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1

Fourth Generation Majorana Neutrinos  

Microsoft Academic Search

We investigate the possibility of a fourth sequential generation in the lepton sector. Assuming neutrinos to be Majorana particles and starting from a recent - albeit weak - evidence for a non-zero admixture of a fourth generation neutrino from fits to weak lepton and meson decays we discuss constraints from neutrinoless double beta decay, radiative lepton decay and like-sign dilepton

Alexander Lenz; Heinrich Päs; Dario Schalla

2011-01-01

2

Constraints on fourth generation Majorana neutrinos  

Microsoft Academic Search

We investigate the possibility of a fourth sequential generation in the lepton sector. Assuming neutrinos to be Majorana particles and starting from a recent - albeit weak - evidence for a non-zero admixture of a fourth generation neutrino from fits to weak lepton and meson decays we discuss constraints from neutrinoless double beta decay, radiative lepton decay and like-sign di-lepton

Alexander Lenz; Heinrich Päs; Dario Schalla

2010-01-01

3

Fourth lepton family is natural in technicolor  

SciTech Connect

Imagine discovering a new fourth family of leptons at the Large Hadron Collider (LHC) but no signs of an associated fourth family of quarks. What would that imply? An intriguing possibility is that the new fermions needed to compensate for the new leptons gauge anomalies simultaneously address the big hierarchy problem of the standard model. A natural way to accomplish such a scenario is to have the Higgs itself be a composite of these new fermions. This is the setup we are going to investigate in this paper using as a template minimal walking technicolor. We analyze a general heavy neutrino mass structure with and without mixing with the standard model families. We also analyze the LHC potential to observe the fourth lepton family in tandem with the new composite Higgs dynamics. We finally introduce a model uniting the fourth lepton family and the technifermion sector at higher energies.

Frandsen, Mads T. [CP3 - Origins, IFK and IMADA, University of Southern Denmark, Campusvej 55, DK-5230 Odense M (Denmark); Rudolf Peierls Centre for Theoretical Physics, University of Oxford, 1 Keble Road, Oxford OX1 3NP (United Kingdom); Masina, Isabella [Dipartimento di Fisica dell'Universita degli Studi di Ferrara and INFN Sezione di Ferrara, Via Saragat 1, I-44100 Ferrara (Italy); CP3 - Origins, IFK and IMADA, University of Southern Denmark, Campusvej 55, DK-5230 Odense M (Denmark); Sannino, Francesco [CP3 - Origins, IFK and IMADA, University of Southern Denmark, Campusvej 55, DK-5230 Odense M (Denmark)

2010-02-01

4

Search for the fourth standard model family  

SciTech Connect

Existence of the fourth family follows from the basics of the standard model (SM) and the actual mass spectrum of the third family fermions. We discuss possible manifestations of the fourth SM family at existing and future colliders. The LHC and Tevatron potentials to discover the fourth SM family have been compared. The scenario with dominance of the anomalous decay modes of the fourth-family quarks has been considered in detail.

Sahin, M.; Sultansoy, S.; Turkoz, S. [TOBB University of Economics and Technology, Physics Division, Ankara (Turkey); TOBB University of Economics and Technology, Physics Division, Ankara (Turkey) and Institute of Physics, National Academy of Sciences, Baku (Azerbaijan); Ankara University, Department of Physics, Ankara (Turkey)

2011-03-01

5

Fourth lepton family is natural in technicolor  

Microsoft Academic Search

Imagine discovering a new fourth family of leptons at the Large Hadron Collider (LHC) but no signs of an associated fourth family of quarks. What would that imply? An intriguing possibility is that the new fermions needed to compensate for the new leptons gauge anomalies simultaneously address the big hierarchy problem of the standard model. A natural way to accomplish

Mads T. Frandsen; Isabella Masina; Francesco Sannino

2010-01-01

6

Family Symmetry and Neutrino Mixing  

Microsoft Academic Search

The observed quark hierarchies suggest a simple family symmetry. Generalized to leptons through grand-unified quantum numbers, it produces a neutrino mixing matrix with order-1 numu-nutau mixing, and order- lambda3 nue-numu and nue-nutau mixings. The intrafamily hierarchy and observed neutrino mass differences together require this symmetry to be anomalous, suggesting through the Green-Schwarz mechanism a string or M-theory origin for the

John K. Elwood; Nikolaos Irges; Pierre Ramond

1998-01-01

7

On the nature of the fourth generation neutrino and its implications  

NASA Astrophysics Data System (ADS)

We consider the neutrino sector of a Standard Model with four generations. While the three light neutrinos can obtain their masses from a variety of mechanisms with or without new neutral fermions, fourth-generation neutrinos need at least one new relatively light right-handed neutrino. If lepton number is not conserved this neutrino must have a Majorana mass term whose size depends on the underlying mechanism for lepton number violation. Majorana masses for the fourth-generation neutrinos induce relative large two-loop contributions to the light neutrino masses which could be even larger than the cosmological bounds. This sets strong limits on the mass parameters and mixings of the fourth-generation neutrinos.

Aparici, Alberto; Herrero-García, Juan; Rius, Nuria; Santamaria, Arcadi

2012-07-01

8

Leptonic mixing, family symmetries, and neutrino phenomenology  

SciTech Connect

Tribimaximal leptonic mixing is a mass-independent mixing scheme consistent with the present solar and atmospheric neutrino data. By conveniently decomposing the effective neutrino mass matrix associated to it, we derive generic predictions in terms of the parameters governing the neutrino masses. We extend this phenomenological analysis to other mass-independent mixing schemes which are related to the tribimaximal form by a unitary transformation. We classify models that produce tribimaximal leptonic mixing through the group structure of their family symmetries in order to point out that there is often a direct connection between the group structure and the phenomenological analysis. The type of seesaw mechanism responsible for neutrino masses plays a role here, as it restricts the choices of family representations and affects the viability of leptogenesis. We also present a recipe to generalize a given tribimaximal model to an associated model with a different mass-independent mixing scheme, which preserves the connection between the group structure and phenomenology as in the original model. This procedure is explicitly illustrated by constructing toy models with the transpose tribimaximal, bimaximal, golden ratio, and hexagonal leptonic mixing patterns.

Medeiros Varzielas, I. de [Departamento de Fisica and Centro de Fisica Teorica de Particulas, Instituto Superior Tecnico, Avenida Rovisco Pais, 1049-001 Lisboa (Portugal); Fakultaet fuer Physik, Technische Universitaet Dortmund D-44221 Dortmund (Germany); Gonzalez Felipe, R. [Departamento de Fisica and Centro de Fisica Teorica de Particulas, Instituto Superior Tecnico, Avenida Rovisco Pais, 1049-001 Lisboa (Portugal); Instituto Superior de Engenharia de Lisboa, Rua Conselheiro Emidio Navarro, 1959-007 Lisboa (Portugal); Serodio, H. [Departamento de Fisica and Centro de Fisica Teorica de Particulas, Instituto Superior Tecnico, Avenida Rovisco Pais, 1049-001 Lisboa (Portugal)

2011-02-01

9

Family hierarchy and large neutrino mixings  

Microsoft Academic Search

The recent neutrino data seem to favor two large and one small mixing angles and a hierarchy of their squared mass differences. We discuss these within the context of hierarchical neutrino masses. We show that this scheme suggests a specific neutrino mass matrix with mild fine-tuning. We then present a Froggatt–Nielsen model that reproduces this matrix.

Fu-Sin Ling; Pierre Ramond

2002-01-01

10

Quasi-degenerate neutrinos from an abelian family symmetry  

SciTech Connect

The authors show that models with an abelian family symmetry which accounts for the observed hierarchies of masses and mixings in the quark sector may also accommodate quasi-degeneracies in the neutrino mass spectrum. Such approximate degeneracies are, in this context, associated with large mixing angles. The parameters of this class of models are constrained. The authors discuss their phenomenological implications for present and foreseen neutrino experiments.

Binetruy, P. [Univ. Paris-Sud, Orsay (France). Lab. de Physique Theorique et Hautes Energies]|[Lawrence Berkeley National Lab., CA (United States); Lavignac, S. [Univ. Paris-Sud, Orsay (France). Lab. de Physique Theorique et Hautes Energies; Petcov, S. [Scuola Internazionale Superiore di Studi Avanzati, Trieste (Italy)]|[Ist. Nazionale di Fisica Nucleare, Trieste (Italy). Sezione di Trieste; Ramond, P. [Florida Univ., Gainesville, FL (United States). Inst. for Fundamental Theory

1996-12-31

11

MSSM extension with a mirror fourth generation, neutrino magnetic moments, and CERN LHC signatures  

SciTech Connect

Recent analyses have shown that a sequential fourth generation can be consistent with precision electroweak data. We consider the possibility that the new generation could be a mirror generation with V+A rather than V-A interactions. Specifically we consider an extension of the minimal supersymmetric standard model with a light mirror generation. Implications of this extension are explored. One consequence is an enhancement of the {tau} neutrino magnetic moment by several orders of magnitude consistent with the current limits on the magnetic moment of the {tau}. The masses of the mirror generation arise due to electroweak symmetry breaking, and if a mirror generation exists its mass spectrum must lie below a TeV, and thus should be discovered at the LHC. Mirror particles and mirror sparticles produce many characteristic signatures which should be detectable at the LHC. Heavy Higgs boson decays into mirror particles and an analysis of the forward-backward asymmetries can distinguish a mirror generation from a sequential fourth generation. The validity of the model can thus be tested at the LHC. A model of the type discussed here could arise from a more unified structure such as grand unification or strings where a mirror generation escapes the survival hypothesis, i.e., a generation and a mirror generation do not tie up to acquire a mass of size M{sub GUT} or M{sub string} due to a symmetry, and thus remain massless down to the electroweak scale.

Ibrahim, Tarek [Department of Physics, Faculty of Science, University of Alexandria, Alexandria (Egypt); Department of Physics, Northeastern University, Boston, Massachusetts 02115-5000 (United States); Nath, Pran [Department of Physics, Northeastern University, Boston, Massachusetts 02115-5000 (United States); Theory Division, Physics Department, CERN, CH-1211 Geneva 23 (Switzerland)

2008-10-01

12

Quasi-degenerate neutrinos from an Abelian family symmetry  

Microsoft Academic Search

We show that models with an Abelian family symmetry which accounts for the observed hierarchies of masses and mixings in the quark sector may also accommodate quasi-degeneracies in the neutrino mass spectrum. Such approximate degeneracies are, in this context, associated with large mixing angles. The parameters of this class of models are constrained. We discuss their phenomenological implications for present

Pierre Binétruy; Stéphane Lavignac; Serguey Petcov; Pierre Ramond

1997-01-01

13

Family Influence: Key to Fruit and Vegetable Consumption among Fourth- and Fifth-Grade Students  

ERIC Educational Resources Information Center

Objective: To assess social and familial environmental influences on fruit and vegetable (FV) consumption of fourth- and fifth-graders living in a culturally diverse, urban setting. Design: In 2006, students from 9 fourth- and fifth-grade classrooms from a public school in the Washington-Baltimore Metropolitan Region were recruited as part of the…

Gross, Susan M.; Pollock, Elizabeth Davenport; Braun, Bonnie

2010-01-01

14

Family Outing Activities and Achievement among Fourth Graders in Compensatory Education Funded Schools.  

ERIC Educational Resources Information Center

This study sought to identify the relationship between operationally-defined family outing activities and measures of achievement among fourth grade students from educationally disadvantaged backgrounds. The results, collected for four successive years from 1715 students in urban Los Angeles, indicated that: (1) participation in family activities…

Griswold, Philip A.

15

Familial third-fourth pharyngeal pouch syndrome with apparent autosomal dominant transmission.  

PubMed

A family is presented in which both siblings and their father had evidence of third-fourth pharyngeal pouch syndrome (DiGeorge syndrome). All three individuals had hypocalcemia and unusual facies. Both infants had truncus arteriosus. One infant had evidence of impaired cell-mediated immunity; the father had a relatively decreased number of T-lymphocytes. The syndrome is uncommon, most cases being isolated, and familial presentations are even rarer. Two recent reports described several affected individuals who also had partial deletions of chromosome 22. Chromosome banding studies in our family were normal. Thus our family demonstrates an autosomal dominant pattern of inheritance, although it cannot be proved that this is a single gene defect. We propose that inasmuch as the presentation of the syndrome is quite varied, thorough family investigation including high-resolution cytogenetic analysis is necessary. Familial cases may be more common and require genetic counseling. PMID:6737148

Rohn, R D; Leffell, M S; Leadem, P; Johnson, D; Rubio, T; Emanuel, B S

1984-07-01

16

Higgs Mass Constraints on a Fourth Family: Upper and Lower Limits on CKM Mixing  

SciTech Connect

Theoretical and experimental limits on the Higgs boson mass restrict CKM mixing of a possible fourth family beyond the constraints previously obtained from precision electroweak data alone. Existing experimental and theoretical bounds on m{sub H} already significantly restrict the allowed parameter space. Zero CKM mixing is excluded and mixing of order {theta}{sub Cabbibo} is allowed. Upper and lower limits on 3-4 CKM mixing are exhibited as a function of m{sub H}. We use the default inputs of the Electroweak Working Group and also explore the sensitivity of both the three and four family fits to alternative inputs.

Chanowitz, Michael S.

2010-06-25

17

Single Anomalous Production of the Fourth SM Family Quarks at Future e+e-, ep, and pp Colliders  

SciTech Connect

Possible single productions of fourth SM family u4 and d4 quarks via anomalous interactions at the e+e-, ep, and pp colliders are investigated. Signatures of such anomalous processes are discussed at above colliders comparatively.

Ciftci, A. K. [Physics Department, Faculty of Sciences, Ankara University, 06100 Tandogan, Ankara (Turkey); Ciftci, R. [Physics Department, Faculty of Sciences and Arts, Gazi University, 06500 Teknikokullar, Ankara (Turkey); Sultansoy, S. [Physics Department, Faculty of Sciences and Arts, Gazi University, 06500 Teknikokullar, Ankara (Turkey); Institute of Physics, Academy of Sciences, H.Cavid Avenue 33, Baku (Azerbaijan); Yildiz, H. Duran [Physics Department, Faculty of Sciences and Arts, Dumlupinar University, Merkez Kampus, Ankara (Turkey)

2007-04-23

18

Predicting neutrino parameters from SO(3) family symmetry and quark-lepton unification  

NASA Astrophysics Data System (ADS)

We show how the neutrino mixing angles and oscillation phase can be predicted from tri-bimaximal neutrino mixing, corrected by charged lepton mixing angles which are related to quark mixing angles via quark-lepton unification. The tri-bimaximal neutrino mixing can naturally originate from the see-saw mechanism via constrained sequential dominance (CSD), where CSD can result from the vacuum alignment of a non-abelian family symmetry such as SO(3). We construct a realistic model of quark and lepton masses and mixings based on SO(3) family symmetry with quark-lepton unification based on the Pati-Salam gauge group. The atmospheric angle is predicted to be approximately maximal ?23 = 45°, corrected by the quark mixing angle ?23CKM approx 2.4°, with the correction controlled by an undetermined phase in the quark sector. The solar angle is predicted by the tri-bimaximal complementarity relation: ?12+(1/21/2)(?C/3)cos (?-?) approx 35.26°, where ?C is the Cabibbo angle and ? is the neutrino oscillation phase. The reactor angle is predicted to be ?13 approx (1/21/2)(?C/3) approx 3.06°. The MNS neutrino oscillation phase ? is predicted in terms of the solar angle to be cos (?-?) approx (35.26°-?12°)/3.06°. These predictions can all be tested by future high precision neutrino oscillation experiments, thereby probing the nature of high energy quark-lepton unification.

King, Stephen F.

2005-08-01

19

Anomalous single production of fourth family up-type quark associated with neutral gauge bosons at the LHC  

NASA Astrophysics Data System (ADS)

The fourth family quarks are expected to have mass larger than the top quark considering the results from recent studies on the allowed parameter space. They could also have different dynamics than the quarks of three families of the standard model. The single production of the fourth family up-type quark t? is studied via the anomalous production process pp ? t?VX (where V = g, Z, ?) at the LHC with the center of mass energy of 7 and 14 TeV. The signatures of such process are discussed within both the SM and the anomalous decay modes of t? quarks. The sensitivity to anomalous coupling ?/? = 0.004 TeV-1 can be reached at \\sqrt{s}=14 TeV and Lint = 100 pb-1.

Çak?r, O.; Çak?r, I. T.; Senol, A.; Tasci, A. T.

2012-05-01

20

Icosahedral (A5) family symmetry and the golden ratio prediction for solar neutrino mixing  

Microsoft Academic Search

We investigate the possibility of using icosahedral symmetry as a family symmetry group in the lepton sector. The rotational icosahedral group, which is isomorphic to A5, the alternating group of five elements, provides a natural context in which to explore (among other possibilities) the intriguing hypothesis that the solar neutrino mixing angle is governed by the golden ratio, varphi=(1+5)\\/2. We

Lisa L. Everett; Alexander J. Stuart

2009-01-01

21

A direct determination of the number of light neutrino families from e +e -?? overline?? at LEP  

NASA Astrophysics Data System (ADS)

The L3 detector at LEP has been used to determine the number of light neutrino families by measuring the cross section of single photon even in e +e - collisions at energies near the Z 0 resonance. We have observed 61 single photon candidates with more than 1.5 GeV of deposited energy in the barrel electromagnetic calorimeter, for a total integrated luminosity of 3.0 pb -1. From a likelihood fir to the single photon cross sections, we determin N?=3.24 ± 0.46 ( statistical) ±0.22 ( systematic).

