on a case-by-case basis. The evolution is seen to strongly depend upon those Fourier modes in the turbulence which are approximately the same as the splitting between neutrino eigenvalues. Transitions are strongly enhanced by those Fourier modes in the turbulence which are approximately the same as the splitting between neutrino eigenvalues. We also find a suppression of transitions due to the long wavelength modes when the ratio of their amplitude and the wave number is of order, or greater than, the first root of the Bessel function J0.

Patton, Kelly M.; Kneller, James P.; McLaughlin, Gail C.

2014-04-01

444

Observation of the Tau Neutrino  

NASA Astrophysics Data System (ADS)

The neutrino was the last standard-model fermion to be directly observed. We report on the strategy, design, and results of the DONuT experiment. The data were acquired at Fermilab during 1997, and in July 2000, the DONuT collaboration presented four -neutrino interactions. Modern nuclear-emulsion processing was the key technology that made it possible to detect the decay of leptons produced in charged-current interactions of neutrinos. The precision of the emulsion data and the speed of digitization enabled the use of novel methods to locate interaction vertices and search for decays in emulsion data. We also discuss the level of background in the signal, which is small enough to permit the identification of individual events with high confidence.

Lundberg, B.; Niwa, K.; Paolone, V.

2003-12-01

445

Magnetic Moment of Neutrino in Statistical Background  

E-print Network

We calculate the magnetic moment of Dirac type of neutrinos in hot and dense background for different ranges of temperature and chemical potential. The properties of neutrinos are studied in the strong magnetic field where the chemical potential of particles is high enough to have more particles than the antiparticles. We show that in this situation, Weyl neutrino seems to explain the neutrino coupling with the magnetic field due to its effective mass which can couple with the magnetic field directly. We also investigate the electromagnetic properties of Weyl neutrino due to its effective mass developed in the strong magnetic field.

Samina S. Masood

2012-03-11

446

Dark Energy and Neutrino CPT Violation  

E-print Network

In this paper we study the dynamical CPT violation in the neutrino sector induced by the dark energy of the Universe. Specifically we consider a dark energy model where the dark energy scalar derivatively interacts with the right-handed neutrinos. This type of derivative coupling leads to a cosmological CPT violation during the evolution of the background field of the dark energy. We calculate the induced CPT violation of left-handed neutrinos and find the CPT violation produced in this way is consistent with the present experimental limit and sensitive to the future neutrino oscillation experiments, such as the neutrino factory.

Pei-Hong Gu; Xiao-Jun Bi; Xinmin Zhang

2005-11-03

447

Investigating CPT Conservation in Sterile Neutrino Fits  

NASA Astrophysics Data System (ADS)

We investigate compatibility between neutrino and antineutrino short-baseline oscillation experiments under a two-neutrino oscillation hypothesis due to a sterile neutrino at ?m^2˜1 eV^2. We explore the preliminary MINOS antineutrino disappearance results as well as antineutrino oscillation results from LSND, MiniBooNE, KARMEN, Bugey, and Chooz, and neutrino oscillation results from NOMAD, MiniBooNE, CCFR84, and CDHS. We find that a combined fit of the antineutrino data yields a high chi-squared probability, while the global fit including neutrino and antineutrino data yields high incompatibility. CPT-violating fits within this scenario are also explored. )

Ignarra, Christina

2010-02-01

448

New astrophysical limit on neutrino millicharge  

E-print Network

An impact of a nonzero neutrino millicharge in astrophysics is tested. It is shown that in astrophysical environments electromagnetic interactions of the neutrino millicharge with strong electromagnetic fields as well as weak interactions of the neutrinos with dense background matter can produce new phenomena accessible for astrophysical observations. On this basis a new limit on the neutrino millicharge $q_0<1.3\\times10^{-19}e_0$ is obtained. This limit is among the strongest astrophysical constraint on the neutrino millicharge. Some other possible applications of the obtained results to astrophysics are discussed in details.

Alexander I. Studenikin; Ilya V. Tokarev

2014-11-09

449

Neutrino oscillations in the early universe  

NASA Astrophysics Data System (ADS)

Numerical studies are performed for neutrino oscillations for t > 1/3 seconds after the big bang. The effects of electron, positron and neutrino backgrounds are properly included. Flavor evolution of the neutrino background is dominantly smooth. However, in a certain parameter region, coherent undamped oscillations of the neutrino background are possible. In addition, neutrino CP asymmetry is found to be considerably smaller than expected. Reasons are provided for the above effects and some physical implications are discussed. On leave of absence from the City College of New York.

Kostelecký, V. Alan; Pantaleone, J.; Samuel, Stuart

1993-09-01

450

Tau neutrino propagation and tau energy loss  

NASA Astrophysics Data System (ADS)

Electromagnetic energy loss of tau leptons is an important ingredient for eventual tau neutrino detection from high energy astrophysical sources. Proposals have been made to use mountains as neutrino converters, in which the emerging tau decays in an air shower. We use a stochastic evaluation of both tau neutrino conversion to taus and of tau electromagnetic energy loss. We examine the effects of the propagation for monoenergetic incident tau neutrinos as well as for several neutrino power-law spectra. Our main result is a parameterization of the tau electromagnetic energy loss parameter ?. We compare the results from the analytic expression for the tau flux using this ? with other parameterizations of ?.

Dutta, Sharada Iyer; Huang, Yiwen; Reno, Mary Hall

2005-07-01

451

The diffuse supernova neutrino flux  

E-print Network

I review the status and perspectives of the research on the diffuse flux of (core collapse) supernova neutrinos (DF). In absence of a positive signal, several upper bounds exist in different detection channels. Of these, the strongest is the limit from SuperKamiokande (SK) of 1.2 electron antineutrinos cm^-2 s^-1 at 90% confidence level above 19.3 MeV of neutrino energy. The predictions of the DF depend on the cosmological rate of supernovae and on the neutrino emission in a individual supernova (spectrum, luminosity,..). Above the SK threshold, they range between 0.05 electron antineutrinos cm^-2 s^-1 up to touching the SK limit. The SK upper bound constrains part of the parameter space of the supernova rate - and indirectly of the star formation rate - only in models with relatively hard neutrino spectra, while predictions with softer spectra would need bounds stronger by about a factor of 4 to be tested. Experimentally, a feasible and very important goal for the future is the improvement of background discrimination and the resulting lowering of the detection threshold. Theory instead will benefit from reducing the uncertainties on the supernova neutrino emission (either with more precise numerical modeling or with data from a galactic supernova) and on the supernova rate. The latter will be provided precisely by next generation supernova surveys up to a normalization factor. Therefore, the detection of the DF is likely to be precious chiefly to constrain such normalization and to study the physics of neutrino emission in supernovae.

Cecilia Lunardini

2006-10-17

452

Non-Zero Electric Charge of the Neutrino and the Solar Neutrino Problem  

E-print Network

It has recently been shown that the neutrino can have non-zero electric charge in a number of gauge theories, including the Minimal Standard Model. Assuming non-zero neutrino charge, we develop a new approach to the solar neutrino problem. The key idea is that the charged neutrinos will be deflected by the Lorentz force while they are crossing the solar magnetic fields. Such a deflection will result in the anisotropy of the solar neutrino flux. Because of this anisotropy, the solar neutrino flux registered on earth can be reduced as compared to the Standard Solar Model prediction. The mechanism is purely classical and does not require neutrino oscillations, spin-flip or neutrino decay. We discuss qualitatively the consequences of our scenario for present and future solar neutrino experiments as well as differences between our mechanism and other proposed solutions.

A. Yu. Ignatiev; G. C. Joshi

1994-07-21

453

Neutrino Oscillations: Eighty Years in Review  

NASA Astrophysics Data System (ADS)

In order to discuss neutrino oscillations, it is necessary to have knowledge of the developments in the field spanning the last eighty years. The existence of the neutrino was posited by Wolfgang Pauli in 1930 to account for the mass defect in beta decay, and to this day physicists are still endeavoring to answer fundamental questions about this enigmatic particle. The scope of this thesis includes a historical background of neutrino physics and a discussion of neutrinos and the Standard Model; subsequent to this is a discussion of the Solar Neutrino Problem, which provided the impetus for the proposal of neutrino oscillations. Bolstering the theory of neutrino oscillations (which is developed in the body of this thesis) are neutrino detector experiments and their results; these include the Homestake experiment, SNO, Kamiokande and Super-Kamiokande, MINOS, and Double-Chooz. We also include relevant derivations, most particularly of the quantum mechanics of neutrino oscillations as treated in the wave packet formalism. We have amassed here the principle theories and experimental results -- a mere tip of the iceberg -- that have brought us to our current understanding of neutrino oscillations. We have also studied the quantum mechanics of neutrino oscillations and developed for ourselves the wave packet formalism describing the phenomenon.