Adeva, B.; Adriani, O.; Aguilar-Benitez, M.; Akbari, H.; Alcaraz, J.; Aloisio, A.; Alverson, G.; Alviggi, M. G.; Ambrosi, G.; An, Q.; Anderhub, H.; Anderson, A. L.; Andreev, V. P.; Angelov, T.; Antonov, L.; Antreasyan, D.; Arce, P.; Arefiev, A.; Atamanchuk, A.; Azemoon, T.; Aziz, T.; Baba, P. V. K. S.; Bagnaia, P.; Bakken, J. A.; Baksay, L.; Ball, R. C.; Banerjee, S.; Bao, J.; Barillère, R.; Barone, L.; Battiston, R.; Bay, A.; Becattini, F.; Becker, U.; Behner, F.; Behrens, J.; Beingessner, S.; Bencze, Gy. L.; Berdugo, J.; Berges, P.; Bertucci, B.; Betev, B. L.; Biasini, M.; Biland, A.; Bilei, G. M.; Bizzarri, R.; Blaising, J. J.; Blömeke, P.; Blumenfeld, B.; Bobbink, G. J.; Bocciolini, M.; Bock, R.; Böhm, A.; Borgia, B.; Bourilkov, D.; Bourquin, M.; Boutigny, D.; Bouwens, B.; Brambilla, E.; Branson, J. G.; Brock, I. C.; Brooks, M.; Bruyant, F.; Buisson, C.; Bujak, A.; Burger, J. D.; Burger, W. J.; Burq, J. P.; Busenitz, J.; Cai, X. D.; Capell, M.; Caria, M.; Carminati, F.; Cartacci, A. M.; Cerrada, M.; Cesaroni, F.; Chang, Y. H.; Chaturvedi, U. K.; Chemarin, M.; Chen, A.; Chen, C.; Chen, G. M.; Chen, H. F.; Chen, H. S.; Chen, J.; Chen, M.; Chen, M. L.; Chen, W. Y.; Chiefari, G.; Chien, C. Y.; Chmeissani, M.; Civinni, C.; Clare, I.; Clare, R.; Coan, T. E.; Cohn, H. O.; Coignet, G.; Colino, N.; Contin, A.; Crijns, F.; Cui, X. Y.; Dai, T. S.; D'Alessandro, R.; de Asmundis, R.; Degré, A.; Deiters, K.; Dénes, E.; Denes, P.; DeNotaristefani, F.; Dhina, M.; DiBitonto, D.; Diemoz, M.; Dimitrov, H. R.; Dionisi, C.; Dova, M. T.; Drago, E.; Driever, T.; Duchesneau, D.; Duinker, P.; Duran, I.; El Mamouni, H.; Engler, A.; Eppling, F. J.; Erné, F. C.; Extermann, P.; Fabbretti, R.; Fabre, M.; Falciano, S.; Fan, Q.; Fan, S. J.; Fackler, O.; Fay, J.; Felcini, M.; Ferguson, T.; Fernandez, D.; Fernandez, G.; Ferroni, F.; Fesefeldt, H.; Fiandrini, E.; Field, J.; Filthaut, F.; Finocchiaro, G.; Fisher, P. H.; Forconi, G.; Foreman, T.; Freudenreich, K.; Friebel, W.; Fukushima, M.; Gailloud, M.; Galaktionov, Yu.; Gallo, E.; Ganguli, S. N.; Garcia-Abia, P.; Gau, S. S.; Gele, D.; Gentile, S.; Goldfarb, S.; Gong, Z. F.; Gonzalez, E.; Gordeev, A.; Göttlicher, P.; Goujon, D.; Gratta, G.; Grinnell, C.; Gruenewald, M.; Guanziroli, M.; Guo, J. K.; Gurtu, A.; Gustafson, H. R.; Gutay, L. J.; Hangarter, K.; Hasan, A.; Hauschildt, D.; He, C. T.; Hebbeker, T.; Hebert, M.; Herten, G.; Herten, U.; Hervé, A.; Hilgers, K.; Hofer, H.; Hoorani, H.; Hu, G.; Hu, G. Q.; Ille, B.; Ilyas, M. M.; Innocente, V.; Janssen, H.; Jezequel, S.; Jin, B. N.; Jones, L. W.; Kasser, A.; Khan, R. A.; Kamyshkov, Yu.; Kapinos, P.; Kapustinsky, J. S.; Karyotakis, Y.; Kaur, M.; Khokhar, S.; Kienzle-Focacci, M. N.; Kinnison, W. W.; Kirby, D.; Kirsch, S.; Kittel, W.; Klimentov, A.; König, A. C.; Kornadt, O.; Koutsenko, V.; Koulbardis, A.; Kraemer, R. W.; Kramer, T.; Krastev, V. R.; Krenz, W.; Krovshich, A.; Krizmanic, J.; Kumar, K. S.; Kumar, V.; Kunin, A.; Landi, G.; Lanius, K.; Lanske, D.; Lanzano, S.; Lebrun, P.; Lecomte, P.; Lecoq, P.; Le Coultre, P.; Lee, D. M.; Leedom, I.; Le Goff, J. M.; Leistam, L.; Leiste, R.; Lenti, M.; Leonardi, E.; Lettry, J.; Leytens, X.; Li, C.; Li, H. T.; Li, J. F.; Li, P. J.; Li, Q.; Li, X. G.; Liao, J. Y.; Lin, W. T.; Lin, Z. Y.; Linde, F. L.; Lindemann, B.; Linnhofer, D.; Liu, R.; Liu, Y.; Lohmann, W.; Longo, E.; Lu, Y. S.; Lubbers, J. M.; Lübelsmeyer, K.; Luci, C.; Luckey, D.; Ludovici, L.; Luminari, L.; Ma, W. G.; MacDermott, M.; Malhorta, P. K.; Malik, R.; Malinin, A.; Maña, C.; Mao, D. N.; Mao, Y. F.; Maolinbay, M.; Marchesini, P.; Martin, J. P.; Martinez-Laso, L.; Marzano, F.; Massaro, G. G. G.; Matsuda, T.; Mazumdar, K.; McBride, P.; McMahon, T.; McNally, D.; Meinholz, Th.; Merk, M.; Merola, L.; Meschini, M.; Metzger, W. J.; Mi, Y.; Mills, G. B.; Mir, Y.; Mirabelli, G.; Mnich, J.; Möller, M.; Monteleoni, B.; Morand, R.; Morganti, S.; Moulai, N. E.; Mount, R.; Müller, S.; Nadtochy, A.; Nagy, E.; Napolitano, M.; Newman, H.; Neyer, C.; Niaz, M. A.; Niessen, L.; Nowak, H.; Organtini, G.; Pandoulas, D.; Pauluzzi, M.; Pauss, F.; Passaleva, G.; Paoletti, S.; Patricelli, S.; Pei, Y. J.; Perret-Gallix, D.; Perrier, J.; Pevsner, A.; Pieri, M.; Piroué, P. A.; Plasil, F.; Plyaskin, V.; Pohl, M.; Pojidaev, V.; Produit, N.; Qian, J. M.; Qureshi, K. N.; Raghavan, R.; Rahal-Callot, G.; Raven, G.; Razis, P.; Read, K.; Ren, D.; Ren, Z.; Rescigno, M.; Reucroft, S.; Ricker, A.; Riemann, S.; Rind, O.; Rizvi, H. A.; Roe, B. P.; Röhner, M.; Röhner, S.; Romero, L.; Rose, J.; Rosier-Lees, S.; Rosmalen, R.; Rosselet, Ph.; Rubbia, A.; Rubio, J. A.; Rykaczewski, H.; Sachwitz, M.; Salicio, J.; Salicio, J. M.; Sanders, G. S.; Santocchia, A.; Sarakinos, M. S.; Sartorelli, G.; Sauvage, G.; Savin, A.; Schegelsky, V.; Schmiemann, K.; Schmitz, D.; Schmitz, P.

1992-01-01

22

Family replicated gauge groups and large mixing angle solar neutrino solution  

NASA Astrophysics Data System (ADS)

We present a modification of our previous family replicated gauge group model, which now generates the Large Mixing Angle MSW solution rather than the experimentally disfavoured Small Mixing Angle MSW solution to the solar neutrino oscillation problem. The model is based on each family of quarks and leptons having its own set of gauge fields, each containing a replica of the Standard Model gauge fields plus a ( B- L)-coupled gauge field. By a careful choice of the Higgs field gauge quantum numbers, we avoid our previous prediction that the solar neutrino mixing angle is equal order of magnitudewise to the Cabibbo angle, replacing it and the well-known Fritzsch relation with the relation ? c˜(? ?) -1/3 (m d/m s) 2/3. At the same time we retain a phenomenologically successful structure for the charged quark and lepton mass matrices. A fit of all the seventeen quark-lepton mass and mixing angle observables, using just six new Higgs field vacuum expectation values, agrees with the experimental data within the theoretically expected uncertainty of about 64%, i.e., it fits perfectly order of magnitudewise.

Froggatt, C. D.; Nielsen, H. B.; Takanishi, Y.

2002-06-01

23

Molecular cloning of a fourth member of the potassium-dependent sodium-calcium exchanger gene family, NCKX4.  

PubMed

We report here the identification and characterization of a fourth member of the potassium-dependent sodium-calcium exchanger gene family, NCKX4 (gene SLC24A4), which mapped to the chromosomal region 14q32. Human NCKX4 encoded a protein of 605 amino acids that displayed a high level of sequence identity to previously described family members, rod NCKX1 (gene SLC24A1), cone/neuronal NCKX2 (gene SLC24A2), and ubiquitous NCKX3 (gene SLC24A3), in the hydrophobic regions surrounding the alpha-repeat sequences thought to form the ion-binding pocket used for transport. The protein product of the NCKX4 gene shared the highest level of amino acid identity, as well as an almost identical arrangement of exon boundaries, with NCKX3, indicating that these two genes have arisen from a recent duplication event. NCKX4 transcripts were abundantly expressed in all brain regions, aorta, lung, and thymus, as well as at a lower level in many other tissues. The NCKX4 protein demonstrated potassium-dependent sodium calcium exchanger activity when assayed in transfected HEK293 cells using digital imaging of fura-2 fluorescence. The discovery of NCKX4, as far as can be ascertained from the current version of the human genome sequence, completes the mammalian potassium-dependent sodium-calcium exchanger gene family. PMID:12379639

Li, Xiao-Fang; Kraev, Alexander S; Lytton, Jonathan

2002-12-13

24

Fermion masses and neutrino oscillations in SO(10) supersymmetric grand unified theory with D3×U(1) family symmetry  

NASA Astrophysics Data System (ADS)

Discrete non-Abelian gauge symmetries appear to be the most advantageous candidates for a family symmetry. We present a predictive SO(10) SUSY GUT model with D3×U(1) family symmetry (D3 is the dihedral group of order 6). The hierarchy in fermion masses is generated by the family symmetry breaking D3×U(1)-->ZN-->nothing. This model fits the low energy data in the charged fermion sector quite well and naturally provides large angle ??-?? mixing describing atmospheric neutrino oscillation data and small angle ?e-?s mixing consistent with the small mixing angle MSW solution to the solar neutrino data. In addition, the non-Abelian family symmetry D3 is sufficient to suppress large flavor violations.

Dermíšek, Radovan; Raby, Stuart

2000-07-01

25

A direct determination of the number of light neutrino families from e+e--->nunugamma at LEP  

Microsoft Academic Search

The L3 detector at LEP has been used to determine the number of light neutrino families by measuring the cross section of single photon even in e+e- collisions at energies near the Z0 resonance. We have observed 61 single photon candidates with more than 1.5 GeV of deposited energy in the barrel electromagnetic calorimeter, for a total integrated luminosity of

B. Adeva; O. Adriani; M. Aguilar-Benitez; H. Akbari; J. Alcaraz; A. Aloisio; G. Alverson; M. G. Alviggi; G. Ambrosi; Q. An; H. Anderhub; A. L. Anderson; V. P. Andreev; T. Angelov; L. Antonov; D. Antreasyan; P. Arce; A. Arefiev; A. Atamanchuk; T. Azemoon; T. Aziz; P. V. K. S. Baba; P. Bagnaia; J. A. Bakken; L. Baksay; R. C. Ball; S. Banerjee; J. Bao; R. Barillère; L. Barone; R. Battiston; A. Bay; F. Becattini; U. Becker; F. Behner; J. Behrens; S. Beingessner; Gy. L. Bencze; J. Berdugo; P. Berges; B. Bertucci; B. L. Betev; M. Biasini; A. Biland; G. M. Bilei; R. Bizzarri; J. J. Blaising; P. Blömeke; B. Blumenfeld; G. J. Bobbink; M. Bocciolini; R. Bock; A. Böhm; B. Borgia; D. Bourilkov; M. Bourquin; D. Boutigny; B. Bouwens; E. Brambilla; J. G. Branson; I. C. Brock; M. Brooks; F. Bruyant; C. Buisson; A. Bujak; J. D. Burger; W. J. Burger; J. P. Burq; J. Busenitz; X. D. Cai; M. Capell; M. Caria; F. Carminati; A. M. Cartacci; M. Cerrada; F. Cesaroni; Y. H. Chang; U. K. Chaturvedi; M. Chemarin; A. Chen; C. Chen; G. M. Chen; H. F. Chen; H. S. Chen; J. Chen; M. Chen; W. Y. Chen; G. Chiefari; C. Y. Chien; M. Chmeissani; C. Civinni; I. Clare; R. Clare; T. E. Coan; H. O. Cohn; G. Coignet; N. Colino; A. Contin; F. Crijns; X. Y. Cui; T. S. Dai; R. D'Alessandro; R. de Asmundis; A. Degré; K. Deiters; E. Dénes; P. Denes; F. Denotaristefani; M. Dhina; D. Dibitonto; M. Diemoz; H. R. Dimitrov; C. Dionisi; M. T. Dova; E. Drago; T. Driever; D. Duchesneau; P. Duinker; I. Duran; H. El Mamouni; A. Engler; F. J. Eppling; F. C. Erné; P. Extermann; R. Fabbretti; M. Fabre; S. Falciano; Q. Fan; S. J. Fan; O. Fackler; J. Fay; M. Felcini; T. Ferguson; D. Fernandez; G. Fernandez; F. Ferroni; H. Fesefeldt; E. Fiandrini; J. Field; F. Filthaut; G. Finocchiaro; P. H. Fisher; G. Forconi; T. Foreman; K. Freudenreich; W. Friebel; M. Fukushima; M. Gailloud; Yu. Galaktionov; E. Gallo; S. N. Ganguli; P. Garcia-Abia; S. S. Gau; D. Gele; S. Gentile; S. Goldfarb; Z. F. Gong; E. Gonzalez; A. Gordeev; P. Göttlicher; D. Goujon; G. Gratta; C. Grinnell; M. Gruenewald; M. Guanziroli; J. K. Guo; A. Gurtu; H. R. Gustafson; L. J. Gutay; K. Hangarter; A. Hasan; D. Hauschildt; C. T. He; T. Hebbeker; M. Hebert; G. Herten; U. Herten; A. Hervé; K. Hilgers; H. Hofer; H. Hoorani; G. Hu; B. Ille; M. M. Ilyas; V. Innocente; H. Janssen; S. Jezequel; B. N. Jin; L. W. Jones; A. Kasser; R. A. Khan; Yu. Kamyshkov; P. Kapinos; J. S. Kapustinsky; Y. Karyotakis; M. Kaur; S. Khokhar; M. N. Kienzle-Focacci; W. W. Kinnison; D. Kirby; S. Kirsch; W. Kittel; A. Klimentov; A. C. König; O. Kornadt; V. Koutsenko; A. Koulbardis; R. W. Kraemer; T. Kramer; V. R. Krastev; W. Krenz; A. Krovshich; J. Krizmanic; K. S. Kumar; V. Kumar; A. Kunin; G. Landi; K. Lanius; D. Lanske; S. Lanzano; P. Lebrun; P. Lecomte; P. Lecoq; P. Le Coultre; D. M. Lee; I. Leedom; J. M. Le Goff; L. Leistam; R. Leiste; M. Lenti; E. Leonardi; J. Lettry; X. Leytens; C. Li; H. T. Li; J. F. Li; P. J. Li; Q. Li; X. G. Li; J. Y. Liao; W. T. Lin; Z. Y. Lin; F. L. Linde; B. Lindemann; D. Linnhofer; R. Liu; Y. Liu; W. Lohmann; E. Longo; Y. S. Lu; J. M. Lubbers; K. Lübelsmeyer; C. Luci; D. Luckey; L. Ludovici; L. Luminari; W. G. Ma; M. MacDermott; P. K. Malhorta; R. Malik; A. Malinin; C. Maña; D. N. Mao; Y. F. Mao; M. Maolinbay; P. Marchesini; J. P. Martin; L. Martinez-Laso; F. Marzano; G. G. G. Massaro; T. Matsuda; K. Mazumdar; P. McBride; T. McMahon; D. McNally; Th. Meinholz; M. Merk; L. Merola; M. Meschini; W. J. Metzger; Y. Mi; G. B. Mills; Y. Mir; G. Mirabelli; J. Mnich; M. Möller; B. Monteleoni; R. Morand; S. Morganti; N. E. Moulai; R. Mount; S. Müller; A. Nadtochy; E. Nagy; M. Napolitano; H. Newman; C. Neyer; M. A. Niaz; L. Niessen; H. Nowak; G. Organtini; D. Pandoulas; M. Pauluzzi; F. Pauss; G. Passaleva; S. Paoletti; S. Patricelli; Y. J. Pei; D. Perret-Gallix; J. Perrier; A. Pevsner; M. Pieri; P. A. Piroué; F. Plasil; V. Plyaskin; M. Pohl; V. Pojidaev; N. Produit; J. M. Qian; K. N. Qureshi; R. Raghavan; G. Rahal-Callot; G. Raven; P. Razis; K. Read; D. Ren; Z. Ren; M. Rescigno; S. Reucroft; A. Ricker; S. Riemann; O. Rind; H. A. Rizvi; B. P. Roe; M. Röhner; S. Röhner; L. Romero; J. Rose; S. Rosier-Lees; R. Rosmalen; Ph. Rosselet; A. Rubbia; J. A. Rubio; H. Rykaczewski; M. Sachwitz; J. Salicio; G. S. Sanders; A. Santocchia; M. S. Sarakinos; G. Sartorelli; G. Sauvage; A. Savin; V. Schegelsky; K. Schmiemann; D. Schmitz; P. Schmitz; M. Schneegans; H. Schopper; D. J. Schotanus; S. Shotkin; H. J. Schreiber; J. Shukla; R. Schulte; S. Schulte; K. Schultze; J. Schütte; J. Schwenke; G. Schwering; C. Scicca; I. Scott; R. Sehgal; P. G. Seiler; J. C. Sens; L. Servoli; I. Sheer; D. Z. Shen; S. Shevchenko; X. R. Shi; K. Shmakov; E. Shumilov; V. Shoutko; E. Soderstrom; A. Sopczak; C. Spartiotis; T. Spickermann; P. Spillantini; R. Starosta; M. Steuer; D. P. Stickland; F. Sticozzi; H. Stone; K. Strauch

1992-01-01

26

Predicting neutrino parameters from SO(3) family symmetry and quark-lepton unification  

Microsoft Academic Search

We show how the neutrino mixing angles and oscillation phase can be predicted from tri-bimaximal neutrino mixing, corrected by charged lepton mixing angles which are related to quark mixing angles via quark-lepton unification. The tri-bimaximal neutrino mixing can naturally originate from the see-saw mechanism via constrained sequential dominance (CSD), where CSD can result from the vacuum alignment of a non-abelian

Stephen F. King

2005-01-01

27

Abelian family symmetries and the simplest models that give {theta}{sub 13}=0 in the neutrino mixing matrix  

SciTech Connect

I construct predictive models of neutrino mass and mixing that have fewer parameters, both in the lepton sector and overall, than the default seesaw model. The predictions are {theta}{sub 13}=0 and one massless neutrino, with the models having a Z{sub 4} or Z{sub 2} symmetry and just one extra degree of freedom: one real singlet Higgs field. It has been shown that models with an unbroken family symmetry, and with no Higgs fields other than the standard model Higgs doublet produce masses and mixing matrices that have been ruled out by experiment. Therefore, this article investigates the predictions of models with Abelian family symmetries that involve Higgs singlets, doublets and triplets, in the hope that they may produce the maximal and minimal mixing angles seen in the best-fit neutrino mixing matrix. I demonstrate that these models can only produce mixing angles that are zero, maximal or unconfined by the symmetry. The maximal mixing angles do not correspond to physical mixing, so an Abelian symmetry can, at best, ensure that {theta}{sub 13}=0, while leaving the solar and atmospheric mixing angles as free parameters. To generate more features of the best-fit mixing matrix a model with a non-Abelian symmetry and a complicated Higgs sector would have to be used.

Low, Catherine I [School of Physics, Research Centre for High Energy Physics, University of Melbourne, Victoria 3010 (Australia)

2005-04-01

28

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

29

Supporting Low-Income Parents of Young Children: The Palm Beach County Family Study Fourth Annual Report  

ERIC Educational Resources Information Center

The Children's Services Council (CSC) of Palm Beach County funded Chapin Hall at the University of Chicago to conduct a 6-year longitudinal study to examine the use and effectiveness of an array of services in the county in promoting school readiness and school success and improving family functioning among children and families most in need of…

Spielberger, Julie; Rich, Lauren; Winje, Carolyn; Scannell, Molly

2010-01-01

30

Fourth generation parity.  

PubMed

We present a very simple fourth generation (4G) model with an abelian gauge interaction under which only the 4G fermions have nonzero charge. The U(1) gauge symmetry can have a Z2 residual discrete symmetry (4G parity), which can stabilize the lightest 4G particle (L4P). When the 4G neutrino is the L4P, it would be a neutral and stable particle and the other 4G fermions would decay into the L4P, leaving the trace of missing energy plus the standard model fermions. Because of the new symmetry, the 4G particle creation and decay modes are different from those of the sequential 4G model, and the 4G particles can be appreciably lighter than typical experimental bounds. PMID:23383889

Lee, Hye-Sung; Soni, Amarjit

2013-01-11

31

Lepton sector of a fourth generation  

SciTech Connect

In extensions of the standard model with a heavy fourth generation, one important question is what makes the fourth-generation lepton sector, particularly the neutrinos, so different from the lighter three generations. We study this question in the context of models of electroweak symmetry breaking in warped extra dimensions, where the flavor hierarchy is generated by choosing the localization of the zero-mode fermions in the extra dimension. In this setup the Higgs sector is localized near the infrared brane, whereas the Majorana mass term is localized at the ultraviolet brane. As a result, light neutrinos are almost entirely Majorana particles, whereas the fourth-generation neutrino is mostly a Dirac fermion. We show that it is possible to obtain heavy fourth-generation leptons in regions of parameter space where the light neutrino masses and mixings are compatible with observation. We study the impact of these bounds, as well as the ones from lepton flavor violation, on the phenomenology of these models.

Burdman, G. [Fermi National Accelerator Laboratory, Batavia, Illinois 60510 (United States); Instituto de Fisica, Universidade de Sao Paulo, Sao Paulo (Brazil); Da Rold, L. [Centro Atomico Bariloche, Bariloche (Argentina); Matheus, R. D. [Instituto de Fisica, Universidade de Sao Paulo, Sao Paulo (Brazil)

2010-09-01

32

Neutrino mixing effects, ? leptonic decays, and the solar-neutrino problem.  

NASA Astrophysics Data System (ADS)

It is assumed that a heavy right-handed Majorana neutrino which is a weak SU(2) singlet exists and its mixing with regular neutrinos causes a Cabibbo - Kobayashi - Maskawa - type matrix. This mixing effect may interpret some problems in ? leptonic decays. To be consistent with the requirements from both the seesaw mechanism and data on Z0 decay, the fourth generation with a heavy neutrino is needed. This also possibly provides a large destructive interference between contributions of magnetic moments of the electron neutrino and ? neutrino to explain away the puzzle about the deficiency of the solar neutrino flux.

Xu, Lieqian; Tao, Zhijian

1991-06-01

33

Neutrino mixing effects,. tau. leptonic decays, and the solar-neutrino problem  

SciTech Connect

It is assumed that a heavy right-handed Majorana neutrino (or more) which is a weak SU(2) singlet exists and its mixing with regular neutrinos causes a Cabibbo-Kobayashi-Maskawa-type matrix. This mixing effect may interpret some problems in {tau} leptonic decays. To be consistent with the requirements from both the seesaw mechanism and data on {ital Z}{sup 0} decay, the fourth generation with a heavy neutrino is needed. This also possibly provides a large destructive interference between contributions of magnetic moments of the electron neutrino and {tau} neutrino to explain away the puzzle about the deficiency of the solar-neutrino flux.