Bowers, Rebecca Lyn

454

Neutrino radiation hazards: A paper tiger  

SciTech Connect

Neutrinos are present in the natural environment due to terrestrial, solar, and cosmic sources and are also produced at accelerators both incidentally and intentionally as part of physics research programs. Progress in fundamental physics research has led to the creation of beams of neutrinos of ever-increasing intensity and/or energy. The large size and cost associated with these beams attracts, and indeed requires, public interest, support, and some understanding of the `exotic` particles produced, including the neutrinos. Furthermore, the very word neutrino (`little neutral one`, as coined by Enrico Fermi) can lead to public concern due to confusion with `neutron`, a word widely associated with radiological hazards. Adding to such possible concerns is a recent assertion, widely publicized, that neutrinos from astronomical events may have led to the extinction of some biological species. Presented here are methods for conservatively estimating the dose equivalent due to neutrinos as well as an assessment of the possible role of neutrinos in biological extinction processes. It is found that neutrinos produced by the sun and modern particle accelerators produce inconsequential dose equivalent rates. Examining recent calculations concerning neutrinos incident upon the earth due to stellar collapse, it is concluded that it is highly unlikely that these neutrinos caused the mass extinctions of species found in the paleontological record. Neutrino radiation hazards are, then, truly a `paper tiger`. 14 refs., 1 fig., 1 tab.

Cossairt, J.D.; Grossman, N.L.; Marshall, E.T.

1996-09-01

455

Probing Neutrino Hierarchy and Chirality via Wakes  

E-print Network

The relic neutrinos are expected to acquire a bulk relative velocity with respect to the dark matter at low redshifts, and downstream of dark matter halos neutrino wakes are expected to develop. We propose a method of measuring the neutrino mass based on this mechanism. The neutrino wake will cause a dipole distortion of the galaxy-galaxy lensing pattern. This effect could be detected by combining upcoming lensing surveys, e.g. the LSST and Euclid surveys with a low redshift galaxy survey or a 21cm intensity mapping survey which can map the neutrino flow field. The data obtained with LSST and Euclid should enable us to make positive detection if the three neutrino masses are Quasi-Degenerate, and a future high precision 21cm lensing survey would allow the normal hierarchy and inverted hierarchy cases to be distinguished, and even the right handed Dirac neutrinos may be detectable.

Hong-Ming Zhu; Ue-Li Pen; Xuelei Chen; Derek Inman

2014-12-04

456

An "archaeological" quest for galactic supernova neutrinos  

E-print Network

We explore the possibility to observe the effects of electron neutrinos from past galactic supernovae, through a geochemical measurement of the amount of Technetium 97 produced by neutrino-induced reactions in a Molybdenum ore. The calculations we present take into account the recent advances in our knowledge of neutrino interactions, of neutrino oscillations inside a supernova, of the solar neutrino flux at Earth and of possible failed supernovae. The predicted Technetium 97 abundance is of the order of 10^7 atoms per 10 kilotons of ore, which is close to the current geochemical experimental sensitivity. Of this, 10-20% is from supernovae. Considering the comparable size of uncertainties, more precision in the modeling of neutrino fluxes as well as of neutrino cross sections is required for a meaningful measurement.

Rimantas Lazauskas; Cecilia Lunardini; Cristina Volpe

2009-01-06

457

End of the cosmic neutrino energy spectrum  

E-print Network

There may be a high-energy cutoff of neutrino events in IceCube data. In particular, IceCube does not observe the Standard Model Glashow-resonance events expected at 6.3 PeV. There are also no higher-energy neutrino signatures in the ANITA and Auger experiments. This absence of high-energy neutrino events motivates models with a fundamental restriction on neutrino energies above a few PeV. The simplest scenario to terminate the neutrino spectrum is Lorentz-invariance violating with a limiting neutrino velocity that is smaller than the speed of light. A consequence is that charged pions are stable above four times the maximum neutrino energy and may serve as a cosmic ray primary.

Anchordoqui, L A; Goldberg, H; Learned, J G; Marfatia, D; Pakvasa, S; Paul, T C; Weiler, T J

2014-01-01

458

Solar Neutrino Experiments Neutrinos are ghostlike particles that  

E-print Network

investigat- ing neutrinos that were produced in Brookhaven's Graphite Research Reactor and at a reactor quadrillion times smaller than its capturing a neutron in a nuclear reactor. Despite these odds, Davis's ex Aeronautics & Space Administration's Lunar Sample Review Board, and was involved in the analysis of lunar dust

459

Effects of random density fluctuations on Supernovae and solar neutrinos  

E-print Network

Effects of random density fluctuations on Supernovae and solar neutrinos Timur Rashba MPI, Munich timur@mppmu.mpg.de Neutrino oscillations in fluctuating media ­ p.1 #12;Outline Solar neutrinos Summary timur@mppmu.mpg.de Neutrino oscillations in fluctuating media ­ p.2 #12;Neutrino oscillations 10

California at Santa Cruz, University of

460

Solar Neutrinos: Solved and Unsolved Problems John N. Bahcall  

E-print Network

Chapter 10 Solar Neutrinos: Solved and Unsolved Problems John N. Bahcall Institute for Advanced study solar neutrinos? What does the combined standard model (solar plus electroweak) predict for solar neutrinos? Why are the calculations of neutrino fluxes robust? What are the three solar neutrino problems

Bahcall, John

461

Tau Neutrino Astronomy in GeV Energies  

E-print Network

We point out the opportunity of the tau neutrino astronomy for the neutrino energy E ranging between 10 GeV and 10^3 GeV. In this energy range, the intrinsic tau neutrino production is suppressed relative to the intrinsic muon neutrino production. Any sizable tau neutrino flux may thus arise because of the \

H. Athar; F. -F. Lee; G. -L. Lin

2005-05-09

462

Search for neutrino decay during the 1999 solar eclipse  

Microsoft Academic Search

The solar neutrino problem could arise from oscillation of one neutrinotype into a secondtype. Neutrinos would have a mass and there could be the possibility ofradiative neutrino decays. We discuss the search for neutrino decaysduring the 1999 solar eclipse: it involves the emitted visible photons,while neutrinos travel from the Moon to the Earth. The concept and themain characteristics of the

S. Cecchini; G. Giacomelli; D. Hasegan; G. Mandrioli; O. Maris; L. Patrizii; A. Plaian; V. Popa; L. ?tefanov; V. V?leanu

2000-01-01

463

If sterile neutrinos exist, how can one determine the total solar neutrino fluxes? John N. Bahcall,1,  

E-print Network

If sterile neutrinos exist, how can one determine the total solar neutrino fluxes? John N. Bahcall solar neutrino flux inferred from a global analysis of solar neutrino experiments is within 11% (1 ) of the predicted standard solar model value if only active neutrinos exist, but could be as large as 1.7 times

Bahcall, John

464

Neutrino conversions in solar random magnetic fields  

NASA Astrophysics Data System (ADS)

We consider the effect of a random magnetic field in the convective zone of the Sun superimposed to a regular magnetic field on resonant neutrino spin-flavor oscillations. We argue for the existence of a field of strongly chaotic nature at the bottom of the convective zone. In contrast to previous attempts we employ a model motivated regular magnetic field profile: it is a static field solution to the solar equilibrium hydro-magnetic equations. These solutions have been known for a long time in the literature. We show for the first time that in addition they are twisting solutions. In this scenario electron antineutrinos are produced through cascades like ?eL-->??L-- >?~eR, The detection of ?~eR at Earth would be a long-awaited signature of the Majorana nature of the neutrino. The expected signals in the different experiments (SK, GALLEX-SAGE, Homestake) are obtained as a function of the level of noise, regular magnetic field and neutrino mixing parameters. Previous results obtained for small mixing and ad-hoc regular magnetic profiles are reobtained. We confirm the strong suppression for a large part of the parameter space of the ?~eR-flux for high energy boron neutrinos in agreement with present data of the SK experiment. We find that MSW (Mikheyev-Smirnov-Wolfenstein) regions (?m2~=10-5 eV2, both small and large mixing solutions) are stable up to very large levels of noise (P=0.7-0.8) but they are acceptable from the point of view of antineutrino production only for moderate levels of noise (P~=0.95). For strong noise and a reasonable regular magnetic field, any parameter region (?m2, sin 2 2?) is excluded. As a consequence, we are allowed to reverse the problem and to put limits on the r.m.s. field strength and transition magnetic moments by demanding a particle physics solution to the SNP in this scenario.