Li, X. (Center of Theoretical Physics, Chinese Center of Advanced Science Technology (World Laboratory), P.O. Box 8730, Beijing, China (CN) Physics Department, Nankai University, Tianjin, China); Tao Zhi-jian (Center of Theoretical Physics, Chinese Center of Advanced Science Technology (World Laboratory), P.O. Box 8730, Beijing, China Institute of Theoretical Physics, Academia Sinica, Beijing, China)

1991-06-01

34

Neutrino mixing effects, ? leptonic decays, and the solar-neutrino problem  

NASA Astrophysics Data System (ADS)

It is assumed that a heavy right-handed Majorana neutrino (or more) which is a weak SU(2) singlet exists and its mixing with regular neutrinos causes a Cabibbo-Kobayashi-Maskawa-type matrix. This mixing effect may interpret some problems in ? leptonic decays. To be consistent with the requirements from both the seesaw mechanism and data on Z0 decay, the fourth generation with a heavy neutrino is needed. This also possibly provides a large destructive interference between contributions of magnetic moments of the electron neutrino and ? neutrino to explain away the puzzle about the deficiency of the solar-neutrino flux.

Li, Xue-Qian; Zhi-Jian, Tao

1991-06-01

35

Cosmic Neutrinos  

SciTech Connect

I recall the place of neutrinos in the electroweak theory and summarize what we know about neutrino mass and flavor change. I next review the essential characteristics expected for relic neutrinos and survey what we can say about the neutrino contribution to the dark matter of the Universe. Then I discuss the standard-model interactions of ultrahigh-energy neutrinos, paying attention to the consequences of neutrino oscillations, and illustrate a few topics of interest to neutrino observatories. I conclude with short comments on the remote possibility of detecting relic neutrinos through annihilations of ultrahigh-energy neutrinos at the Z resonance.

Quigg, Chris; /Fermilab /CERN

2008-02-01

36

Neutrinos:. Theory  

NASA Astrophysics Data System (ADS)

These lectures are a theoretical introduction to the phenomenology of massive neutrinos. First I will present the low energy formalism for adding neutrino masses to the Standard Model and the induced leptonic mixing, and then I will describe the phenomenology associated with neutrino oscillations in vacuum and in matter. I will also comment on the laboratory probes of the absolute neutrino mass scale. Finally I will briefly describe some possible collider signatures associated to neutrino mass models.

Gonzalez-Garcia, M. C.

2010-08-01

37

Neutrino tomography  

NASA Astrophysics Data System (ADS)

Neutrinos are produced in weak interactions as states with definite flavor--electron, muon, or tau--and these flavor states are superpositions of states of different mass. As a neutrino propagates through space, the different mass eigenstates interfere, resulting in time-dependent flavor oscillation. Though matter is transparent to neutrinos, the flavor oscillation probability is modified when neutrinos travel through matter. Herein, we present an introduction to neutrino propagation through matter in a manner accessible to advanced undergraduate students. As an interesting application, we consider neutrino propagation through matter with a piecewise-constant density profile. This scenario has relevance in neutrino tomography, in which the density profile of matter, like the Earth's interior, can be probed via a broad-spectrum neutrino beam. We provide an idealized example to demonstrate the principle of neutrino tomography.

Millhouse, Margaret A.; Latimer, David C.

2013-09-01

38

Rapid detection of mutations by conformation sensitive gel electrophoresis: Application to the identification of three new mutations in the type II procollagen gene and a fourth family with the Arg{sub 519}{yields}Cys base substitution  

SciTech Connect

Conformation sensitive gel electrophoresis (CSGE) detects differences as small as a single base mismatch in DNA heteroduplexes of polymerase chain reaction (PCR) products. The altered migration of heteroduplexes versus homoduplexes is resolved in a polyacrylamide-based gel electrophoresis system. The technique was used here to detect conformational changes in the type II procollagen gene (COL2A1) in patients with growth plate defects. PCR products which displayed heteroduplex species were directly sequenced and all revealed either base substitutions or base deletions. Three of the base substitutions resulted in the identification of new mutations. These include a Gly{sub 691}{yields}Arg substitution in a proband with hypochondrogenesis, a Gly{sub 975}{yields}Ser base substitution in a family with late-onset spondyloepiphyseal dysplasia (SEDT) and precocious osteoarthritis (POA), and a Gly{sub 988}{yields}Arg mutation in another patient with hypochondrogenesis. A fourth substitution was found to be the fourth example of an Arg{sub 519}{yields}Cys point mutation in a family with SEDT and POA. All mutations were confirmed by restriction site analysis. These results illustrate the utility of the CSGE method for the rapid detection of mutations in PCR products without the need for special equipment, primers or sample preparation.

Williams, C.J.; Rock, M.; McCarron, S. [Thomas Jefferson Univ., Philadelphia, PA (United States)] [and others

1994-09-01

39

Family Child Care Calendar-Keeper[TM] 2001: A Record Keeping System Including Nutrition Information for Child Care Providers. Twenty-Fourth Edition.  

ERIC Educational Resources Information Center

Noting that accurate recordkeeping for tax purposes is extremely important for family child care providers, this calendar provides a format for recording typical family child care expenses and other information. Included are the following: (1) monthly expense charts with categories matching Schedule C; (2) attendance and payment log; (3) payment…

Beuch, Beth, Ed.; Beuch, Ethel, Ed.; Schloff, Pam, Ed.

40

Neutrino Telescopes  

SciTech Connect

We review the present status of high energy neutrino astronomy. The advantages of neutrinos as extra-terrestrial messengers are recalled and their possible extra-terrestrial sources examined. We review as well the status of present and future neutrino telescopes and summarize the results obtained so far in this field.

Hernandez-Rey, Juan Jose [IFIC - Instituto de Fisica Corpuscular, C.S.I.C. - Universitat de Valencia, E-46071, Valencia (Spain)

2006-11-28

41

Neutrino oscillations in a predictive SUSY GUT  

NASA Astrophysics Data System (ADS)

In this paper we present a predictive SO(10) supersymmetric grand unified theory with the family symmetry U(2)×U(1) which has several nice features. We are able to fit fermion masses and mixing angles, including recent neutrino data, with nine parameters in the charged fermion sector and four in the neutrino sector. The family symmetry plays a preeminent role. (i) The model is ``natural''-we include all terms allowed by the symmetry. It restricts the number of arbitrary parameters and enforces many zeros in the effective mass matrices. (ii) Family symmetry breaking from U(2)×U(1)-->U(1)--> nothing generates the family hierarchy. It also constrains squark and slepton mass matrices, thus ameliorating flavor violation resulting from squark and slepton loop contributions. (iii) It naturally gives large angle ??-?? mixing describing atmospheric neutrino oscillation data and small angle ?e-?s mixing, consistent with the small mixing angle Mikheyev-Smirnov-Wolfenstein (MSW) solution to solar neutrino data. (iv) Finally, in this paper we assume minimal family symmetry-breaking vacuum expectation values (VEV's). As a result we cannot obtain a three neutrino solution to both atmospheric and solar neutrino oscillations. In addition, the solution discussed here cannot fit liquid scintillation neutrino detector (LSND) data even though this solution requires a sterile neutrino ?s. It is important to note, however, that with nonminimal family symmetry-breaking VEV's, a three neutrino solution is possible with the small mixing angle MSW solution to solar neutrino data and large angle ??-?? mixing describing atmospheric neutrino oscillation data. In the four neutrino case, nonminimal family VEV's may also permit a solution for LSND. The results with nonminimal family breaking are still under investigation and will be reported in a future paper.

Blažek, T.; Raby, S.; Tobe, K.

1999-12-01

42

Primordial Neutrinos  

NASA Astrophysics Data System (ADS)

This review discusses in detail the connection between cosmological observations and neutrino physics. Neutrinos decouple from thermal contact in the early universe at a temperature of order 1 MeV, which coincides with the temperature at which light-element synthesis occurs. Observations of light-element abundances therefore provide important information about properties such as neutrino energy density and chemical potential. Precision observations of the cosmic microwave background and large-scale structure of galaxies can be used to probe neutrino masses with greater precision than current laboratory experiments. This review discusses current cosmological bounds on neutrino properties, as well as possible bounds from upcoming measurements.

Hannestad, Steen

2006-11-01

43

Neutrino factories  

NASA Astrophysics Data System (ADS)

The discovery of neutrino oscillations marks a major milestone in the history of neutrino physics, and opens a window to what lies beyond the Standard Model. Many current and forthcoming experiments will answer open questions; however, a major step forward, up to and possibly including CP violation in the neutrino mixing matrix, will be offered by the neutrino beams from a neutrino factory. The neutrino factory is a new concept for producing neutrino beams of unprecedented quality in terms of intensity, flavour composition, and precision of the beam parameters. These beams enable the exploration of otherwise inaccessible domains in neutrino oscillation physics by exploiting baselines of planetary dimensions. Suitable detectors pose formidable challenges but seem within reach with only moderate extrapolations from existing technologies. Although the main physics attraction of the neutrino factory is in the area of neutrino oscillations, an interesting spectrum of further opportunities ranging from high-precision, high-rate neutrino scattering to physics with high-intensity stopped muons comes with it.

Dydak, F.

2002-07-01

44

Neutrino counting with the SLD at the Stanford Linear Collider  

SciTech Connect

One of the fundamental measurements to be made at the e/sup +/e/sup /minus// colliders, SLC and LEP, is the determination of the number of neutrino families produced in Z/sup 0/ boson decays. In the event that a fourth generation of light Dirac neutrinos exists, the experimental consequences at the Z/sup 0/ resonances are easily seen; the total width will be increased by 171 MeV over its three generation value, to be compared to the /approx/30 MeV precision that should be achievable once the systematic limit has been reached. A reasonable figure of merit for the precision of a neutrino counting measurement of 0.2 standard model generations corresponds to a Z/sup 0/ width measurement error of 35 MeV; close to the limit of anticipated experimental capability. In fact, it is highly desirable to achieve an even higher precision if possible, in order to distinguish potentially small effects due to exotic phenomena from beyond the Standard Model. This paper will address the issue of how to obtain the best measurement of the number of neutrino generations as a function of the size of the available sample of Z/sup 0/ decays. The results presented here were obtained by our study group in an attempt to understand the limitations of a realistic neutrino counting measurement with the SLD at the Stanford Linear Collider. However, many of our findings are general enough to be applicable to any e/sup +/e/sup /minus// detector designed to take data at the Z/sup 0/ resonance. 19 refs., 5 figs., 6 tabs.

Band, H.; Bugg, W.; Chadwick, G.; Coyne, D.; Gyure, M.; Hertzbach, S.; Messner, R.; Mincer, A.; Mockett, P.; Nauenberg, U.

1989-06-01

45

Neutrino mass matrices with a democratic texture  

SciTech Connect

The structure of the neutrino mass matrices is investigated, in a scheme where the minimal three-family Standard Model is extended by including right-handed neutrinos. No assumption is made about the presence of a large mass scale, like in the see-saw scheme. Certain peculiar features of the usual democratic mass matrix are investigated, and used to define matrices with a 'democratic texture'. By demanding that the neutrino mass matrices have a specific form with such a democratic texture, Majorana mass spectra with three massless (light) neutrinos and either two or three massive neutrinos, are obtained.

Kleppe, A. [Dep. of Mathematical Physics, LTH, Box 118, 22100 Lund (Sweden)

1997-06-15

46

A theoretical perspective on neutrino physics  

SciTech Connect

A survey of sin{sup 2} {theta}{sub W}, {rho}, CKM matrix, and axial-isoscalar neutral current measurements via neutrino scattering is presented. Loop effects due to heavy top or a fourth generation are described. Neutrino oscillations are discussed in a three generation mixing framework and some motivation for {nu}{sub {mu}} {yields} {nu}{sub {tau}} oscillation searches is given. 15 refs., 1 tab.

Marciano, W.J. (Brookhaven National Lab., Upton, NY (USA))

1989-09-01

47

Neutrino mass  

SciTech Connect

The existence of a finite neutrino mass would have important consequences in particle physics, astrophysics, and cosmology. Experimental sensitivities have continued to be pushed down without any confirmed evidence for a finite neutrino mass. Yet there are several observations of discrepancies between theoretical predictions and observations which might be possible indications of a finite neutrino mass. Thus, extensive theoretical and experimental work is underway to resolve these issues.

Bowles, T.J.

1994-04-01

48

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.

49

Search for Majorana Neutrinos in B-??+?-?- Decays  

NASA Astrophysics Data System (ADS)

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.

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, Th.; 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, Ch.; Cenci, R.; Charles, M.; Charpentier, Ph.; 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, Ch.; 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, Ph.; 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, Yu.; 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.

2014-04-01

50

Neutrinos:. Windows to Planck Physics  

NASA Astrophysics Data System (ADS)

After recalling some elegant contributions of the late Freydoon Mansouri, we turn to neutrino physics and use a modicum of grand unification to relate quark and lepton mixing matrices. We advocate an expansion for the MNS matrix, à la Wolfenstein, and argue that in a wide class of models, ?13 is a Cabibbo mixing effect. Also the large neutrino mixing angles reflect the mass patterns of the right-handed neutrinos near the Planck scale, and provide evidence for family structure at that scale.

Ramond, P.

2004-10-01

51

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

52

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

53

Neutrino clouds.  

National Technical Information Service (NTIS)

We consider the possibility that neutrinos are coupled very weakly to an extremely light scalar boson. We first analyze the simple problem of one generation of neutrino and show that, for ranges of parameters that are allowed by existing data, such a syst...

G. J. Stephenson T. Goldman B. H. J. McKellar

1997-01-01

54

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

55

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

56

Neutrinos Today.  

National Technical Information Service (NTIS)

After the famous 1983 discovery of intermediate W, Z/sup 0/ bosons, it may be stated with certainty that W, Z/sup 0/ are entirely responsible for the production of neutrinos and for their interactions. Neutrino physics notions are presented from this poin...

B. Pontecorvo S. Bilen'kij

1987-01-01

57

A fourth polymorph in the family of BEDT-TTF salts with thiocyanatocuprate(I) anions: (BEDT-TTF){<_4}Cu{<_3}(NCS){<_5}.  

SciTech Connect

A new crystallographic modification was found in the family of BEDT-TTF salts containing thiocyanatocuprate(I) anions. The cation radical salt crystallizes in the P{sup {bar 1}} space group with a = 8.2720(9) {angstrom}, b = 19.099(2) {angstrom}, c = 43.758(5) {angstrom}, {alpha} = 81.088(4){sup o}, {beta} = 87.253(4){sup o}, {gamma} = 83.790(4){sup o}, V = 6786.2(13) {angstrom}{sup 3} at 150 K. The BEDT-TTF radical cations pack in an {alpha}-type motif, but every four columns, there is a slip in the layer. Where this slip occurs, the stacks are coupled in a {beta}'' manner. The material exhibits semiconductive behavior with an activation energy of 0.13 eV above 250 K and 0.22 eV below. Packing motif of the (BEDT-TTF){sub 4}Cu{sub 3}(NCS){sub 5} structure.

Schlueter, J. A.; Geiser, U.; Wang, H. H.; Manson, J. L. (Materials Science Division); (Eastern Washington Univ.)

2012-05-01

58

Neutrino mixing effects, tau leptonic decays, and the solar-neutrino problem  

Microsoft Academic Search

It is assumed that a heavy right-handed Majorana neutrino (or more) which is a weak SU(2) singlet exists and its mixing with regular neutrinos causes a Cabibbo-Kobayashi-Maskawa-type matrix. This mixing effect may interpret some problems in tau leptonic decays. To be consistent with the requirements from both the seesaw mechanism and data on Z0 decay, the fourth generation with a

Xue-Qian Li; Tao Zhi-Jian

1991-01-01

59

The Fourth Grader.  

ERIC Educational Resources Information Center

Profiles typical characteristics and behaviors of fourth graders. Highlights physical development, including energy and growth, motor development, physical activities, and health; mental development, including Piagetian stages, academic development, mental limitations, and effective classroom rewards; and psychosocial development, including…

Howe, Frederick C.

1993-01-01

60

Electronics: The fourth element  

Microsoft Academic Search

Almost four decades since its existence was first proposed, a fourth basic circuit element joins the canonical three. The 'memristor' might herald a step-change in the march towards ever more powerful circuitry.

James M. Tour; Tao He

2008-01-01

61

Testing the Reactor and Gallium Anomalies with Intense (Anti)Neutrino Emitters  

NASA Astrophysics Data System (ADS)

Several observed anomalies in neutrino oscillation data could be explained by a hypothetical fourth neutrino separated from the three standard neutrinos by a squared mass difference of a few 0.1 eV or more. This hypothesis can be tested with MCi neutrino electron capture sources (51Cr) or kCi antineutrino ?-source (144Ce) deployed inside or next to a large low background neutrino detector. In particular, the compact size of this source coupled with the localization of the interaction vertex lead to an oscillating pattern in event spatial (and possibly energy) distributions that would unambiguously determine neutrino mass differences and mixing angles.

Lasserre, Thierry

2013-02-01

62

Implications of new generations on neutrino masses  

NASA Astrophysics Data System (ADS)

We explore the possible implications that new families, that are being searched for at the LHC, would have on neutrino masses. In particular, we have explored the possibility that the smallness of the observed neutrino masses is naturally understood in a modified version of the Standard Model (SM) with complete extra generations of fermions, i.e., that have right-handed neutrinos, in which neutrino masses are generated at two loops. With one extra family it is not possible to fit the observed spectrum of masses and mixings. However, the radiative mass generated provides an important constraint in these kind of models, so the neutrino masses do not exceed their cosmological bound. Within the context of two extra families, we analyse the allowed parameter space and the possible phenomenological signals.

Aparici, A.; Herrero-Garcia, J.; Rius, N.; Santamaria, A.

2013-02-01

63

Underground Neutrino Astronomy.  

National Technical Information Service (NTIS)

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 s...

D. N. Schramm

1983-01-01

64

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.

65

Discriminating neutrino see-saw models  

NASA Astrophysics Data System (ADS)

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.

Hirsch, M.; King, S. F.

2001-09-01

66

Crossing the fourth hurdle  

PubMed Central

The fourth hurdle, the requirement that pharmaceutical manufacturers can demonstrate that their new products represent good value for money as well as being of good quality, effective and safe, is increasingly being required by healthcare systems. In crossing this ‘fourth’ hurdle, companies will usually need to demonstrate that their products are more effective than relevant comparators and that the increased cost is offset by the enhanced benefits. Decision makers, however, must draw their conclusions not only on the basis of the underpinning science but also on the social values of the people they serve.

Rawlins, Michael D

2012-01-01

67

Crossing the fourth hurdle.  

PubMed

The fourth hurdle, the requirement that pharmaceutical manufacturers can demonstrate that their new products represent good value for money as well as being of good quality, effective and safe, is increasingly being required by healthcare systems. In crossing this 'fourth' hurdle, companies will usually need to demonstrate that their products are more effective than relevant comparators and that the increased cost is offset by the enhanced benefits. Decision makers, however, must draw their conclusions not only on the basis of the underpinning science but also on the social values of the people they serve. PMID:22404227

Rawlins, Michael D

2012-06-01

68

Fourth goal of perinatal medicine.  

PubMed Central

Reduction in maternal mortality, infant mortality, and infant morbidity have been successively the goals of perinatal medicine. The fourth is to reduce bonding failure. In July 1978 a preventive service was started in the John Radcliffe Maternity Hospital. A twice-weekly round is made. Midwives refer families who cause them concern. In the first year the referral rate ws 20.5 per 1000 liveborn babies. The referred sample differed from the hospital population in terms of maternal psychiatric history, marital state and babies' admission to special care. The main reasons for referral were: doubt about parenting ability (27%), psychiatric history (15%), disturbed behaviour in hospital (14%), and diffuse social and medical problems (17%). Long-term care was needed for only 14% of families. At their first birthdays, six babies were placed away from their natural parents; the sample had had a slightly higher than expected admission rate to hospital; the distribution of weights did not differ from the expected; doctors and health visitors were still concerned about one-quarter of the families. Seven cases of screening failure were found among those not referred to our service, but only one was seriously abused. No child referred in the first year has been seriously neglected or abused.

Ounsted, C; Roberts, J C; Gordon, M; Milligan, B

1982-01-01

69

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

70

Fourth Grade Lab Activities  

NSDL National Science Digital Library

These are a collection of sites related to the Fourth Grade CORE, to be explored in the computer lab. For SCIENCE explorations click below. 1. Clouds and the water cycle at the Enchanted Learning site. 2. Look at the Cloud Man&s pictures of clouds. 3. Cloud Types 4. Clouds and Precipitation: online meteorology guide 5. The Dirt on Soil 6. The Dirt on Soil 7. Soil Horizons For MATH activities click below. Math activities "A" ...

Boissonnault, Ms.

2005-06-23

71

Linearizing neutrino evolution equations including ??¯ pairing correlations  

NASA Astrophysics Data System (ADS)

We linearize the neutrino mean-field evolution equations describing the neutrino propagation in a background of matter and of neutrinos, using techniques from many-body microscopic approaches. The procedure leads to an eigenvalue equation that allows us to identify instabilities in the evolution, associated with a change of the curvature of the neutrino energy-density surface. Our result includes all contributions from the neutrino Hamiltonian and is generalizable to linearize the equations of motion at an arbitrary point of the evolution. We then consider the extended equations that comprise the normal mean field as well as the abnormal mean field that is associated with neutrino-antineutrino pairing correlations. We first rederive the extended neutrino Hamiltonian and show that such a Hamiltonian can be diagonalized by introducing a generalized Bogoliubov-Valatin transformation with quasiparticle operators that mix neutrinos and antineutrinos. We give the eigenvalue equations that determine the energies of the quasiparticle eigenstates. Finally we derive the eigenvalue equation of the extended equations of motion, valid in the small amplitude approximation. Our results apply to an arbitrary number of neutrino families.