Semikoz, V. B.; Torrente-Lujan, E.

1999-09-01

465

Medium-energy neutrino physics  

SciTech Connect

A selection of opportunities for neutrino physics from a source generated from pions that decay in flight and at rest is described. The present source at LAMPF has a duty factor of about 6%; improvements in opportunities that emerge from a source using a pulse 0.25 {mu}sec long from a proton storage ring are also described. 7 refs., 9 figs.

White, D.H.

1991-11-22

466

Cosmic rays & Neutrinos Historical development  

E-print Network

| Perm in hairdressing Deutsch The Neutrino Wolfgang Pauli's name is inseparable from his pioneering. The starting point for Pauli was the continuous energy spectrum of beta rays, which could not be interpreted conservation, which Pauli could not accept because the principle of the conservation of energy had proved

Gaisser, Thomas K.

467

What are the Neutrino Masses  

E-print Network

The possible source of the production of neutrino with large masses is considered. For this purpose the reaction nu+n to e+p+gamma, in which the electron in neW+ vertex is produced off-mass-shell, is studied.

V. P. Efrosinin

2009-04-03

468

IceCube Neutrino Observatory  

NSDL National Science Digital Library

A neutrino, for those of us who might not immerse ourselves regularly in the world of very small things, is a nearly massless sub-atomic particle that travels at just about the speed of light. Born in the cauldron of exploding stars, they can move through lead like you and I move through air. Hence, their nickname: âÂÂghost particles.â IceCube, a particle detector planted in the barren wilds of the South Pole, measures neutrinos in hopes to contribute to the scientific understanding of dark matter and other universal mysteries. From the homepage, have a look at About Us, which explains IceCube and includes interviews with drillers, scientists, and support staff. Check out the Science section to read All About Neutrinos and other linked articles. If youâÂÂre interested in what it might be like to live at the worldâÂÂs largest neutrino detector, click Life@Pole, where you can read about Daily Life and other interesting tidbits about Life at the South Pole.

469

Effects of neutrino oscillations on nucleosynthesis and neutrino signals for an 18 M supernova model  

E-print Network

In this paper, we explore the effects of neutrino flavor oscillations on supernova nucleosynthesis and on the neutrino signals. Our study is based on detailed information about the neutrino spectra and their time evolution from a spherically-symmetric supernova model for an 18 M progenitor. We find that collective neutrino oscillations are not only sensitive to the detailed neutrino energy and angular distributions at emission, but also to the time evolution of both the neutrino spectra and the electron density profile. We apply the results of neutrino oscillations to study the impact on supernova nucleosynthesis and on the neutrino signals from a Galactic supernova. We show that in our supernova model, collective neutrino oscillations enhance the production of rare isotopes 138La and 180Ta but have little impact on the nu p-process nucleosynthesis. In addition, the adiabatic MSW flavor transformation, which occurs in the C/O and He shells of the supernova, may affect the production of light nuclei such as 7Li and 11B. For the neutrino signals, we calculate the rate of neutrino events in the Super-Kamiokande detector and in a hypothetical liquid argon detector. Our results suggest the possibility of using the time profiles of the events in both detectors, along with the spectral information of the detected neutrinos, to infer the neutrino mass hierarchy.

Meng-Ru Wu; Yong-Zhong Qian; Gabriel Martinez-Pinedo; Tobias Fischer; Lutz Huther

2014-12-30

470

Neutrino radiography of the Earth with the IceCube Neutrino Observatory  

NASA Astrophysics Data System (ADS)