Väänänen, Daavid; Volpe, Cristina

2013-09-01

72

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

73

Neutrino magnetic moment  

SciTech Connect

We review attempts to achieve a large neutrino magnetic moment ({mu}{sub {nu}} {le} 10{sup {minus}11}{mu}{sub B}), while keeping neutrino light or massless. The application to the solar neutrino puzzle is discussed. 24 refs.

Chang, D. (Northwestern Univ., Evanston, IL (USA). Dept. of Physics and Astronomy Fermi National Accelerator Lab., Batavia, IL (USA)); Senjanovic, G. (Zagreb Univ. (Yugoslavia). Dept. of Theoretical Physics)

1990-01-01

74

Neutrino masses and solar neutrinos.  

National Technical Information Service (NTIS)

It has been pointed out by Bahcall and Bethe and others that all solar neutrino data can be explained by MSW oscillations with m((nu)(sub (mu))) (approximately) 10(sup (minus)3) eV consistent with ideas grand unified theories (GUTS). There is a second pos...

L. Wolfenstein

1992-01-01

75

First Neutrino Point-Source Results from the 22 String Icecube Detector  

Microsoft Academic Search

We present new results of searches for neutrino point sources in the northern sky, using data recorded in 2007-2008 with 22 strings of the IceCube detector (approximately one-fourth of the planned total) and 275.7 days of live time. The final sample of 5114 neutrino candidate events agrees well with the expected background of atmospheric muon neutrinos and a small component

R. Abbasi; Y. Abdou; M. Ackermann; J. Adams; J. Aguilar; K. Andeen; J. Auffenberg; X. Bai; M. Baker; S. W. Barwick; R. Bay; J. L. Bazo Alba; K. Beattie; J. J. Beatty; S. Bechet; J. K. Becker; K.-H. Becker; M. L. Benabderrahmane; J. Berdermann; P. Berghaus; D. Berley; E. Bernardini; D. Bertrand; D. Z. Besson; M. Bissok; E. Blaufuss; D. J. Boersma; C. Bohm; J. Bolmont; S. Böser; O. Botner; L. Bradley; J. Braun; D. Breder; T. Castermans; D. Chirkin; B. Christy; J. Clem; S. Cohen; D. F. Cowen; M. V. D'Agostino; M. Danninger; C. T. Day; C. De Clercq; L. Demirörs; O. Depaepe; F. Descamps; P. Desiati; G. de Vries-Uiterweerd; T. De Young; J. C. Diaz-Velez; J. Dreyer; J. P. Dumm; M. R. Duvoort; W. R. Edwards; R. Ehrlich; J. Eisch; R. W. Ellsworth; O. Engdegård; S. Euler; P. A. Evenson; O. Fadiran; A. R. Fazely; T. Feusels; K. Filimonov; C. Finley; M. M. Foerster; B. D. Fox; A. Franckowiak; R. Franke; T. K. Gaisser; J. Gallagher; R. Ganugapati; L. Gerhardt; L. Gladstone; A. Goldschmidt; J. A. Goodman; R. Gozzini; D. Grant; T. Griesel; A. Groß; S. Grullon; R. M. Gunasingha; M. Gurtner; C. Ha; A. Hallgren; F. Halzen; K. Han; K. Hanson; Y. Hasegawa; J. Heise; K. Helbing; P. Herquet; S. Hickford; G. C. Hill; K. D. Hoffman; K. Hoshina; D. Hubert; W. Huelsnitz; J.-P. Hülß; P. O. Hulth; K. Hultqvist; S. Hussain; R. L. Imlay; M. Inaba; A. Ishihara; J. Jacobsen; G. S. Japaridze; H. Johansson; J. M. Joseph; K.-H. Kampert; A. Kappes; T. Karg; A. Karle; J. L. Kelley; P. Kenny; J. Kiryluk; F. Kislat; S. R. Klein; S. Klepser; S. Knops; G. Kohnen; H. Kolanoski; L. Köpke; M. Kowalski; T. Kowarik; M. Krasberg; K. Kuehn; T. Kuwabara; M. Labare; S. Lafebre; K. Laihem; H. Landsman; R. Lauer; H. Leich; D. Lennarz; A. Lucke; J. Lundberg; J. Lünemann; J. Madsen; P. Majumdar; R. Maruyama; K. Mase; H. S. Matis; C. P. McParland; K. Meagher; M. Merck; P. Mészáros; E. Middell; N. Milke; H. Miyamoto; A. Mohr; T. Montaruli; R. Morse; S. M. Movit; K. Münich; R. Nahnhauer; J. W. Nam; P. Nießen; D. R. Nygren; S. Odrowski; A. Olivas; M. Olivo; M. Ono; S. Panknin; S. Patton; C. Pérez de los Heros; J. Petrovic; A. Piegsa; D. Pieloth; A. C. Pohl; R. Porrata; N. Potthoff; P. B. Price; M. Prikockis; G. T. Przybylski; K. Rawlins; P. Redl; E. Resconi; W. Rhode; M. Ribordy; A. Rizzo; J. P. Rodrigues; P. Roth; F. Rothmaier; C. Rott; C. Roucelle; D. Rutledge; D. Ryckbosch; H.-G. Sander; S. Sarkar; K. Satalecka; S. Schlenstedt; T. Schmidt; D. Schneider; A. Schukraft; O. Schulz; M. Schunck; D. Seckel; B. Semburg; S. H. Seo; Y. Sestayo; S. Seunarine; A. Silvestri; A. Slipak; G. M. Spiczak; C. Spiering; M. Stamatikos; T. Stanev; G. Stephens; T. Stezelberger; R. G. Stokstad; M. C. Stoufer; S. Stoyanov; E. A. Strahler; T. Straszheim; K.-H. Sulanke; G. W. Sullivan; Q. Swillens; I. Taboada; O. Tarasova; A. Tepe; S. Ter-Antonyan; C. Terranova; S. Tilav; M. Tluczykont; P. A. Toale; D. Tosi; D. Turcan; N. van Eijndhoven; J. Vandenbroucke; A. Van Overloop; B. Voigt; C. Walck; T. Waldenmaier; M. Walter; C. Wendt; S. Westerhoff; N. Whitehorn; C. H. Wiebusch; A. Wiedemann; G. Wikström; D. R. Williams; R. Wischnewski; H. Wissing; K. Woschnagg; X. W. Xu; G. Yodh

2009-01-01

76

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

77

Neutrinos: Recent Developments  

SciTech Connect

Certainly one of the most exciting areas of research at present is neutrino physics. The neutrinos are fantastically numerous in the universe and as such they have bearing on our understanding of the universe. Therefore, we must understand the neutrinos, particularly their mass. There is compelling evidence from solar and atmospheric neutrinos and those from reactors for neutrino oscillations implying that neutrinos mix and have nonzero mass but without pinning down their absolute mass. This is reviewed. The implications of neutrino oscillations and mass squared splitting between neutrinos of different flavor on pattern of neutrino mass matrix is discussed. In particular, a neutrino mass matrix, which shows approximate flavor symmetry where the neutrino mass differences arise from flavor violation in off-diagonal Yukawa couplings is elaborated on. The implications in double beta decay are also discussed.

Riazuddin [National Center for Physics, Quaid-i-Azam University, Islamabad 45320 (Pakistan)

2005-03-17

78

Neutrino in Cosmology  

NASA Astrophysics Data System (ADS)

The relic neutrinos from the Big Bang or the Cosmic Neutrino Background (CNB) neutrinos are expected to be the most abundant particles in our universe after the relic photons of the Cosmic Microwave Background (CMB). They carry precious information from the early epoch when our universe was only 1 sec old. Although not yet directly detected, CNB may be revealed indirectly through cosmological observations due to their important cosmological influence. I review the cosmological role of neutrinos and the present cosmological constraints on neutrino characteristics. Namely, I discuss the impact of neutrinos in the cosmic expansion, neutrino decoupling, the role of neutrinos in the primordial production of light elements, their effect on CMB anisotropies, LSS formation, the possible neutrino contribution to the Dark Matter in the universe, leptogenesis, etc. Due to the considerable cosmological influence of neutrinos, cosmological bounds on neutrino properties from observational data exist. I review the cosmological constraints on the neutrino characteristics, such as the effective number of neutrino species, neutrino mass and mixing parameters, lepton number of the universe, gravitational clustering of neutrinos, presence of sterile neutrino, etc.

Kirilova, D.

2010-09-01

79

Nonaccelerator neutrino physics  

NASA Astrophysics Data System (ADS)

The subject of these lectures is experimental nonaccelerator neutrino physics. We discuss experiments on solar and atmospheric neutrino flux measurements, as well as experiments devoted to recording the antineutrino on nuclear reactors in the context of determining the parameters of neutrino oscillations. Neutrino geophysics, a new field of science, is overviewed.

Smirnov, O. Yu.

2012-12-01

80

Neutrino - Link Between the Microcosmos and the Macrocosmos, a Study in Two Parts: (1) Theoretical - Look at the Tau Neutrino Mass and Other Quantum Electrodynamical Effects in Third Family Lepton Interactions and (2) Experimental - Astronomy in Hawai'i, the Short Prototype String of the Deep Underwater Muon and Neutrino Detector Project (hawaii)  

Microsoft Academic Search

The nineteen eighties has been a time in which Cosmology and Particle Physics have come together. This dissertation reflects that trend. It does so in two ways. First, in Chapters 1 through 3, there is a theoretical investigation into some aspects of generational universality. The consequences of a third lepton, namely the tauon, and an associated tau neutrino, are explored

John Freeman Babson

1989-01-01

81

Neutrino physics-the link between the microcosmos and the macrocosmos, a study in two parts: (1) Theoretical-a look at the tau neutrino mass and other quantum electrodynamical effects in third family lepton interactions and (2) Experimental-underwater astronomy in Hawai'i, the short prototype string of the Deep Underwater Muon and Neutrino Detector project  

Microsoft Academic Search

The nineteen eighties has been a time in which Cosmology and Particle Physics have come together. This dissertation reflects that trend. It does so in two ways. First, in Chapters 1 through 3, there is a theoretical investigation into some aspects of generational universality. The consequences of a third lepton, namely the tauon, and an associated tau neutrino, are explored

Babson

1989-01-01

82

Future Neutrino Experiments  

SciTech Connect

There are a number of future neutrino experiments addressing fundamental questions about the neutrino and about what the neutrino can tell us about the universe. A class of these experiments are long baseline neutrino oscillation v{sub e} appearance searches which can measure the final unknowns of the 3x3 neutrino mixing matrix and look for CP violation in the neutrino sector. The massive detectors needed for these experiments can also search for proton decay and measure extra-terrestrial neutrino sources. There are a number of efforts worldwide to launch these experiments. These efforts, with a focus on US plans, are described.

Fleming, B. T. [Physics Department, Yale University, New Haven, CT 60510 (United States)

2009-12-17

83

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

84

Tachyonic neutrinos and the neutrino masses  

NASA Astrophysics Data System (ADS)

With a recent claim of superluminal neutrinos shown to be in error, 2012 may not be a propitious time to consider the evidence that one or more neutrinos may indeed be tachyons. Nevertheless, there are a growing number of observations that continue to suggest this possibility - albeit with an m?2<0 having a much smaller magnitude than was implied by the original OPERA claim. One recently published non-standard analysis of SN 1987A neutrinos supports a tachyonic mass eigenstate, and here we show how it leads to 3 + 3 mirror neutrino model having an unconventional mass hierarchy. The model incorporates one superluminal active-sterile neutrino pair, and it is testable in numerous ways, including making a surprising prediction about an unpublished aspect of the SN 1987A neutrinos. Additional supporting evidence involving earlier analyses of cosmic rays is summarized to add credence to the tachyonic neutrino hypothesis.

Ehrlich, Robert

2013-01-01

85

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

86

Predictive model of radiative neutrino masses  

NASA Astrophysics Data System (ADS)

We present a simple and predictive model of radiative neutrino masses. It is a special case of the Zee model which introduces two Higgs doublets and a charged singlet. We impose a family-dependent Z4 symmetry acting on the leptons, which reduces the number of parameters describing neutrino oscillations to four. A variety of predictions follow: the hierarchy of neutrino masses must be inverted; the lightest neutrino mass is extremely small and calculable; one of the neutrino mixing angles is determined in terms of the other two; the phase parameters take CP-conserving values with ?CP=?; and the effective mass in neutrinoless double beta decay lies in a narrow range, m??=(17.6-18.5) meV. The ratio of vacuum expectation values of the two Higgs doublets, tan?, is determined to be either 1.9 or 0.19 from neutrino oscillation data. Flavor-conserving and flavor-changing couplings of the Higgs doublets are also determined from neutrino data. The nonstandard neutral Higgs bosons, if they are moderately heavy, would decay dominantly into ? and ? with prescribed branching ratios. Observable rates for the decays ? ?e? and ??3? are predicted if these scalars have masses in the range of 150-500 GeV.

Babu, K. S.; Julio, J.

2014-03-01

87

Inverted hierarchy models of neutrino masses  

NASA Astrophysics Data System (ADS)

We study models of neutrino masses which naturally give rise to an inverted mass hierarchy and bi-maximal mixing. The models are based on the see-saw mechanism with three right-handed neutrinos, which generates a single mass term of the form ? e(? ?+? ?) corresponding to two degenerate neutrinos ? e and ? ?+? ?, and one massless neutrino ? ?-? ?. Atmospheric neutrino oscillations are accounted for if the degenerate mass term is about 5×10 -2 eV. Solar neutrino oscillations of the Large Mixing Angle MSW type arise when small perturbations are included leading to a mass splitting between the degenerate pair of about (1.7 -2.0)×10 -4 eV for the successful cases. We study the conditions that such models must satisfy in the framework of a U(1) chiral family symmetry broken by a pair of scalar singlets with vector-like charges, and catalogue the simplest examples. We then perform a renormalisation group analysis of the neutrino masses and mixing angles, assuming the supersymmetric standard model, and find modest radiative corrections of a few per cent, showing that the model is stable. At low energies we find sin22? 23?0.93 - 0.96 and sin22? 12?0.9 - 1.0.

King, S. F.; Nimai Singh, N.

2001-02-01

88

Neutrino mass, a status report  

SciTech Connect

Experimental approaches to neutrino mass include kinematic mass measurements, neutrino oscillation searches at rectors and accelerators, solar neutrinos, atmospheric neutrinos, and single and double beta decay. The solar neutrino results yield fairly strong and consistent indications that neutrino oscillations are occurring. Other evidence for new physics is less consistent and convincing.

Robertson, R.G.H.

1993-08-01

89

Experimental Neutrino Physics: Final Report  

SciTech Connect

Experimental studies of neutrino properties, with particular emphasis on neutrino oscillation, mass and mixing parameters. This research was pursued by means of underground detectors for reactor anti-neutrinos, measuring the flux and energy spectra of the neutrinos. More recent investigations have been aimed and developing detector technologies for a long-baseline neutrino experiment (LBNE) using a neutrino beam from Fermilab.

Lane, Charles E.; Maricic, Jelena

2012-09-05

90

Neutrino properties and puzzles  

SciTech Connect

Sixty years after the existence of the neutrino was first postulated, we are still lacking in information on the fundamental properties of neutrinos. Measurements have consistently pushed the limits on the mass, magnetic moment, and possible mixing down. Solar neutrino experiments are now shedding more light on the solar neutrino problem'' and are starting to give a hint that perhaps these quantities are nonzero. The present status of our knowledge of neutrino properties, the newest experimental data on the solar neutrino problem,'' and future plans will be presented. 27 refs.

Bowles, T.J.

1990-01-01

91

Neutrinos from hell  

NASA Astrophysics Data System (ADS)

The detection of neutrinos is studied. The use of the Kamiokande II detector, which is a cylindrical tank holding about 3000 tons of highly purified water, for neutrino detection is examined. The operation and capabilities of the Kamiokande II detector are described. The Kamiokande II and Irvine-Michigan-Brookhaven detector observed the neutrinos from SN 1987A. The relation between the supernova and the neutrinos is analyzed. Particular consideration is given to the shock wave and the energies of the neutrinos. Additional data provided by the neutrino observations are discussed.

Schorn, Ronald A.

1987-05-01

92

Neutrino Physics at Fermilab  

ScienceCinema

Neutrino oscillations provide the first evidence for physics beyond the Standard Model. I will briefly overview the neutrino "hi-story", describing key discoveries over the past decades that shaped our understanding of neutrinos and their behavior. Fermilab was, is and hopefully will be at the forefront of the accelerator neutrino experiments.  NuMI, the most powerful accelerator neutrino beam in the world has ushered us into the era of precise measurements. Its further upgrades may give a chance to tackle the remaining mysteries of the neutrino mass hierarchy and possible CP violation.

93

Neutrino Physics at Fermilab  

ScienceCinema

Neutrino oscillations provide the first evidence for physics beyond the Standard Model. I will briefly overview the neutrino "hi-story", describing key discoveries over the past decades that shaped our understanding of neutrinos and their behavior. Fermilab was, is and hopefully will be at the forefront of the accelerator neutrino experiments.  NuMI, the most powerful accelerator neutrino beam in the world has ushered us into the era of precise measurements. Its further upgrades may give a chance to tackle the remaining mysteries of the neutrino mass hierarchy and possible CP violation.

Niki Saoulidou

2010-01-08

94

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

95

Fourth Light at Paranal!  

NASA Astrophysics Data System (ADS)

VLT YEPUN Joins ANTU, KUEYEN and MELIPAL It was a historical moment last night (September 3 - 4, 2000) in the VLT Control Room at the Paranal Observatory , after nearly 15 years of hard work. Finally, four teams of astronomers and engineers were sitting at the terminals - and each team with access to an 8.2-m telescope! From now on, the powerful "Paranal Quartet" will be observing night after night, with a combined mirror surface of more than 210 m 2. And beginning next year, some of them will be linked to form part of the unique VLT Interferometer with unparalleled sensitivity and image sharpness. YEPUN "First Light" Early in the evening, the fourth 8.2-m Unit Telescope, YEPUN , was pointed to the sky for the first time and successfully achieved "First Light". Following a few technical exposures, a series of "first light" photos was made of several astronomical objects with the VLT Test Camera. This instrument was also used for the three previous "First Light" events for ANTU ( May 1998 ), KUEYEN ( March 1999 ) and MELIPAL ( January 2000 ). These images served to evaluate provisionally the performance of the new telescope, mainly in terms of mechanical and optical quality. The ESO staff were very pleased with the results and pronounced YEPUN fit for the subsequent commissioning phase. When the name YEPUN was first given to the fourth VLT Unit Telescope, it was supposed to mean "Sirius" in the Mapuche language. However, doubts have since arisen about this translation and a detailed investigation now indicates that the correct meaning is "Venus" (as the Evening Star). For a detailed explanation, please consult the essay On the Meaning of "YEPUN" , now available at the ESO website. The first images At 21:39 hrs local time (01:39 UT), YEPUN was turned to point in the direction of a dense Milky Way field, near the border between the constellations Sagitta (The Arrow) and Aquila (The Eagle). A guide star was acquired and the active optics system quickly optimized the mirror system. At 21:44 hrs (01:44 UT), the Test Camera at the Cassegrain focus within the M1 mirror cell was opened for 30 seconds, with the planetary nebula Hen 2-428 in the field. The resulting "First Light" image was immediately read out and appeared on the computer screen at 21:45:53 hrs (01:45:53 UT). "Not bad! - "Very nice!" were the first, "business-as-usual"-like comments in the room. The zenith distance during this observation was 44° and the image quality was measured as 0.9 arcsec, exactly the same as that registered by the Seeing Monitoring Telescope outside the telescope building. There was some wind. ESO PR Photo 22a/00 ESO PR Photo 22a/00 [Preview - JPEG: 374 x 400 pix - 128k] [Normal - JPEG: 978 x 1046 pix - 728k] Caption : ESO PR Photo 22a/00 shows a colour composite of some of the first astronomical exposures obtained by YEPUN . The object is the planetary nebula Hen 2-428 that is located at a distance of 6,000-8,000 light-years and seen in a dense sky field, only 2° from the main plane of the Milky Way. As other planetary nebulae, it is caused by a dying star (the bluish object at the centre) that shreds its outer layers. The image is based on exposures through three optical filtres: B(lue) (10 min exposure, seeing 0.9 arcsec; here rendered as blue), V(isual) (5 min; 0.9 arcsec; green) and R(ed) (3 min; 0.9 arcsec; red). The field measures 88 x 78 arcsec 2 (1 pixel = 0.09 arcsec). North is to the lower right and East is to the lower left. The 5-day old Moon was about 90° away in the sky that was accordingly bright. The zenith angle was 44°. The ESO staff then proceeded to take a series of three photos with longer exposures through three different optical filtres. They have been combined to produce the image shown in ESO PR Photo 22a/00 . More astronomical images were obtained in sequence, first of the dwarf galaxy NGC 6822 in the Local Group (see PR Photo 22f/00 below) and then of the spiral galaxy NGC 7793 . All 8.2-m telesco

2000-09-01

96

Neutrino interactions in matter  

SciTech Connect

If a fermion is travelling through a medium, it can have matter-induced magnetic and electric dipole moments. These contributions conserve chirality, and can be nonvanishing even for a Majorana neutrino. Several implications for neutrino physics are discussed.

Pal, P.B.

1993-03-01

97

Baryogenesis via neutrino oscillations.  

National Technical Information Service (NTIS)

We propose a new mechanism of leptogenesis in which the asymmetries in lepton numbers are produced through the CP-violating oscillations of ''sterile'' (electroweak singlet) neutrinos. The asymmetry is communicated from singlet neutrinos to ordinary lepto...

E. Akhmedov V. A. Rubakov A. Smirnov

1998-01-01

98

Birth of Neutrino Oscillation  

Microsoft Academic Search

This is a brief presentation of historical introduction to the theoretical concept of neutrino oscillation during the early stage up to 60's. (Openig address at the Europhysics NEUTRINO OSCILLATION WORKSHOP (NOW' 98), 7-9 Sept. 1998, Amsterdam.

M. Nakagawa

1998-01-01

99

Comparing Neutrino Event Generators  

SciTech Connect

This paper provides a description of a model of nucleon emission following nuclear pion absorption which has been developed for use with the NEUT Monte Carlo neutrino generator. It also discusses the comparison of several different neutrino event generators.

Tacik, Roman [Department of Physics, University of Regina, Regina, SK and TRIUMF, Vancouver, BC (Canada)

2011-11-23

100

High energy neutrino Astronomy  

NASA Astrophysics Data System (ADS)

Astrophysical candidate sources of ultra-high energy cosmic rays inevitably produce high-energy neutrinos in and/or around them. While cosmic rays are scattered in the inter-galactic magnetic fields, neutrinos point back to their origin. Hence neutrinos can be used to probe astrophysical sources just like in usual photon astronomy. Here we present the expected neutrino signals from different astrophysical objects and discuss their possible applications to study these intriguing sources.

Razzaque, Soebur

2011-12-01

101

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

102

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

103

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

104

Solar neutrino experiments  

Microsoft Academic Search

Observational methods for detecting solar neutrinos are reviewed, and the current results presented. Four operating systems, the Homestake Mine Cl-37 radio-chemical method, the real-time neutrino scattering detector at Kamiokande II, in Japan, and two radiochemical gallium-germanium experiments are discussed in some detail. The results from these operating detectors are compared to solar model calculations and various neutrino neutrino oscillation processes

Raymond Davis Jr.; Arthur N. Cox

1991-01-01

105

Neutrinos in the early universe  

NASA Astrophysics Data System (ADS)

The neutrinos from the Big Bang or the Cosmic Neutrino Background (CNB) carry precious information from the early epoch when our universe was only 1 s old. Although not yet directly detected, CNB may be revealed indirectly through cosmological observations due to neutrino important cosmological influence. We review the cosmological role of neutrinos and the cosmological constraints on neutrino characteristics. Namely, we discuss the impact of neutrinos in the early universe: the cosmic expansion, neutrino decoupling, the role of neutrinos in the primordial production of light elements, leptogenesis, etc. We briefly discuss the role of neutrino at later stages of the universe. Due to the considerable cosmological influence of neutrinos, cosmological bounds on neutrino properties from observational data exist. We review the cosmological constraints on the effective number of neutrino species, neutrino mass and mixing parameters, lepton number of the universe, presence of sterile neutrino, etc.

Kirilova, D.; Frere, J.-M.

2012-12-01

106

Neutrino Factories - Physics Potentials.  

National Technical Information Service (NTIS)

The recent results from Super-Kamiolrande 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 prese...

Z. Parsa

2001-01-01

107

Neutrino Cosmology - AN Update  

NASA Astrophysics Data System (ADS)

Present cosmological observations yield an upper bound on the neutrino mass which is significantly stronger than laboratory bounds. However, the exact value of the cosmological bound is model dependent and therefore less robust. Here, I review the current status of cosmological neutrino mass bounds and also discuss implications for sterile neutrinos and LSND in particular.

Hannestad, Steen

108

Molybdenum solar neutrino experiment  

Microsoft Academic Search

The molybdenum solar neutrino experiment goal is to deduce the (8)B solar neutrino flux, averaged over the past several million years, from the concentration of (98)Tc in a deeply buried molybdenum deposit. It is important because it will shed light on the reason for the discrepancy between theory and observation of the chlorine solar neutrino experiment. It is suggested that

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

1984-01-01

109

Neutrino masses, neutrino oscillations, double beta decay  

SciTech Connect

Experimental evidence for neutrino oscillations is so far inconclusive. Experimental data for the neutrino mass yields <5 eV from double beta decay and m<20 eV for the electron antineutrino. A review of these experimental data is given. (AIP)

Vuilleumier, J.h.

1984-05-01

110

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

111

Solar neutrinos: Probing the sun or neutrinos.  

National Technical Information Service (NTIS)

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 poi...

J. F. Wilkerson

1991-01-01

112

Neutrino Nuclear Responses For Neutrino Studies In Nuclear Femto Laboratories  

SciTech Connect

Neutrinos are key particles for particle and astro-nuclear physics. Majorana neutrino masses and phases, solar and supernova neutrino productions and oscillations, and neutrino nuclear synthesis and fundamental weak interactions are well studied in nuclei as femto laboratories. Here neutrino nuclear responses are crucial for the neutrino studies. This reports briefly experimental studies of neutrino nuclear responses, charge exchange reactions on Ga to study nuclear responses for solar and {sup 51}Cr neutrinos, and {beta}{sup +} neutrino responses for {beta}{beta}-{nu} matrix elements and astro {nu} interactions by photon and muon probes.

Ejiri, H. [Research Center for Nuclear Physics, Osaka University, Osaka 567-0047, Japan and Nuclear Science, Czech Technical University, Brehova, Prague (Czech Republic)

2011-12-16

113

Testing neutrino flavor mixing plus decay with neutrino telescopes  

Microsoft Academic Search

We discuss the interplay of neutrino oscillation and decay properties at neutrino telescopes. Motivated by recent unparticle scenarios, which open the possibility of new neutrino decay modes over astrophysical distances, we perform a complete classification of possible decay schemes, and we illustrate how different scenarios can be identified. Moreover, we show that the sensitivity of neutrino telescopes to standard neutrino

Michele Maltoni; Walter Winter

2008-01-01

114

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

115

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

116

The Neutrino Factory  

NASA Astrophysics Data System (ADS)

The discovery of neutrino oscillations marks a major milestone in the history of neutrino physics, and opens a window to what lies beyond the Standard Model. Many current and forthcoming experiments will answer open questions; however, a major step forward, up to and possibly including CP violation in the neutrino mixing matrix, will be offered by the neutrino beams from a neutrino factory. The neutrino factory is a new concept for producing neutrino beams of unprecedented quality in terms of intensity, flavour composition, and precision of the beam parameters. These beams enable the exploration of otherwise inaccessible domains in neutrino oscillation physics by exploiting baselines of planetary dimensions. Suitable detectors pose formidable challenges but seem within reach with only moderate extrapolations from existing technologies. Although the main physics' attraction of the neutrino factory is in the area of neutrino oscillations, an interesting spectrum of further opportunities ranging from high-precision, high-rate neutrino scattering to physics with high-intensity stopped muons comes with it.

Dydak, F.

117

Neutrinos from WIMP Annihilations  

NASA Astrophysics Data System (ADS)

In this talk, we make an improved analysis on the production of neutrinos coming from WIMP annihilations inside the Sun as well as the Earth. We treat both neutrino interaction and oscillation effects in a consistent three-flavor framework. Our numerical simulations are performed in an event-based setting, which is useful for both theoretical studies and creating neutrino telescope Monte Carlo simulations. We find that the yield of muon-type neutrinos is enhanced or suppressed depending on the dominant WIMP annihilation channel. In addition, we find that oscillations can significantly affect the neutrino yields from WIMP annihilations in the Sun. Effectively, the neutrino flavors are mixed. Finally, for the Earth, the oscillations have no large impact at energies for the new neutrino telescopes such as IceCube, ANTARES, and NESTOR.

Ohlsson, Tommy

2008-04-01

118

Molybdenum solar neutrino experiment  

NASA Astrophysics Data System (ADS)

The molybdenum solar neutrino experiment goal is to deduce the (8)B solar neutrino flux, averaged over the past several million years, from the concentration of (98)Tc in a deeply buried molybdenum deposit. It is important because it will shed light on the reason for the discrepancy between theory and observation of the chlorine solar neutrino experiment. It is suggested that possible reasons for the discrepancy lie in the properties of neutrinos or in deficiencies of the standard solar model. The chlorine experiment only measures the (8)B neutrino flux in current times. In the molybdenum experiments, (98)Tc (4.2 Myr) are measured, which are produced by (8)B neutrinos, and possibly (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.

119

The number of neutrino species  

NASA Astrophysics Data System (ADS)

The authors review the methods used before the operation of the high energy Stanford and CERN e+e- colliders to determine the number of neutrino species N?, or an upper limit on this number, within the framework of the Standard Model of light stable neutrinos interacting according to the SU(2)×U(1) universal couplings. The astrophysical limit based on the neutrino burst from supernova 1987A is discussed first, followed by a discussion of the cosmological constraint based on the observed He/H abundance ratio. Finally, the particle physics methods based on single-photon production in e+e- collisions, on the production of monojets in pp¯ collisions, and on the determination of N? from the ratio of the W-->l?¯ to Z0-->ll¯ partial cross sections in pp¯ collisions are discussed. The various sources of uncertainty and the experimental backgrounds are presented, as well as an idea of what may be expected on this subject in the future. There is a remarkable agreement between the various methods, with central values for N? between 2 and 3 and with upper limits N?<6. Combining all determinations, the authors obtain a central value N?=2.1+0.6-0.4 for mtop=50 GeV/c2 and N?=2.0+0.6-0.4 if mtop>=mW. The results are perfectly compatible with the a priori knowledge that at least three families of neutrinos should exist. The observed consistency between this a priori knowledge, the laboratory determinations of N?, and determinations from SN 1987A and cosmology represent an astounding success for the Standard Model and for the current descriptions of stellar collapse and the Big-Bang primordial nucleosynthesis. These results, however, severely limit the number of additional families. Although the consistency is significantly worse, four families still provide a reasonable fit. In the framework of the Standard Model, a fifth light neutrino is, however, unlikely. A noted added in proof summarizes the results recently obtained at the Fermilab p¯p and the Stanford and CERN e+e- colliders which confirm these conclusions.

Denegri, D.; Sadoulet, B.; Spiro, M.

1990-01-01

120

Neutrino masses from cosmological probes  

Microsoft Academic Search

There is a renewed interest in constraining the sum of the masses of the three neutrino flavours by using cosmological measurements. Solar, atmospheric, reactor and accelerator neutrino experiments have confirmed neutrino oscillations, implying that neutrinos have non-zero mass, but without pinning down their absolute masses. While it has been established that the effect of light neutrinos on the evolution of

Øystein Elgarøy; Ofer Lahav

2005-01-01

121

A New Neutrino Oscillation  

SciTech Connect

Starting in the late 1960s, neutrino detectors began to see signs that neutrinos, now known to come in the flavors electron ({nu}{sub e}), muon ({nu}{sub {mu}}), and tau ({nu}{sub {tau}}), could transform from one flavor to another. The findings implied that neutrinos must have mass, since massless particles travel at the speed of light and their clocks, so to speak, don't tick, thus they cannot change. What has since been discovered is that neutrinos oscillate at two distinct scales, 500 km/GeV and 15,000 km/GeV, which are defined by the baseline (L) of the experiment (the distance the neutrino travels) divided by the neutrino energy (E). Neutrinos of one flavor can oscillate into neutrinos of another flavor at both L/E scales, but the amplitude of these oscillations is different for the two scales and depends on the initial and final flavor of the neutrinos. The neutrino states that propogate unchanged in time, the mass eigenstates {nu}1, {nu}2, {nu}3, are quantum mechanical mixtures of the electron, muon, and tau neutrino flavors, and the fraction of each flavor in a given mass eigenstate is controlled by three mixing angles and a complex phase. Two of these mixing angles are known with reasonable precision. An upper bound exists for the third angle, called {theta}{sub 13}, which controls the size of the muon neutrino to electron neutrino oscillation at an L/E of 500 km/GeV. The phase is completely unknown. The existence of this phase has important implications for the asymmetry between matter and antimatter we observe in the universe today. Experiments around the world have steadily assembled this picture of neutrino oscillation, but evidence of muon neutrino to electron neutrino oscillation at 500 km/GeV has remained elusive. Now, a paper from the T2K (Tokai to Kamioka) experiment in Japan, reports the first possible observation of muon neutrinos oscillating into electron neutrinos at 500 km/GeV. They see 6 candidate signal events, above an expected background of 1.5 events. The probability that the 6 events are all background is only about 0.7%. Stated differently, this is a 2.7{sigma} indication that the parameter that controls the oscillation, the neutrino mixing angle {theta}{sub 13}, is nonzero, just shy of the 3{sigma} requirement to claim 'evidence for.' Nevertheless, this experiment provides the strongest indication to date that this oscillation actually occurs in nature.

Parke, Stephen J.; /Fermilab

2011-07-01

122

The Fourth WTO Ministerial Conference  

NSDL National Science Digital Library

Important new developments at the fourth World Trade Ministerial Conference inculded a statement that intellectual property rights (patent rights) cannot stand in the way of public health for developing countries and the admission of China into the World Trade Organisation (WTO). This site brings users summaries of the meetings, declarations, and proposed procedures. Users can also watch archived Webcasts of the proceedings.

2001-01-01

123

Two New Fourth-Order Three-Stage Symplectic Integrators  

NASA Astrophysics Data System (ADS)

Two new fourth-order three-stage symplectic integrators are specifically designed for a family of Hamiltonian systems, such as the harmonic oscillator, mathematical pendulum and lattice phi4 model. When the nonintegrable lattice phi4 system is taken as a test model, numerical comparisons show that the new methods have a great advantage over the second-order Verlet symplectic integrators in the accuracy of energy, become explicitly better than the usual non-gradient fourth-order seven-stage symplectic integrator of Forest and Ruth, and are almost equivalent to a fourth-order seven-stage force gradient symplectic integrator of Chin. As the most important advantage, the new integrators are convenient for solving the variational equations of many Hamiltonian systems so as to save a great deal of the computational cost when scanning a lot of orbits for chaos.

Li, Rong; Wu, Xin

2011-07-01

124

Charged Cosmic Rays and Neutrinos  

NASA Astrophysics Data System (ADS)

High-energy neutrino astronomy has grown up, with IceCube as one of its main experiments having sufficient sensitivity to test "vanilla" models of astrophysical neutrinos. I review predictions of neutrino fluxes as well as the status of cosmic ray physics. I comment also briefly on an improvement of the Fermi-LAT limit for cosmogenic neutrinos and on the two neutrino events presented by IceCube first at "Neutrino 2012".

Kachelrieß, M.

2013-04-01

125

Neutrino Oscillations in MINOS  

NASA Astrophysics Data System (ADS)

The MINOS experiment is a two detector experiment to study the phenomenon of neutrino oscillations, with the Near detector located at Fermilab, near Chicago and the Far detector located 734 km away, at the Soudan Underground Laboratory in Minnesota. A precision measurement of the neutrino oscillation parameters 2??23 and ?m32^2 can be accomplished using charged current neutrino events, which record both the neutrino flavor and energy. A deficit of events in the Far detector relative to that expected from the Near detector is seen, especially at low energy. In this talk we will discuss the neutrino oscillation measurement, the techniques utilized to select charged current events, as well as the expected backgrounds from neutral current neutrino scattering. Most recent results from a data set corresponding to 3.3x10^20 protons on target will be given.

Ma, Jasmine

2009-05-01

126

The neutrino telescope ANTARES  

NASA Astrophysics Data System (ADS)

The ANTARES neutrino telescope is currently the largest neutrino detector in the Northern Hemisphere. The detector consists of a three-dimensional array of 885 photomultiplier tubes, distributed along 12 lines, located at a depth of 2500 m in the Mediterranean Sea. The purpose of the experiment is the detection of high-energy cosmic neutrinos. The detection principle is based on the observation of Cherenkov-Light emitted by muons resulting from charged-current interactions of muon neutrinos in the vicinity of the detection volume. The main scientific targets of ANTARES include the search for astrophysical neutrino point sources, the measurement of the diffuse neutrino flux and the indirect search for dark matter.

Gleixner, Andreas

2014-04-01

127

Novel Ideas for Neutrino Beams  

SciTech Connect

Recent developments in neutrino physics, primarily the demonstration of neutrino oscillations in both atmospheric neutrinos and solar neutrinos, provide the first conclusive evidence for physics beyond the Standard Model of particle physics. The simplest phenomenology of neutrino oscillations, for three generations of neutrino, requires six parameters - two squared mass differences, 3 mixing angles and a complex phase that could, if not 0 or {pi}, contribute to the otherwise unexplained baryon asymmetry observed in the universe. Exploring the neutrino sector will require very intense beams of neutrinos, and will need novel solutions.

Peach, Ken [John Adams Institute for Accelerator Science, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH (United Kingdom); Royal Holloway University of London, Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH (United Kingdom)

2007-04-23

128

Neutrino mass and leptogenesis  

NASA Astrophysics Data System (ADS)

We show that the seesaw mechanism may explain two independent physical parameters, small neutrino masses and universe's baryon-number asymmetry. The seesaw mechanism, thus, provides us with a big dream to relate the present baryon asymmetry to observables in neutrino physics. We show a simple model that can predict the sign of CP violation in low-energy neutrino oscillation provided that the baryon number in the present universe is positive.

Yanagida, T.

2003-04-01

129

Neutrino Mass Anarchy  

NASA Astrophysics Data System (ADS)

What is the form of the neutrino mass matrix which governs the oscillations of the atmospheric and solar neutrinos? Features of the data have led to a dominant viewpoint where the mass matrix has an ordered, regulated pattern, perhaps dictated by a flavor symmetry. We challenge this viewpoint and demonstrate that the data are well accounted for by a neutrino mass matrix which appears to have random entries.

Hall, Lawrence; Murayama, Hitoshi; Weiner, Neal

2000-03-01

130

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

131

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

132

Neutrino mass and unification  

SciTech Connect

In this talk a discussion of neutrino masses in grand unified theories is presented. Special care is paid to the question of intermediate mass scales and it is shown how they play a crucial role in the predictions for neutrino masses. SU(5) and SO(10) models are covered, with SO(10) offering a possibility of low energy parity restoration and appreciable neutrino masses and lepton number violation.

Senjanovic, G.

1981-01-01

133

Neutrinos in supernovae  

SciTech Connect

The role of neutrinos in Type II supernovae is discussed. An overall view of the neutrino luminosity as expected theoretically is presented. The different weak interactions involved are assessed from the standpoint of how they exchange energy, momentum, and lepton number. Particular attention is paid to entropy generation and the path to thermal and chemical equilibration, and to the phenomenon of trapping. Various methods used to calculate the neutrino flows are considered. These include trapping and leakage schemes, distribution-averaged transfer, and multi-energy group methods. The information obtained from the neutrinos caught from Supernova 1987a is briefly evaluated. 55 refs., 7 figs.

Cooperstein, J.

1986-10-01

134

Neutrino-Nucleus Interactions  

NASA Astrophysics Data System (ADS)

The study of neutrino oscillations has necessitated a new generation of neutrino experiments that are exploring neutrino-nuclear scattering processes. We focus in particular on charged-current quasi-elastic scattering, a particularly important channel that has been extensively investigated both in the bubble-chamber era and by current experiments. Recent results have led to theoretical reexamination of this process. We review the standard picture of quasi-elastic scattering as developed in electron scattering, review and discuss experimental results, and discuss additional nuclear effects such as exchange currents and short-range correlations that may play a significant role in neutrino-nucleus scattering.

Gallagher, H.; Garvey, G.; Zeller, G. P.

2011-11-01

135

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

136

Neutrino-nucleus interactions  

SciTech Connect

The study of neutrino oscillations has necessitated a new generation of neutrino experiments that are exploring neutrino-nuclear scattering processes. We focus in particular on charged-current quasi-elastic scattering, a particularly important channel that has been extensively investigated both in the bubble-chamber era and by current experiments. Recent results have led to theoretical reexamination of this process. We review the standard picture of quasi-elastic scattering as developed in electron scattering, review and discuss experimental results, and discuss additional nuclear effects such as exchange currents and short-range correlations that may play a significant role in neutrino-nucleus scattering.

Gallagher, H.; /Tufts U.; Garvey, G.; /Los Alamos; Zeller, G.P.; /Fermilab

2011-01-01

137

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

138

Fourth-generation storage rings  

SciTech Connect

It seems clear that a linac-driven free-electron laser is the accepted prototype of a fourth-generation facility. This raises two questions: can a storage ring-based light source join the fourth generation? Has the storage ring evolved to its highest level of performance as a synchrotrons light source? The answer to the second question is clearly no. The author thinks the answer to the first question is unimportant. While the concept of generations has been useful in motivating thought and effort towards new light source concepts, the variety of light sources and their performance characteristics can no longer be usefully summed up by assignment of a ''generation'' number.

Galayda, J. N.

1999-11-16

139

The fourth generation in supergravity  

NASA Astrophysics Data System (ADS)

We consider model-independent constraints on the fourth-generation fermion masses and the magnitude of the D-term contribution to the scalar masses. We find that the ratio of vacuum expectation values is limited to the range 1/5 <~ ?2/? 1 <~ 4.5. We compute the mass spectrum in the class of models where the only source of soft supersymmetry breaking is the gaugino mass m1/2. The lightest charged scalar turns out to be the fourth-generation slepton, which may be ligth enough to be pair-produced at LEP. The present PETRA bound on new charged particles implies that m1/2 >~ 150 GeV. A general feature of the four-generation models is thus a heavy spectrum of sparticles. On leave from International School for Advanced Studies, Trieste, and Istituto Nazionale di Fisica Nucleare, Padua, Italy.