Probing interior structures of the Earth with neutrinos has been discussed for more than 30 years. Unlike muons, neutrinos are chargeless particles and have very small cross-sections. They normally penetrate the Earth without any interaction, and from the rare interactions that do occur we obtain information on the density profile of the Earth's interior. Since this method is independent of any geophysical models, it has been expected to complement indirect physical methods such as seismic wave propagation analysis. However, the elusive characteristic of neutrinos poses a challenge for detecting them at experimental sites. To compensate for the small interaction cross-section, one needs a large volume neutrino detector. In the spring of 2011, IceCube, the world's largest neutrino observatory, was completed within deep glacial ice at the South Pole. IceCube is designed to detect Cherenkov light emitted by secondary charged particles generated from high-energy neutrinos. The primary mission of IceCube is to discover the origin of cosmic neutrinos. Toward that end, detailed studies of the atmospheric neutrino background have been performed in the last six years. Using these atmospheric neutrino events, we started a practical application of "neutrino radiography" which used to be known as "neutrino absorption tomography." In this talk we present a review of neutrino radiography including history from past decades and recent progress with the IceCube Neutrino Observatory.lt;img border=0 src="images/P23D-03_B.jpg">

Hoshina, K.; Tanaka, H.

2012-12-01

471

Coronal Neutrino Emission in Hypercritical Accretion Flows  

NASA Astrophysics Data System (ADS)

Hypercritical accretion flows onto stellar mass black holes (BHs) are commonly believed to be as a promising model of central engines of gamma-ray bursts (GRBs). In this model a certain fraction of the gravitational binding energy of accreting matter is deposited to the energy of relativistic jets via neutrino annihilation and/or magnetic fields. However, some recent studies have indicated that the energy deposition rate by neutrino annihilation is somewhat smaller than that needed to power a GRB. To overcome this difficulty, Ramirez-Ruiz and Socrates proposed that high-energy neutrinos from the hot corona above the accretion disk might enhance the efficiency of the energy deposition. We elucidate the disk corona model in the context of hypercritical accretion flows. From the energy balance in the disk and the corona, we can calculate the disk and coronal temperature, Td and Tc, and neutrino spectra, taking into account the neutrino cooling processes by neutrino-electron scatterings and neutrino pair productions. The calculated neutrino spectra consist of two peaks: one by the neutrino emission from the disk and the other by that from the corona. We find that the disk corona can enhance the efficiency of energy release but only by a factor of 1.5 or so, unless the height of the corona is very small, H<neutrino emission is very sensitive to the temperature of the emitting region, and then the ratio Tc/Td cannot be very large.

Kawabata, R.; Mineshige, S.; Kawanaka, N.

2008-03-01

472

Nonlinear matter spectra in growing neutrino quintessence  

E-print Network

We investigate the nonlinear power spectra of density perturbations and acoustic oscillations in growing neutrino quintessence. In this scenario, the neutrino mass has a strong dependence on the quintessence field. The induced coupling stops the evolution of the field when the neutrinos become nonrelativistic, and triggers the transition to the accelerating phase of the cosmological expansion. At redshifts around five, the neutrino fluctuations are still linear and acoustic oscillations are present in the neutrino power spectrum, induced by the acoustic oscillations in the baryonic and dark-matter sectors. The neutrino perturbations become nonlinear at redshifts around three. The mode coupling generated by the nonlinearities erases the oscillations in the neutrino spectrum at some redshift above two. There is a potential danger that at later times the influence of the gravitational potentials induced by the neutrino inhomogeneities could erase the oscillations from the baryonic and dark-matter spectra, making the scenario incompatible with observations. For the scenario to be viable, the neutrino-induced gravitational potentials in the range of baryonic acoustic oscillations should not grow to average values much larger than 10^{-4}. The magnitude of the expected potentials is still not known reliably, as the process of structure formation is poorly understood in growing neutrino quintessence.

N. Brouzakis; V. Pettorino; N. Tetradis; C. Wetterich

2014-04-10

473

Beta Beams for Neutrino Production  

NASA Astrophysics Data System (ADS)