Enqvist, K.; Nanopoulos, D. V.; Zwirner, F.

1985-12-01

140

Neutrino-nucleus coherent scattering as a probe of neutron density distributions  

NASA Astrophysics Data System (ADS)

Neutrino-nucleus coherent elastic scattering provides a theoretically appealing way to measure the neutron part of nuclear form factors. Using an expansion of form factors into moments, we show that neutrinos from stopped pions can probe not only the second moment of the form factor (the neutron radius) but also the fourth moment. Using simple Monte Carlo techniques for argon, germanium, and xenon detectors of 3.5 tonnes, 1.5 tonnes, and 300 kg, respectively, we show that the neutron radii can be found with an uncertainty of a few percent when near a neutrino flux of 3×107 neutrinos/(cm2 s). If the normalization of the neutrino flux is known independently, one can determine the moments accurately enough to discriminate among the predictions of various nuclear energy functionals.

Patton, Kelly; Engel, Jonathan; McLaughlin, Gail C.; Schunck, Nicolas

2012-08-01

141

Fourth International Microgravity Combustion Workshop  

NASA Technical Reports Server (NTRS)

This Conference Publication contains 84 papers presented at the Fourth International Microgravity Combustion Workshop held in Cleveland, Ohio, from May 19 to 21, 1997. The purpose of the workshop was twofold: to exchange information about the progress and promise of combustion science in microgravity and to provide a forum to discuss which areas in microgravity combustion science need to be expanded profitably and which should be included in upcoming NASA Research Announcements (NRA).

Sacksteder, Kurt R. (Compiler)

1997-01-01

142

Fourth Aircraft Interior Noise Workshop  

NASA Technical Reports Server (NTRS)

The fourth in a series of NASA/SAE Interior Noise Workshops was held on May 19 and 20, 1992. The theme of the workshop was new technology and applications for aircraft noise with emphasis on source noise prediction; cabin noise prediction; cabin noise control, including active and passive methods; and cabin interior noise procedures. This report is a compilation of the presentations made at the meeting which addressed the above issues.

Stephens, David G. (compiler)

1992-01-01

143

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., IFIC; Pastor, Sergio; /Valencia U., IFIC; Pisanti, O.; /Naples U. /INFN, Naples; Serpico, Pasquale Dario; /Fermilab

2007-09-01

144

Neutrino mass and mixing with discrete symmetry.  

PubMed

This is a review paper about neutrino mass and mixing and flavour model building strategies based on discrete family symmetry. After a pedagogical introduction and overview of the whole of neutrino physics, we focus on the PMNS mixing matrix and the latest global fits following the Daya Bay and RENO experiments which measure the reactor angle. We then describe the simple bimaximal, tri-bimaximal and golden ratio patterns of lepton mixing and the deviations required for a non-zero reactor angle, with solar or atmospheric mixing sum rules resulting from charged lepton corrections or residual trimaximal mixing. The different types of see-saw mechanism are then reviewed as well as the sequential dominance mechanism. We then give a mini-review of finite group theory, which may be used as a discrete family symmetry broken by flavons either completely, or with different subgroups preserved in the neutrino and charged lepton sectors. These two approaches are then reviewed in detail in separate chapters including mechanisms for flavon vacuum alignment and different model building strategies that have been proposed to generate the reactor angle. We then briefly review grand unified theories (GUTs) and how they may be combined with discrete family symmetry to describe all quark and lepton masses and mixing. Finally, we discuss three model examples which combine an SU(5) GUT with the discrete family symmetries A?, S? and ?(96). PMID:23645075

King, Stephen F; Luhn, Christoph

2013-05-01

145

Neutrino mass and mixing with discrete symmetry  

NASA Astrophysics Data System (ADS)

This is a review paper about neutrino mass and mixing and flavour model building strategies based on discrete family symmetry. After a pedagogical introduction and overview of the whole of neutrino physics, we focus on the PMNS mixing matrix and the latest global fits following the Daya Bay and RENO experiments which measure the reactor angle. We then describe the simple bimaximal, tri-bimaximal and golden ratio patterns of lepton mixing and the deviations required for a non-zero reactor angle, with solar or atmospheric mixing sum rules resulting from charged lepton corrections or residual trimaximal mixing. The different types of see-saw mechanism are then reviewed as well as the sequential dominance mechanism. We then give a mini-review of finite group theory, which may be used as a discrete family symmetry broken by flavons either completely, or with different subgroups preserved in the neutrino and charged lepton sectors. These two approaches are then reviewed in detail in separate chapters including mechanisms for flavon vacuum alignment and different model building strategies that have been proposed to generate the reactor angle. We then briefly review grand unified theories (GUTs) and how they may be combined with discrete family symmetry to describe all quark and lepton masses and mixing. Finally, we discuss three model examples which combine an SU(5) GUT with the discrete family symmetries A4, S4 and ?(96).

King, Stephen F.; Luhn, Christoph

2013-05-01

146

Neutrino Nuclear Responses for Neutrino Studies in Nuclear Femto Laboratories  

SciTech Connect

Fundamental properties of neutrinos and neutrino nuclear interactions are of great interest from particle and astro-nuclear physics view points. They are well studied in nuclear femto laboratories, where neutrino nuclear responses are crucial. Neutrino masses and neutrino natures are studied by neutrino-less double beta decays (0{nu}{beta}{beta}) in nuclei. Here neutrino nuclear responses are required to extract neutrino properties from 0{nu}{beta}{beta} rates. Neutrino nuclear responses are sensitive to nuclear spin isospin correlations and nuclear structures. They are experimentally studied by nuclear probes for charge exchange nuclear reactions, photon EM probes for photo-nuclear reactions, and lepton probes for muon and neutrino capture reactions.

Ejiri, Hiroyasu [Research Center for Nuclear Physics, Osaka University, Osaka 567-0047 (Japan); Nuclear Science, Czech Technical University, Brehova, Prague (Czech Republic)

2010-11-24

147

Ice fishing for neutrinos  

NASA Astrophysics Data System (ADS)

A new telescope, the Antarctic Muon and Neutrino Dtector Array (AMANDA), at the South Pole is attempting to collect 'ghost' particles from some of the highest energy sources in the universe. The goal is to transform a piece of the south-polar icecap into a telescope that will map the locations of high-energy neutrinos in the sky. Ten kilometer-long strings beaded with 20 multiplier tubes along their lower 200 meters make up AMANDA. Occasionally a neutrino, racing through the 3-km-thick Antarctic icecap, interacts with an atom and spawns a muon, which emits an expanding cone of Cherenkov light as it continues along nearly the same track as the neutrino itself. By timing when this light is detected by various photomultipliers, the neutrino's origin in the sky can be determined. AMANDA records light flashes from muons created by neutrinos that have passed through the Earth to arrive at the South Pole from the northern sky. If the neutrinos come from enduring sources, such as black holes, detections will cluster around 'hot spots' in the sky. Background 'noise' from neutrinos born in Northern Hemisphere cosmic-ray showers will be distributed randomly. Other aspects AMANDA are discussed.

Robinson, Lief J.

1994-07-01

148

The Baksan Neutrino Observatory  

NASA Astrophysics Data System (ADS)

An overall view of the history of the Baksan Neutrino Observatory INR RAS creation is presented. Ground-based and underground facilities used to study cosmic rays, rare nuclear reactions and decays, register solar neutrinos, observe various geophysical phenomena are described. Some main results obtained with these facilities are given.

Kuzminov, V. V.

2012-09-01

149

Neutrino astronomy: An update  

NASA Astrophysics Data System (ADS)

Detecting neutrinos associated with the still enigmatic sources of cosmic rays has reached a new watershed with the completion of IceCube, the first detector with sensitivity to the anticipated fluxes. In this review, we will briefly revisit the rationale for constructing kilometer-scale neutrino detectors and summarize the status of the field.

Halzen, Francis

2013-12-01

150

Neutrino astronomy: An update  

NASA Astrophysics Data System (ADS)

Detecting neutrinos associated with the still enigmatic sources of cosmic rays has reached a new watershed with the completion of IceCube, the first detector with sensitivity to the anticipated fluxes. In this review, we will briefly revisit the rationale for constructing kilometer-scale neutrino detectors and summarize the status of the field.

Halzen, Francis

2014-01-01

151

Neutrino Astronomy: An Update  

NASA Astrophysics Data System (ADS)

Detecting neutrinos associated with the still enigmatic sources of cosmic rays has reached a new watershed with the completion of IceCube, the first detector with sensitivity to the anticipated fluxes. In this review, we will briefly revisit the rationale for constructing kilometer-scale neutrino detectors and summarize the status of the field.

Halzen, Francis

2013-01-01

152

Theory of Neutrinos  

Microsoft Academic Search

After a brief overview of the present knowledge of neutrino masses and mixing, we summarize what can be learned about physics beyond the standard model from the various proposed neutrino experiments. We also comment on the impact of the experiments on our understanding of the origin of the matter-antimatter asymmetry of the Universe as well as what can be learned

R. N. Mohapatra; S. Antusch; K. S. Babu; G. Barenboim; Mu-Chun Chen; S. Davidson; A. de Gouvea; P. de Holanda; B. Dutta; Y. Grossman; A. Joshipura; 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. Petcov; A. Pilaftsis; P. Ramond; M. Ratz; W. Rodejohann; R. Shrock; T. Takeuchi; T. Underwood; F. Vissani; L. Wolfenstein

2004-01-01

153

Helioseismology and solar neutrinos  

Microsoft Academic Search

The manner by which helioseismic date are obtained and analysed to diagnose the interior structure and rotation of the Sun is briefly described. The principal results of the analysis pertinent to solar neutrino production are presented; they have constrained standard theoretical models of the Sun in such a way as to prevent them from explaining the neutrino flux measurements without

D. O. Gough

1999-01-01

154

Molybdenum Solar Neutrino Experiment.  

National Technical Information Service (NTIS)

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 u...

K. Wolfsberg G. A. Cowan E. A. Bryant K. S. Daniels S. W. Downey

1984-01-01

155

Helioseismology and solar neutrinos  

Microsoft Academic Search

The manner by which helioseismic data are obtained and analysed to diagnose the interior structure and rotation of the Sun is briefly described. The principal results of the analysis pertinent to solar neutrino production are presented; they have constrained standard theoretical models of the Sun in such a way as to prevent them from explaining the neutrino flux measurements without

D. O. Gough

1999-01-01

156

Reactor neutrino anomaly and sterile neutrinos revisited  

NASA Astrophysics Data System (ADS)

In this contribution we will present results from two separate experiments dealing with the neutrino response on 71Ga. Both experiments provide input to the calibration of the SAGE and GALLEX solar neutrino detectors and address a long-standing discrepancy between the measured and evaluated capture rates from the 51Cr and 37Ar neutrino calibration sources. The first is a 71Ga(3He,t)71Ge charge-exchange experiment performed at RCNP, Osaka, which allows to extract with high precision the Gamow-Teller transition strengths to the three lowest-lying states in 71Ge, i.e., the ground state (1/2-), the 175 (5/2-) and the 500 keV (3/2-) excited states. These are the states, which are populated via a charged-current reaction induced by neutrinos from reactor produced 51Cr and 37Ar sources. In the second part we present a new precision Q-value measurement for the 71Ga(nu,e-)71Ge reaction using the TITAN mass measurement facility at TRIUMF. From the results of the two experiments we now conclude that there are no further unknowns in the nuclear structure, which could remove the persistent discrepancy in the SAGE and GALLEX calibration measurement performed with neutrinos from 51Cr and 37Ar sources.

Lennarz, Annika

2012-10-01

157

Neutrino Astronomy and Intermediate Bosons.  

National Technical Information Service (NTIS)

Neutrino fluxes from strong radio sources are estimated, assuming the neutrino-production mechanism: p+p yields nucleons+mesons yields nucleons+electrons, gamma rays, and neutrinos. The neutrino fluxes calculated on the basis of this mechanism are too sma...

J. N. Bahcall S. C. Frautschi

1964-01-01

158

Neutrino mass bounds from cosmology  

NASA Astrophysics Data System (ADS)

Cosmology is at present one of the most powerful probes of neutrino properties. The advent of precision data from the cosmic microwave background and large scale structure has allowed for a very strong bound on the neutrino mass. Here, I review the status of cosmological bounds on neutrino properties with emphasis on mass bounds on light neutrinos.

Hannestad, Steen

2005-08-01

159

Summary: Neutrinos and nonaccelerator physics  

SciTech Connect

This paper contains brief synopsis of the following major topics discussed in the neutrino and nonaccelerator parallel sessions: dark matter; neutrino oscillations at accelerators and reactors; gamma-ray astronomy; double beta decay; solar neutrinos; and the possible existence of a 17-KeV neutrino. (LSP)

Hoffman, C.M.

1991-01-01

160

Muon neutrino to electron neutrino oscillations in the MINOS experiment  

NASA Astrophysics Data System (ADS)

MINOS is a long-baseline neutrino oscillation experiment situated along Fermilab's high-intensity NuMI neutrino beam. MINOS has completed an updated search for muon neutrino to electron neutrino transitions, observation of which would indicate a non-zero value for the neutrino mixing angle ?13. The present 7×1020 protons-on-target data set represents more than double the exposure used in the previous analysis. The new results are presented.

Toner, R.; Pawloski, G.; Whitehead, L.; Minos Collaboration

2012-08-01

161

Higgs phenomenology in warped extra dimensions with a fourth generation  

NASA Astrophysics Data System (ADS)

We study a warped extra-dimension scenario where the standard model fields lie in the bulk, with the addition of a fourth family of fermions. We concentrate on the flavor structure of the Higgs couplings with fermions in the flavor anarchy ansatz. Even without a fourth family, these couplings will be generically misaligned with respect to the standard model fermion mass matrices. The presence of the fourth family typically enhances the misalignment effects and we show that one should expect them to be highly nonsymmetrical in the (34) intergenerational mixing. The radiative corrections from the new fermions and their flavor-violating couplings to the Higgs affect negligibly known experimental precision measurements such as the oblique parameters and Z?bb¯ or Z??+?-. On the other hand, ?F=1, 2 processes, mediated by tree-level Higgs exchange, as well as radiative corrections to b?s? and ??e? put some generic pressure on the allowed size of the flavor-violating couplings. But more importantly, these couplings will alter the Higgs decay patterns as well as those of the new fermions, and produce very interesting new signals associated to Higgs phenomenology in high energy colliders. These signals might become very important indirect signals for these type of models as they would be present even when the KK mass scale is high and no heavy KK particle is discovered.

Frank, Mariana; Korutlu, Beste; Toharia, Manuel

2011-10-01

162

Neutrino Oscillations, Masses and Mixing  

Microsoft Academic Search

The original B. Pontecorvo idea of neutrino oscillations is discussed.\\u000aNeutrino mixing and basics of neutrino oscillations in vacuum and in matter are\\u000aconsidered. Recent evidences in favour of neutrino oscillations, obtained in\\u000aSuper-Kamiokande, SNO, KamLAND and other neutrino experiments are discussed.\\u000aNeutrino oscillations in the solar and atmospheric ranges of the neutrino\\u000amass-squared differences are considered in the framework

W. M. Alberico; S. M. Bilenky

2003-01-01

163

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

164

Tau Neutrinos Favored over Sterile Neutrinos in Atmospheric Muon Neutrino Oscillations  

Microsoft Academic Search

The previously published atmospheric neutrino data did not distinguish whether muon neutrinos were oscillating into tau neutrinos or sterile neutrinos, as both hypotheses fit the data. Using data recorded in 1100 live days of the Super-Kamiokande detector, we use three complementary data samples to study the difference in zenith angle distribution due to neutral currents and matter effects. We find

S. Fukuda; Y. Fukuda; M. Ishitsuka; Y. Itow; T. Kajita; J. Kameda; K. Kaneyuki; K. Kobayashi; Y. Koshio; M. Miura; S. Moriyama; M. Nakahata; S. Nakayama; Y. Obayashi; A. Okada; K. Okumura; N. Sakurai; M. Shiozawa; Y. Suzuki; H. Takeuchi; Y. Takeuchi; T. Toshito; 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. Barszczak; D. Casper; W. Gajewski; W. R. Kropp; S. Mine; L. R. Price; M. Smy; H. W. Sobel; M. R. Vagins; K. S. Ganezer; W. E. Keig; R. W. Ellsworth; S. Tasaka; A. Kibayashi; J. G. Learned; S. Matsuno; D. Takemori; Y. Hayato; T. Ishii; T. Kobayashi; K. Nakamura; Y. Oyama; A. Sakai; M. Sakuda; O. Sasaki; M. Kohama; A. T. Suzuki; T. Inagaki; K. Nishikawa; T. J. Haines; E. Blaufuss; B. K. Kim; R. Sanford; R. Svoboda; M. L. Chen; J. A. Goodman; G. Guillian; G. W. Sullivan; J. Hill; C. K. Jung; K. Martens; M. Malek; C. Mauger; C. McGrew; E. Sharkey; B. Viren; C. Yanagisawa; M. Kirisawa; S. Inaba; C. Mitsuda; K. Miyano; H. Okazawa; C. Saji; M. Takahashi; M. Takahata; Y. Nagashima; K. Nitta; M. Takita; M. Yoshida; S. B. Kim; T. Ishizuka; M. Etoh; Y. Gando; T. Hasegawa; K. Inoue; K. Ishihara; T. Maruyama; J. Shirai; M. Koshiba; Y. Hatakeyama; Y. Ichikawa; M. Koike; K. Nishijima; H. Fujiyasu; H. Ishino; M. Morii; Y. Watanabe; U. Golebiewska; D. Kielczewska; S. C. Boyd; A. L. Stachyra; R. J. Wilkes; K. K. Young

2000-01-01

165

Neutrino-neutrino interactions in a supernova and their effect on neutrino flavor conversions  

SciTech Connect

The neutrino-neutrino interactions inside a supernova core give rise to nonlinear collective effects that significantly influence the neutrino flavor conversions inside the star. I shall describe these interactions, the new oscillation phenomena they generate, and their effect on the neutrino fluxes arriving at the earth.

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

2011-11-23

166

Neutrino oscillations: theory and phenomenology  

NASA Astrophysics Data System (ADS)

A brief overview of selected topics in the theory and phenomenology of neutrino oscillations is given. These include: oscillations in vacuum and in matter; phenomenology of 3-flavour neutrino oscillations; CP and T violation in neutrino oscillations in vacuum and in matter; matter effects on ????? oscillations; parametric resonance in neutrino oscillations inside the earth; oscillations below and above the MSW resonance; unsettled issues in the theory of neutrino oscillations.

Akhmedov, E. K.

2011-12-01

167

Neutrinos Are Nearly Dirac Fermions  

Microsoft Academic Search

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 x_nu characterizes the kind of the neutrinos, with x_nu = 0 for Dirac neutrinos and x_nu = pi\\/2 for Majorana neutrinos. If x_nu = 0, then baryon-minus-lepton number is conserved. When x_nu is

Kevin Cahill

1999-01-01

168

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

169

Presupernovae as Powerful Neutrino Sources  

NASA Astrophysics Data System (ADS)

In this report, some research results of the neutrino astrophysics group at the Institute of Physics of Jagellonian University are presented http://ribes.if.uj.edu.pl/psns . It is shown that neutrinos emitted by presupernovae located within a few kpc from Earth could be detected by new generation of neutrino detectors. We encourage planners of the future neutrino experiments to include presupernova neutrino measurements on their agenda.

Kutschera, M.; Odrzywo?ek, A.; Misiaszek, M.

2009-11-01

170

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

171

Neutrino cosmology and Planck  

NASA Astrophysics Data System (ADS)

Relic neutrinos play an important role in the evolution of the Universe, modifying some of the cosmological observables. We summarize the main aspects of cosmological neutrinos and describe how the precision of present cosmological data can be used to learn about neutrino properties. In particular, we discuss how cosmology provides information on the absolute scale of neutrino masses, complementary to beta decay and neutrinoless double-beta decay experiments. We explain why the combination of Planck temperature data with measurements of the baryon acoustic oscillation angular scale provides a strong bound on the sum of neutrino masses, 0.23 eV at the 95% confidence level, while the lensing potential spectrum and the cluster mass function measured by Planck are compatible with larger values. We also review the constraints from current data on other neutrino properties. Finally, we describe the very good perspectives from future cosmological measurements, which are expected to be sensitive to neutrino masses close to the minimum values guaranteed by flavour oscillations.

Lesgourgues, Julien; Pastor, Sergio

2014-06-01

172

Nonzero ?13 and Neutrino Masses from Modified Neutrino Mixing Matrix  

NASA Astrophysics Data System (ADS)

The nonzero and relatively large ?13 have been reported by Daya Bay, T2K, MINOS and Double Chooz Collaborations. In order to accommodate the nonzero ?13, we modified the tribimaximal (TB), bimaxima (BM) and democratic (DC) neutrino mixing matrices. From three modified neutrino mixing matrices, two of them (the modified BM and DC mixing matrices) can give nonzero ?13 which is compatible with the result of the Daya Bay and T2K experiments. The modified TB neutrino mixing matrix predicts the value of ?13 which is greater than the upper bound value of the latest experimental results. By using the modified neutrino mixing matrices and imposing an additional assumption that neutrino mass matrices have two zeros texture, we then obtain the neutrino mass in normal hierarchy when (M?)22 = (M?)33 = 0 for the neutrino mass matrix from the modified TB neutrino mixing matrix and (M?)11 = (M?)13 = 0 for the neutrino mass matrix from the modified DC neutrino mixing matrix. For these two patterns of neutrino mass matrices, either the atmospheric mass squared difference or the solar mass squared difference can be obtained, but not both of them simultaneously. From four patterns of two zeros texture to be considered on the obtained neutrino mass matrix from the modified BM neutrino mixing matrix, none of them can correctly predict the neutrino mass spectrum (normal or inverted hierarchy).