This paper gives an overview of the work done so far to produce sufficient neutrino fluxes for neutrino oscillation physics using beta beams. The design study on a beta beam scenario, the EURISOL (European Isotope Separation On-Line Radioactive Ion Beam Facility) Design Study, a project funded by the European Commission (EC), is now ready to be published. The study is based on the acceleration of 6He and 18Ne ions to produce the (anti-)neutrino beam using the existing CERN infrastructure for acceleration of the ions. We will here briefly describe the work with emphasis on how potential showstoppers, in particular radiation safety and equipment damage, have been dealt with. New results for the production of 6He show very encouraging results. We are now confident that this ion is a good choice to produce antineutrinos. However, the ion production needed for the physics experiments could not, up to now, be reasonably satisfied for 18Ne. Therefore, studies of alternative beta emitters, 8Li and 8B, with properties interesting for physics reach, have been proposed. The production of these ions is studied within the EC funded EUROnu project, "A High Intensity Neutrino Oscillation Facility for Europe." This project will end in 2012. A small storage ring, in which the beam traverses a target, creating the 8Li and 8B isotopes that will be collected and accelerated, is studied in this proposal. We present the latest developments for the production of these ions, including a production ring lattice. Extensive Geant4 simulations have been done with the aim of developing a model of the production target that can be used for simulations of the necessary cooling system. In this paper we present the status of the work performed and an overview of ongoing and planned activities to make the beta beam project a solid proposal for neutrino production within the EUROnu project.

Wildner, Elena

2010-03-01

474

Beta Beams for Neutrino Production  

SciTech Connect

This paper gives an overview of the work done so far to produce sufficient neutrino fluxes for neutrino oscillation physics using beta beams. The design study on a beta beam scenario, the EURISOL (European Isotope Separation On-Line Radioactive Ion Beam Facility) Design Study, a project funded by the European Commission (EC), is now ready to be published. The study is based on the acceleration of {sup 6}He and {sup 18}Ne ions to produce the (anti-)neutrino beam using the existing CERN infrastructure for acceleration of the ions. We will here briefly describe the work with emphasis on how potential showstoppers, in particular radiation safety and equipment damage, have been dealt with. New results for the production of {sup 6}He show very encouraging results. We are now confident that this ion is a good choice to produce antineutrinos. However, the ion production needed for the physics experiments could not, up to now, be reasonably satisfied for {sup 18}Ne. Therefore, studies of alternative beta emitters, {sup 8}Li and {sup 8}B, with properties interesting for physics reach, have been proposed. The production of these ions is studied within the EC funded EUROnu project, ''A High Intensity Neutrino Oscillation Facility for Europe.'' This project will end in 2012. A small storage ring, in which the beam traverses a target, creating the {sup 8}Li and {sup 8}B isotopes that will be collected and accelerated, is studied in this proposal. We present the latest developments for the production of these ions, including a production ring lattice. Extensive Geant4 simulations have been done with the aim of developing a model of the production target that can be used for simulations of the necessary cooling system. In this paper we present the status of the work performed and an overview of ongoing and planned activities to make the beta beam project a solid proposal for neutrino production within the EUROnu project.

Wildner, Elena [CERN, Geneva (Switzerland)

2010-03-30

475

Capturing Relic Neutrinos with beta-decaying nuclei  

E-print Network

We summarize a novel approach which has been recently proposed for direct detection of low energy neutrino backgrounds such as the cosmological relic neutrinos, exploiting neutrino/antineutrino capture on nuclei that spontaneously undergo beta decay.

Alfredo G. Cocco; Gianpiero Mangano; Marcello Messina

2007-11-12

476

Cross section dependence of event rates at neutrino telescopes  

E-print Network

We examine the dependence of event rates at neutrino telescopes on the neutrino-nucleon cross section for neutrinos with energy above 1 PeV, and contrast the results with those for cosmic ray experiments. Scaling of the ...

Marfatia, Danny; Seckel, D.; McKay, D. W.; Hussain, S.

2006-10-20

477

Neutrino-2008: Where are we? Where are we going?  

E-print Network

Our present knowledge of neutrinos can be summarized in terms of the "standard neutrino scenario". Phenomenology of this scenario as well as attempts to uncover physics behind neutrino mass and mixing are described. Goals of future studies include complete reconstruction of the neutrino mass and flavor spectrum, further test of the standard scenario and search for new physics beyond it. Developments of new experimental techniques may lead to construction of new neutrino detectors from table-top to multi-Megaton scales which will open new horizons in the field. With detection of neutrino bursts from the Galactic supernova and high energy cosmic neutrinos neutrino astrophysics will enter qualitatively new phase. Neutrinos and LHC (and future colliders), neutrino astronomy, neutrino structure of the Universe, and probably, neutrino technologies will be among leading topics of research.

Smirnov, Alexei Yu

2008-01-01

478

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

PubMed

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