Damanik, Asan

2012-06-01

173

Review of Recent Neutrino Physics Research  

NASA Astrophysics Data System (ADS)

We review recent research in neutrino physics, including neutrino oscillations to test time reversal and CP symmetry violations, the measurement of parameters in the U matrix, sterile neutrino emission causing pulsar kicks, and neutrino energies in the neutrinosphere.

Kisslinger, Leonard S.

2013-09-01

174

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

175

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

176

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

177

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.

Dr. Don Lincoln

2013-07-11

178

Majorana neutrino superfluidity and stability of neutrino dark energy  

SciTech Connect

We demonstrate that Majorana neutrinos can form Cooper pairs due to long-range attractive forces and show BCS superfluidity in a class of mass varying neutrino dark energy models. We describe the condensates for Majorana neutrinos and estimate the value of the gap, critical temperature, and Pippard coherence length for a simple neutrino dark energy model. In the strong coupling regime bosonic degree of freedom can become important, and Bose-Einstein condensate may govern the dynamics for the mass varying neutrino models. Formation of the condensates can significantly alter the instability scenario in the mass varying neutrino models.

Bhatt, Jitesh R.; Sarkar, Utpal [Physical Research Laboratory, Ahmedabad 380009 (India)

2009-08-15

179

Observational Neutrino Astronomy.  

National Technical Information Service (NTIS)

Experiments to be performed in 1965 involving neutrinos from the sun, from the decay of cosmic-ray secondaries, and from strong radio sources are discussed. The foundations of the theoretical predictions and the significance of the experiments are emphasi...

J. N. Bahcall

1964-01-01

180

Sterile neutrino anarchy  

NASA Astrophysics Data System (ADS)

Lepton mixing, which requires physics beyond the Standard Model, is surprisingly compatible with a minimal, symmetryless and unbiased approach, called anarchy. This contrasts with highly involved flavor symmetry models. On the other hand, hints for light sterile neutrinos have emerged from a variety of independent experiments and observations. If confirmed, their existence would represent a groundbreaking discovery, calling for a theoretical interpretation. We discuss anarchy in the two-neutrino eV-scale seesaw framework. The distributions of mixing angles and masses according to anarchy are in agreement with global fits for the active and sterile neutrino parameters. Our minimal and economical scenario predicts the absence of neutrinoless double beta decay and one vanishing neutrino mass, and can therefore be tested in future experiments.

Heeck, Julian; Rodejohann, Werner

2013-02-01

181

The ANTARES neutrino telescope  

NASA Astrophysics Data System (ADS)

The ANTARES collaboration completed the installation of the first neutrino detector in the sea in 2008. It consists of a three dimensional array of 885 photomultipliers to gather the Cherenkov photons induced by relativistic muons produced in charged-current interactions of high energy neutrinos close to/in the detector. The scientific scope of neutrino telescopes is very broad: the origin of cosmic rays, the origin of the TeV photons observed in many astrophysical sources or the nature of dark matter. The data collected up to now have allowed us to produce a rich output of physics results, including the map of the neutrino sky of the Southern hemisphere, search for correlations with GRBs, flaring sources, gravitational waves, limits on the flux produced by dark matter self-annihilations, etc. In this paper a review of these results is presented.

Zornoza, J. D.; Zúñiga, J.

2013-05-01

182

Helioseismology and solar neutrinos  

NASA Astrophysics Data System (ADS)

The manner by which helioseismic data are obtained and analysed to diagnose the interior structure and rotation of the Sun is briefly described. The principal results of the analysis pertinent to solar neutrino production are presented; they have constrained standard theoretical models of the Sun in such a way as to prevent them from explaining the neutrino flux measurements without recourse to neutrino transitions. However, standard solar models do not represent the entire class of plausible models, and indeed they suffer the deficiency of being unstable. Models in which the products of the nuclear reactions are redistributed in the core may represent the Sun more closely, and should at least be considered and tested further in the process of developing a reliable model of the neutrino source.

Gough, D. O.

1999-05-01

183

Very high energy neutrinos  

NASA Astrophysics Data System (ADS)

A sky survey with neutrinos may considerably extend our understanding of cosmic phenomena. Due to the low interaction cross section of neutrinos with matter and due to the high cosmic ray background the detector must be very large (of the order of 1 km 3) and must be shielded. These new devices consist of a network of photo-tubes which are deployed in the depth of the ocean, of a lake or of the ice of South Pole. The detection of the Cherenkov light emitted by muons produced in muon neutrino interactions with the matter surrounding the detector will allow the reconstruction of the neutrino direction with an angular resolution of the order or lower than one degree. Several projects are underway. Their status will be reviewed in this paper.

Moscoso, Luciano; Spiering, Christian

2000-03-01

184

Neutrino electron plasma instability  

NASA Astrophysics Data System (ADS)

Weak interactions play an important role in early universe plasma collection, especially on neutrinos and the corresponding leptons. It also has important effects on the detail balance of the primordial nucleosynthesis, especially on the production of He and light elements. At around T = 300 GeV, the primordial plasma undergone electroweak spontaneous symmetry breaking (SSB) phase transition. Some of the gauge bosons and other particles gain mass via Higgs mechanism. Deduced from Weinberg-Salam electroweak theory, a Boltzmann equation and subsequent fluid equations are derived for the primordial electron-positron-neutrino- photon plasma. A collective instability that separates the phases of electrons (and positrons) and neutrinos (and anti-neutrinos) is discussed. We also discussed the application of the fluctuation-dissipation theory in this system of plasma. An approach with Hubble expansion included in Boltzmann equation is also discussed. Astrophysical applications and implications are explored, particularly in supernovae.

Lai, Chi-Hsuan

1999-03-01

185

Neutrino flavor conversion in random magnetic fields  

Microsoft Academic Search

If massive neutrinos possess magnetic moments, a magnetic field can cause a spin flip. In the case of Dirac neutrinos the spin flip converts an active neutrino into a sterile one and vice versa. By constrast, if neutrinos are Majorana particles, a spin flip converts them to a neutrino of a different flavor. We examine the behavior of neutrinos in

G. Domokos; S. Kovesi-Domokos

1997-01-01

186

Neutrino Masses, Where Do We Stand?  

Microsoft Academic Search

I review the status of neutrino physics post-Neutrino~98, including the implications of solar and atmospheric neutrino data, which strongly indicate nonzero neutrino masses. LSND and the possible role of neutrinos as hot dark matter (HDM) are also mentioned. The simplest schemes proposed to reconcile these requirements invoke a light sterile neutrino in addition to the three active ones, two of

J. W. F. Valle

1999-01-01

187

Fourth Personnel Dosimetry Intercomparison Study  

SciTech Connect

The fourth Personnel Dosimetry Intercomparison Study was held at the Oak Ridge National Laboratory's Dosimetry Applications Research Facility during March 15-23, 1978. The Health Physics Research Reactor (HPRR) used unshielded, with a 12-cm-thick Lucite shield, a 20-cm-thick concrete shield, or a 5-cm-thick steel and 15-cm-thick concrete shield, and provided four neutron and gamma-ray spectra. Then the dose was calculated based on the HPRR neutron spectra and dose conversion factors which had been determined previously for the four spectra. The results of these personnel dosimetry intercomparison studies reveal that estimates of dose equivalent vary over a wide range. The standard deviation of the mean of participants data for gamma measurements was in the range of 29 to 43%; for neutrons it was 57 to 188%. (PCS)

Dickson, H.W.

1980-02-01

188

Asteroid families  

NASA Astrophysics Data System (ADS)

Dynamical and physical investigations of asteroid families are reviewed. Particular attention is given to recent work carried out mainly by means of a combination of numerical integration and filtering techniques and aimed at assessing the accuracy of proper elements with respect to the linear theory as well as evaluating some aspects of the second-order fourth-degree analytical theory of Yuasa (1973). It is noted that recent numerical results show that the issue of proper elements has to be reconsidered, particularly concerning the effect of the proximity to the mean motion resonances.

Froeschle, Cl.; Froeschle, Ch.; Gonczi, R.; Farinella, P.; Carpino, M.

189

Neutrino Flavor Tagging in a Four-Neutrino Mixing and Oscillation Model  

Microsoft Academic Search

A neutrino mass dominance quantity is introduced for tagging the neutrino flavor in the phenomenological two-parameter four neutrino mixing matrix with two neutrino mass doublets and thorough maximal neutrino doublet mixing. While there is no hierarchy of the neutrino masses in the neutrino flavor eigenstates of this model, it may rather be a special hierarchy of the mass dominance ratios

E. M. Lipmanov

1999-01-01

190

Neutrino oscillation based on the mixings with a heavy right-handed neutrino  

Microsoft Academic Search

We study a consistent explanation for both deficits of solar neutrino and atmospheric neutrino due to the neutrino oscillation induced by the mixing of light neutrinos with a heavy right-handed neutrino. We propose such a phenomenological neutrino mass matrix that realizes this scenario in the simple three generation left- and right- handed neutrino framework. Although this model contains only one

Daijiro Suematsu

1997-01-01

191

GUT, neutrinos, and baryogenesis  

NASA Astrophysics Data System (ADS)

It is an exciting time for flavor physics. In this talk, I discuss recent topics in baryogenesis and leptogenesis in light of new data, and implications in B and neutrino physics. I also discuss current situation of grand unified theories concerning coupling unification, proton decay, and indirect consequences in lepton flavor violation and B physics. I explain attempts to understand the origin of flavor based on flavor symmetry, in particular "anarchy" in neutrinos.

Murayama, Hitoshi

2002-11-01

192

Radiochemical solar neutrino experiments  

NASA Astrophysics Data System (ADS)

Radiochemical experiments have been crucial to solar neutrino research. Even today, they provide the only direct measurement of the rate of the proton-proton fusion reaction, p+p?d+e++?e, which generates most of the Sun's energy. We first give a little history of radiochemical solar neutrino experiments with emphasis on the gallium experiment SAGE - the only currently operating detector of this type. The combined result of all data from the Ga experiments is a capture rate of 67.6±3.7 SNU. For comparison to theory, we use the calculated flux at the Sun from a standard solar model, take into account neutrino propagation from the Sun to the Earth and the results of neutrino source experiments with Ga, and obtain 67.3-3.5+3.9 SNU. Using the data from all solar neutrino experiments we calculate an electron neutrino pp flux of ?pp?=(3.41-0.77+0.76)×1010/(cm-s), which agrees well with the prediction from a detailed solar model of ?pp?=(3.30-0.14+0.13)×1010/(cm-s). Four tests of the Ga experiments have been carried out with very intense reactor-produced neutrino sources and the ratio of observed to calculated rates is 0.88±0.05. One explanation for this unexpectedly low result is that the cross section for neutrino capture by the two lowest-lying excited states in 71Ge has been overestimated. We end with consideration of possible time variation in the Ga experiments and an enumeration of other possible radiochemical experiments that might have been.

Gavrin, V. N.; Cleveland, B. T.

2011-12-01

193

Boxing with Neutrino Oscillations  

NASA Astrophysics Data System (ADS)

We have developed a model-independent ``box'' parameterization of neutrino oscillations. Oscillation probabilities are linear in these new parameters, so measurements can straighforwardly determine the box parameters which can then be manipulated to yield magnitudes of mixing matrix elements. We will present these new parameters and examine the effects of unitarity which reduce the number of independent parameters to the minimum set. The framework presented here will facilitate general analyses of neutrino oscillations among n >= 3 flavors.

Wagner, Dj; Weiler, Thomas J.

1998-03-01

194

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

195

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

196

Frontiers of neutrino astrophysics. Proceedings.  

NASA Astrophysics Data System (ADS)

This symposium highlighted the recent developments and the future direction of neutrino astrophysics and related topics. The results from on-going solar neutrino experiments as well as detailed discussions on the possible solutions to the solar neutrino problems were presented, including the observed deficit of the atmospheric muon neutrinos. The status of many new solar neutrino experiments were reported, and topics from grand unified theories, big bang cosmology, and dark matter were presented. Discussions were also held on radiation from supernovae and compact astrophysical objects, not just with regard to neutrinos, but also X-rays, ?-rays, and gravitational waves.

Suzuki, Y.; Nakamura, K.

197

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

198

Neutrino quantum kinetics  

NASA Astrophysics Data System (ADS)

We present a formulation of the quantum kinetic equations (QKEs), which govern the evolution of neutrino flavor at high density and temperature. Here, the structure of the QKEs is derived from the ground up, using fundamental neutrino interactions and quantum field theory. We show that the resulting QKEs describe coherent flavor evolution with an effective mass when inelastic scattering is negligible. The QKEs also contain a collision term. This term can reduce to the collision term in the Boltzmann equation when scattering is dominant and the neutrino effective masses and density matrices become diagonal in the interaction basis. We also find that the QKEs include equations of motion for a new dynamical quantity related to neutrino spin. This quantity decouples from the equations of motion for the density matrices at low densities or in isotropic conditions. However, the spin equations of motion allow for the possibility of coherent transformation between neutrinos and antineutrinos at high densities and in the presence of anisotropy. Although the requisite conditions for this exist in the core collapse supernova and compact object merger environments, it is likely that only a self-consistent incorporation of the QKEs in a sufficiently realistic model could establish whether or not significant neutrino-antineutrino conversion occurs.

Vlasenko, Alexey; Fuller, George M.; Cirigliano, Vincenzo

2014-05-01

199

MINOS neutrino oscillation results  

NASA Astrophysics Data System (ADS)

Neutrinos interact only weakly with other matter and had been thought to be massless. However, if their mass is non-zero, they could change flavors as they propagate. Recent results from observations of atmospheric, solar, and reactor neutrinos indicate that they do change flavor and these observations have provided measurements of two of the three possible mixings. The MINOS experiment is now making precise measurements of the ??? oscillations seen in atmospheric neutrinos, and extends our reach towards the so far unseen angle ?3 by looking for ? appearance from the ? beam. It does so by using the intense, well-understood NuMI neutrino beam created at Fermilab and observing it 735 km away at the Soudan Mine in Northeast Minnesota. This combination also allows investigation of the oscillation properties of anti-neutrinos, as the NuMI beam can focus opposite-charged pions to produce the anti-neutrinos, and the MINOS detectors are magnetized, allowing event-by-event discrimination of the resulting muon charge-sign.

Habig, A.; Minos Collaboration

200

Complications of Fourth-Ventricular Shunts  

Microsoft Academic Search

Fourth-ventricular shunting is commonly used to treat symptomatic posterior fossa cysts of the Dandy-Walker malformation and trapped fourth ventricle. Although the benefits of this procedure have been widely reported, there is a paucity of data on the pitfalls of posterior fossa shunting in the neurosurgical literature. During the 4-year period from July 1989 to June 1993, we placed fourth-ventricular shunts

Mark Lee; Diana Leahu; Howard L. Weiner; Rick Abbott; Jeffrey H. Wisoff; Fred J. Epstein

1995-01-01

201

Shock wave propagation in prompt supernova explosion and the MSW effect of neutrino  

NASA Astrophysics Data System (ADS)

The MSW effect of supernova neutrino is one of foci of recent neutrino astrophysics. It is still an open question how the shock wave propagation affects the neutrino oscillation. Using an implicit Lagrangian code for general relativistic spherical hydrodynamics, we succeeded in numerical simulations of breakout of shock wave propagation through the stellar envelope. We first discuss our successful result of shock wave propagation which is generated by adiabatic collapse of iron core, and compare with non-adiabatic models. Secondly, we apply our model to the neutrino oscillation and calculate survival probabilities of three light-neutrino families. We discuss how the flux and energy spectrum of each neutrino species can change due to the MSW effect.

Kawagoe, Shiou; Kajino, T.; Suzuki, H.; Sumiyoshi, K.; Yamada, S.

2006-05-01

202

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

203

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

204

Astrophysical tau neutrinos and their detection by large neutrino telescopes  

SciTech Connect

We present results of the detailed Monte Carlo calculation of the rates of double-bang events in a 1-km{sup 3} underwater neutrino telescope taking into account the effects of {tau}-neutrino propagation through the Earth. As an input, the moderately optimistic theoretical predictions for diffuse neutrino spectra of AGN jets are used.

Bugaev, E.V. [Institute for Nuclear Research, Russian Academy of Sciences, Moscow (Russian Federation); Montaruli, T. [Physics Department, Bari University (Italy); INFN/Bari (Italy); Sokalski, I.A. [INFN/Bari (Italy)

2004-06-01

205

Neutrino masses: evidences and implications  

NASA Astrophysics Data System (ADS)

I give an overview of the evidences for neutrino masses and mixing, the associated neutrino mass generation schemes, as well as the resulting implications in particle physics experiments and cosmology.

Valle, J. W. F.

2014-03-01

206

Cosmology of "visible" Sterile Neutrinos  

NASA Astrophysics Data System (ADS)

We point out that in scenarios with a low reheating temperature TR << 100 MeV at the end of (the last episode of) inflation or entropy production, the abundance of sterile neutrinos becomes largely independent of their coupling to active neutrinos. Thus, cosmological bounds become less stringent than usually assumed, allowing sterile neutrinos to be "visible" in future experiments. For example, the sterile neutrino required by the LSND result does not have any cosmological problem within these scenarios.

Gelmini, Graciela B.

207

Neutrino Masses and Flavor Mixing  

NASA Astrophysics Data System (ADS)

I give a theoretical overview of some basic properties of massive neutrinos in these lectures. Particular attention is paid to the origin of neutrino masses, the pattern of lepton flavor mixing, the feature of leptonic CP violation and the electromagnetic properties of massive neutrinos. I highlight the TeV seesaw mechanisms as a possible bridge between neutrino physics and collider physics in the era characterized by the Large Hadron Collider.

Xing, Zhi-zhong

2010-06-01

208

Observation of geo-neutrinos  

Microsoft Academic Search

Geo-neutrinos, electron anti-neutrinos produced in ? 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? C.L. of geo-neutrinos, performed with the Borexino detector at Laboratori Nazionali del Gran Sasso. Anti-neutrinos are detected through the neutron inverse ? decay reaction. With a 252.6

G. Bellini; J. Benziger; S. Bonetti; M. Buizza Avanzini; B. Caccianiga; L. Cadonati; F. Calaprice; C. Carraro; A. Chavarria; F. Dalnoki-Veress; D. D'Angelo; S. Davini; H. de Kerret; A. Derbin; A. Etenko; G. Fiorentini; K. Fomenko; D. Franco; C. Galbiati; S. Gazzana; C. Ghiano; M. Giammarchi; A. Goretti; E. Guardincerri; S. Hardy; Aldo Ianni; Andrea Ianni; M. Joyce; V. V. Kobychev; Y. Koshio; G. Korga; D. Kryn; M. Laubenstein; T. Lewke; E. Litvinovich; B. Loer; P. Lombardi; L. Ludhova; I. Machulin; S. Manecki; W. Maneschg; G. Manuzio; Q. Meindl; E. Meroni; L. Miramonti; M. Misiaszek; D. Montanari; V. Muratova; L. Oberauer; M. Obolensky; F. Ortica; M. Pallavicini; L. Papp; L. Perasso; S. Perasso; A. Pocar; R. S. Raghavan; G. Ranucci; A. Razeto; B. Ricci; P. Risso; A. Romani; D. Rountree; A. Sabelnikov; R. Saldanha; C. Salvo; S. Schönert; H. Simgen; M. Skorokhvatov; O. Smirnov; A. Sotnikov; S. Sukhotin; Y. Suvorov; R. Tartaglia; G. Testera; D. Vignaud; R. B. Vogelaar; F. von Feilitzsch; J. Winter; M. Wojcik; A. Wright; M. Wurm; J. Xu; O. Zaimidoroga; S. Zavatarelli; G. Zuzel

2010-01-01

209

Neutrino Mixing in the ??SSM  

NASA Astrophysics Data System (ADS)

Recently, several reactor oscillation experiments have successively measured a nonzero value for the neutrino mixing angle ?13, which is greater than five standard deviations. Within framework of the ? from ? Supersymmetric Standard Model (??SSM), three tiny neutrino masses are generated at the tree level through TeV scale seesaw mechanism. In this work, we analyze the neutrino masses and mixing in the ??SSM with a "top-down" method, assuming neutrino mass spectrum with normal ordering or inverted ordering.

Zhang, Hai-Bin; Feng, Tai-Fu; Kou, Li-Na; Zhao, Shu-Min

2013-09-01

210

FABRIC FILTER SYSTEM STUDY; FOURTH ANNUAL REPORT  

EPA Science Inventory

The report gives results of the fourth year of operation (ending October 1, 1981) of a fabric filter installed by Southwestern Public Service Co. on its Harrington Station Unit 2 coal-fired boiler in Amarillo, Texas. Project work during the fourth year concentrated on fabric stud...

211

Fourth Grade Level Science Sample Curriculum.  

ERIC Educational Resources Information Center

This document presents a sample of the Arkansas science curriculum and identifies the content standards for physical science systems, life science systems, and Earth science/space science systems for fourth grade students. Each content standard is explained and includes student learning expectations, fourth grade benchmarks, assessments, and…

Arkansas State Dept. of Education, Little Rock.

212

AGS Broad Band Neutrino Beam.  

National Technical Information Service (NTIS)

We describe the broad band neutrino beam in the north area of the AGS and discuss the calculation of the neutrino flux. The horns were initially designed by Robert Palmer and this beam has been used for almost all neutrino running at the AGS. All of the w...

D. H. White

1985-01-01

213

Gravitational Lensing of Supernova Neutrinos  

SciTech Connect

The black hole at the center of the galaxy is a powerful lens for supernova neutrinos. In the very special circumstance of a supernova near the extended line of sight from Earth to the galactic center, lensing could dramatically enhance the neutrino flux at Earth and stretch the neutrino pulse.

Mena, Olga; /Fermilab /Rome U.; Mocioiu, Irina; /Penn State U.; Quigg, Chris; /Fermilab

2006-10-01

214

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

215

Is Neutrino a Superluminal Particle?  

Microsoft Academic Search

Based on the experimental discovery that the mass-square of neutrino is negative, a quantum theory for superluminal neutrino is proposed. Two Weyl equations coupled together via a mass term respecting the maximum parity violation lead to a new equation which describes the superluminal motion of neutrino with permanent helicity. Various strange features of subluminal and superluminal particles can be ascribed

Guang-jiong Ni; Tsao Chang

2001-01-01

216

Tau events in neutrino telescopes  

Microsoft Academic Search

We discuss the propagation of muon and tauon neutrinos through the inner Earth. In particular, we investigate the effects of crossing the Earth on the spectra of high-energy tauon neutrinos and on generic neutrino flux limits. Finally, we comment on the possibility of carrying out a tomography of the Earth using total event rates.

Christian Hettlage; Karl Mannheim

2001-01-01

217

Physics at a Neutrino Factory  

Microsoft Academic Search

In response to the growing interest in building a Neutrino Factory to produce high intensity beams of electron- and muon-neutrinos and antineutrinos, in October 1999 the Fermilab Directorate initiated two six-month studies. The first study, organized by N. Holtkamp and D. Finley, was to investigate the technical feasibility of an intense neutrino source based on a muon storage ring. This

C. Albright; G. Anderson; V. Barger; R. Bernstein; G. Blazey; A. Bodek; E. Buckley-Geer; A. Bueno; M. Campanelli; D. Carey; D. Casper; A. Cervera; C. Crisan; F. DeJongh; S. Eichblatt; A. Erner; R. Fernow; D. Finley; J. Formaggio; J. Gallardo; S. Geer; M. Goodman; D. Harris; E. Hawker; J. Hill; R. Johnson; D. Kaplan; S. Kahn; B. Kayser; E. Kearns; B. J. King; H. Kirk; J. Krane; D. Krop; Z. Ligeti; J. Lykken; K. McDonald; K. McFarland; I. Mocioiu; J. Morfin; H. Murayama; J. Nelson; D. Neuffer; P. Nienaber; R. Palmer; S. Parke; Z. Parsa; R. Plunkett; E. Prebys; C. Quigg; R. Raja; S. Rigolin; A. Rubbia; H. Schellman; M. Shaevitz; P. Shanahan; R. Shrock; P. Spentzouris; R. Stefanski; J. Stone; L. Sulak; G. Unel; M. Velasco; K. Whisnant; J. Yu; E. D. Zimmerman

2000-01-01

218

Neutrino Mass and New Physics  

Microsoft Academic Search

Reconstruction of the neutrino mass and flavor spectrum is described. Essentially two processes are relevant for interpretation of the neutrino results which were used in determination of neutrino parameters: oscillations (averaged and non-averaged) in vacuum and matter and the adiabatic flavor conversion in matter (the MSW-effect). Detailed physics picture of these processes is elaborated and their realizations in solar and

A. Yu. Smirnov

2006-01-01

219

Neutrino Masses in Superstring Theories  

NASA Astrophysics Data System (ADS)

The author discusses the problems associated with generating small masses for the left-handed physical neutrinos in the superstring E6 theories. He then proposes a solution to this problem, in the context of the intermediate scale scenario. The ranges of the neutrino masses obtained in this way are compatible with those needed for the MSW explanation of the solar neutrino problem.

Nandi, S.

220

Atmospheric electron neutrinos in the MINOS far detector  

SciTech Connect

Neutrinos produced as a result of cosmic-ray interactions in the earth's atmosphere offer a powerful probe into the nature of this three-membered family of low-mass, weakly-interacting particles. Ten years ago, the Super-Kamiokande Experiment has confirmed earlier indications that neutrinos undergo lepton-flavor oscillations during propagation, proving that they are massive contrary to the previous Standard Model assumptions. The Soudan Underground Laboratory, located in northern Minnesota, was host to the Soudan2 Experiment, which has made important contributions to atmospheric neutrino research. This same lab has more recently been host to the MINOS far detector, a neutrino detector which serves as the downstream element of an accelerator-based long-baseline neutrino-oscillation experiment. This thesis has examined 418.5 live days of atmospheric neutrino data (fiducial exposure of 4.18 kton-years) collected in the MINOS far detector prior to the activation of the NuMI neutrino beam, with a specific emphasis on the investigation of electron-type neutrino interactions. Atmospheric neutrino interaction candidates have been selected and separated into showering or track-like events. The showering sample consists of 89 observed events, while the track-like sample consists of 112 observed events. Based on the Bartol atmospheric neutrino flux model of Barr et al. plus a Monte Carlo (MC) simulation of interactions in the MINOS detector, the expected yields of showering and track-like events in the absence of neutrino oscillations are 88.0 {+-} 1.0 and 149.1 {+-} 1.0 respectively (where the uncertainties reflect only the limited MC statistics). Major systematic uncertainties, especially those associated with the flux model, are cancelled by forming a double ratio of these observed and expected yields: R{sup data}{sub trk/shw}/R{sup MC}{sub trk/shw} = 0.74{sup +0.12}{sub -01.0}(stat.) {+-} 0.04 (syst.) This double ratio should be equal to unity in the absence of oscillations, and the value above disfavors null oscillation with 96.0% confidence. In addition, the showering sample can be used to measure the atmospheric neutrino flux. Based on the analysis presented in this thesis, the Bartol flux should be scaled by a factor of: S{sub atm} = 1.08 {+-} 0.12(stat.) {+-} 0.08(syst.) This is larger than, but consistent with, a measurement at the same location by the Soudan2 Experiment of S{sub atm} = 0.91 {+-} 0.07.

Speakman, Benjamin Phillip; /Minnesota U.

2007-01-01

221

Supernova Neutrino-Process and Implication in Neutrino Oscillation  

NASA Astrophysics Data System (ADS)

We studied the supernova nucleosynthesis induced by neutrino interactions and found that several isotopes of rare elements like 7Li, 11B, 138La, 180Ta and many others are predominantly produced by the neutrino-process in core-collapse supernovae. These isotopes are strongly affected by the neutrino flavor oscillation due to the MSW (Mikheyev-Smirnov-Wolfenstein) effect. We here propose a new novel method to determine the unknown neutrino oscillation parameters, ?13 and mass hierarchy simultaneously from the supernova neutrino-process, combined with the r-process for heavy-element synthsis and the Galactic chemical evolution on light nuclei.

Kajino, T.; Aoki, W.; Fujiya, W.; Mathews, G. J.; Yoshida, T.; Shaku, K.; Nakamura, K.; Hayakawa, T.

2012-08-01

222

Search for the Neutrino Mass and Low Energy Neutrino Astronomy  

NASA Astrophysics Data System (ADS)

The history of neutrinos is strongly coupled with the understanding of weak interactions, which in turn rules energy production in stars. Thus there is a important interplay of nuclear-, particle and astrophysics to explain stellar energy production and to disentangle neutrino properties. In addition to terrestrial searches for neutrino masses the article focuses on the discovery and solution of solar neutrinos, a mystery for decades in the field of particle astrophysics. Furthermore, the first detection of supernova neutrinos is described. A discussion of open issues and an outlook into future activities is given.

Zuber, Kai

223

Neutrino dark energy with more than one neutrino species  

SciTech Connect

The mass varying neutrino scenario is a model that successfully explains the origin of dark energy while at the same time solves the coincidence problem. The model is, however, heavily constrained by its stability towards the formation of neutrino bound states when the neutrinos become nonrelativistic. We discuss these constraints and find that natural, adiabatic, stable models with the right amount of dark energy today do not exist. Second, we explain why using the lightest neutrino, which is still relativistic, as an explanation for dark energy does not work because of a feedback mechanism from the heavier neutrinos.

Bjaelde, Ole Eggers; Hannestad, Steen [Department of Physics and Astronomy, University of Aarhus, Ny Munkegade, DK-8000 Aarhus C, Denmark and Center for Cosmology and Particle Physics, Department of Physics, New York University, New York, New York 10003 (United States); Department of Physics and Astronomy, University of Aarhus, Ny Munkegade, DK-8000 Aarhus C (Denmark)

2010-03-15

224

Magnetic moments of active and sterile neutrinos  

NASA Astrophysics Data System (ADS)

Since most of the neutrino parameters are well measured, we illustrate precisely the prediction of the Standard Model, minimally extended to allow massive neutrinos, for the electron neutrino magnetic moment. We elaborate on the effects of light sterile neutrinos on the effective electron neutrino magnetic moment measured at the reactors. We explicitly show that the kinematical effects of the neutrino masses are negligible even for light sterile neutrinos.

Balantekin, A. B.; Vassh, N.

2014-04-01

225

Neutrino magnetic moments and the solar neutrino problem  

SciTech Connect

Present status of the neutrino magnetic moment solutions of the solar neutrino problem is reviewed. In particular, we discuss a possibility of reconciling different degrees of suppression and time variation of the signal (or lack of such a variation) observed in different solar neutrino experiments. It is shown that the resonant spin-flavor precession of neutrinos due to the interaction of their transitions magnetic moments with solar magnetic field can account for all the available solar neutrino data. For not too small neutrino mixing angles (sin 2{theta}{sub o} {approx_gt} 0.2 the combined effect of the resonant spin-flavor precession and neutrino oscillations can result in an observable flux of solar {bar {nu}}{sub e}`s.

Akhmedov, E.Kh. [Washington Univ., Seattle, WA (United States). Inst. for Nuclear Theory]|[Valencia Univ. (Spain). Dept. de Fisica Teorica

1994-08-01

226

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

NASA Astrophysics Data System (ADS)

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

2011-10-01

227

Overview of Neutrino Mixing Models and Their Mixing Angle Predictions  

SciTech Connect

An overview of neutrino-mixing models is presented with emphasis on the types of horizontal flavor and vertical family symmetries that have been invoked. Distributions for the mixing angles of many models are displayed. Ways to differentiate among the models and to narrow the list of viable models are discussed.

Albright, Carl H.

2009-11-01

228

High Energy Neutrino Astronomy  

NASA Astrophysics Data System (ADS)

The short review of theoretical aspects of ultra high energy (UHE) neutrinos. The accelerator sources, such as Supernovae remnants, Gamma Ray Bursts, AGN etc are discussed. The top-down sources include Topological Defects (TDs), Superheavy Dark Matter (SHDM) and Mirror Matter. The diffuse fluxes are considered accordingly as that of cosmogenic and top-down neutrinos. Much attention is given to the cascade upper limit to the diffuse neutrino fluxes in the light of Fermi-LAT data on diffuse high energy gamma radiation. This is most general and rigorous upper limit, valid for both cosmogenic and top-down models. At present upper limits from many detectors are close to the cascade upper limit, and 5 yr IceCube upper limit will be well below it.

Berezinsky, V.

2012-08-01

229

Neutrino Astronomy with Icecube  

NASA Astrophysics Data System (ADS)

IceCube is a kilometer-scale high energy neutrino telescope under construction at the South Pole, a second-generation instrument expanding the capabilities of the AMANDA telescope. The scientific portfolio of IceCube includes the detection of neutrinos from astrophysical objects such as the sources of the cosmic rays, the search for dark matter, and fundamental physics using a very large data set of atmospheric neutrinos. The design and status of IceCube are briefly reviewed, followed by a summary of results to date from AMANDA and initial IceCube results from the 2007 run, with 22 of a planned 86 strings operational. The new infill array known as Deep Core, which will extend IceCube's capabilities to energies as low as 10 GeV, is also described.

Deyoung, Tyce

230

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

231

Sterile Neutrinos and Supernova Nucleosynthesis  

NASA Astrophysics Data System (ADS)

Neutrinos play an important role in the core-collapse supernova environment, from facilitating the explosion mechanism to influencing the outflow's elemental composition. Traditional heavy element nucleosynthesis, the r-process, are stifled by electron neutrinos during the alpha particle formation epoch. Introduction of a sterile neutrino species can temper this alpha effect as well as generate an environment sufficiently neutron-rich for fission cycling to occur. Fission cycling in the r-process produces abundance patterns similar to the halo star data. Here we examine reductions in the neutrino flux necessary to achieve fission cycling; sterile neutrinos or other new physics may realize these reductions.

Beun, Joshua; McLaughlin, Gail; Surman, Rebecca; Hix, Raph

2006-10-01

232

Supernova nucleosynthesis and neutrino oscillation  

NASA Astrophysics Data System (ADS)

Neutrinos play the critical roles in nucleosynthesis of light-to-heavy mass nuclei like 7Li, 11B, 138La and 180Ta in core-collapse supernovae. We find average neutrino temperatures of three flavor neutrinos so that the supernova nucleosynthesis models of the neutrino-process and the r-process can explain the observed solar-system abundance and Galactic chemical evolution of these isotopes. We propose a method to determine the unknown neutrino oscillation parameters ?13 and mass hierarchy by the use of the MSW effects on the supernova nucleosynthesis.

Kajino, T.; Aoki, W.; Cheoun, M.-K.; Chiba, S.; Fujiya, W.; Hayakawa, T.; Mathews, G. J.; Nakamura, K.; Shaku, K.; Yoshida, T.

2012-04-01

233

Testing CPT invariance with neutrinos  

NASA Astrophysics Data System (ADS)

We investigate possible tests of CPT invariance on the level of event rates at neutrino factories. We do not assume any specific model, but phenomenological differences in the neutrino-antineutrino masses and mixing angles in a Lorentz invariance preserving context, which could be induced by physics beyond the Standard Model. We especially focus on the muon neutrino and antineutrino disappearance channels in order to obtain constraints on the neutrino-antineutrino mass and mixing angle differences. In a typical neutrino factory setup simulation, we find, for example, that |m 3 - overlinem3| $?1.9 · 10 -4eV and |? 23 - overline?23|? 2° .

Ohlsson, Tommy

2003-04-01

234

Double-Chooz Neutrino Experiment  

NASA Astrophysics Data System (ADS)

The Double Chooz experiment will use the electron anti-neutrinos produced by the Chooz nuclear power station to search for a non-vanishing value of the ?13 neutrino mixing angle. Double Chooz will be the first of a new generation of neutrino experiments using identical detectors at different distances from the neutrino source to reduce the systematic errors due to the uncertainties on the neutrino flux and to the detector acceptance. The far detector will be operative by the beginning of 2011. Installation of the near detector will occur in 2012.

Palomares, Carmen; Double Chooz Collaboration

2011-12-01

235

Familial multiple lipomatosis.  

PubMed

A clinical study was made of 14 cases of multiple symmetrical lipomata in two families. There were 7 female and 7 male patients. In one family the members affected were observed in four generations. The disease set in during the third or fourth decade of life. The lipomata ranged in size from that of a pea to that of a hen's egg. They were limited to the forearms and trunk were asymptomatic. PMID:71835

Rabbiosi, G; Borroni, G; Scuderi, N

1977-01-01

236

Flavor oscillations of supernova neutrinos  

NASA Astrophysics Data System (ADS)

Neutrinos emitted by core-collapse supernovae (SNe) represent an important laboratory for both particle physics and astrophysics. While propagating in the dense SN environment, they can feel not only the presence of background matter (via ordinary Mikheev-Smirnov-Wolfenstein effects) but also of the gas of neutrinos and antineutrinos (via neutrino-neutrino interaction effects). The MSW effect would imprint on SN neutrinos a track of the shock-wave propagation and of the matter turbulences in the stellar envelope. Moreover, the neutrino-neutrino interactions appear to modify the flavor evolution of SN neutrinos in a collective way, completely different from the ordinary matter effects. In these conditions, the flavor evolution equations become highly nonlinear, sometimes resulting in surprising phenomena when the entire neutrino system oscillates coherently as a single collective mode. In this talk, I will present the recent results on supernova neutrino flavor conversions and I will discuss about the sensitivity of these effects to the ordering of the neutrino mass spectrum.

Mirizzi, Alessandro

2012-08-01

237

Neutrino Oscillation Results from MINOS  

NASA Astrophysics Data System (ADS)

The Main Injector Neutrino Oscillation Search (MINOS) long baseline experiment has been actively taking beam data since 2005, having already accumulated 2.6E20 protons-on-target. MINOS uses the most powerful neutrino beam currently in operation measured in two locations: at Fermilab, close to beam production, and 735 km downstream, in Northern Minnesota. By observing the oscillatory structure in the neutrino energy spectrum, MINOS can make the most precise measurement of the mass-square difference neutrino mixing parameter in the atmospheric sector. In this talk, The latest MINOS neutrino oscillation results are presented, along with a discussion of the MINOS sensitivity to other neutrino oscillation phenomena, such as the nu_mu into nu_e subdominant oscillation mode and oscillations into sterile neutrinos.

Sousa, Alexandre

238

A two parameter four neutrino mixing model with an exchange symmetry of the mass doublet neutrinos  

Microsoft Academic Search

In a model with four neutrino mass eigenstates grouping in two narrow doublets the condition of maximal mixing of the doublet neutrino components leads to a simple 4-neutrino mixing matrix which is related to two connected effective two-neutrino mixing patterns. As a result, large values of the neutrino oscillation amplitudes for both the solar and atmospheric neutrino anomalies appear quite

E. M. Lipmanov

1998-01-01

239

Resonant neutrino activation and neutrino oscillations  

NASA Astrophysics Data System (ADS)

Low Q value weak nuclear decays are considered which have two body final states (electron captures and bound state beta decays, BSD). This permits an analogy with the Mössbauer effect, where the emitted (anti) neutrinos will resonantly activate daughter nuclei in a suitable absorber. Candidates for such a process are examined and the relevant solid state host problems are discussed. We point out that resonant line widths as large as the narrowest observed in Mössbauer spectroscopy suffice to greatly extend the sensitivity of ? [disappearance] oscillation experiments.

Kells, William P.

1983-06-01

240

Resonant neutrino activation and neutrino oscillations  

SciTech Connect

Low Q value weak nuclear decays are considered which have two body final states (electron captures and bound state ..beta.. decays, BSD). This permits an analogy with the Moessbauer effect, where the emitted (anti)neutrinos will resonantly activate daughter nuclei in a suitable absorber. Candidates for such a process are examined and the relevant solid state host problems are discussed. The authors point out that resonant line widths as large as the narrowest observed in Moessbauer spectroscopy suffice to greatly extend the sensitivity of nu (disappearance) oscillation experiments.

Kells, W.P.

1983-01-01

241

Neutrinos from a core collapse supernova  

SciTech Connect

The neutrino burst from a galactic supernova can help determine the neutrino mass hierarchy and {theta}{sub 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.

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

2008-02-21

242

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

243

Neutrino Mass MSW Oscillations & Seesaw Mechanism  

Microsoft Academic Search

In the Hugs 2002 student seminar sessions, I treat a number of topical issues in neutrino physics: the phenomenology of the MSW mechanism; a brief discussion of global analysis of atmospheric and solar neutrinos; Dirac and Majorana neutrino masses and the Seesaw mechanism as an explanation for the smallness of the neutrino mass. MSW model assumes that neutrinos are created

Hasan Yüksel

2004-01-01

244

Decaying Dirac neutrinos. [SN1987a  

SciTech Connect

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.

Acker, A.; Pakvasa, S. (Department of Physics and Astronomy, University of Hawaii at Manoa, Honolulu, Hawaii 96822 (United States)); Pantaleone, J. (Department of Physics, University of California, Riverside, California 92521 (United States))

1992-01-01

245

Massive neutrinos in the standard model and beyond  

NASA Astrophysics Data System (ADS)

The generation of the fermion mass hierarchy in the standard model of particle physics is a long-standing puzzle. The recent discoveries from neutrino physics suggests that the mixing in the lepton sector is large compared to the quark mixings. To understand this asymmetry between the quark and lepton mixings is an important aim for particle physics. In this regard, two promising approaches from the theoretical side are grand unified theories and family symmetries. In the first part of my thesis we try to understand certain general features of grand unified theories with Abelian family symmetries by taking the simplest SU(5) grand unified theory as a prototype. We construct an SU(5) toy model with U(1) F ?Z'2 ?Z'' 2?Z''' 2 family symmetry that, in a natural way, duplicates the observed mass hierarchy and mixing matrices to lowest approximation. The system for generating the mass hierarchy is through a Froggatt-Nielsen type mechanism. One idea that we use in the model is that the quark and charged lepton sectors are hierarchical with small mixing angles while the light neutrino sector is democratic with larger mixing angles. We also discuss some of the difficulties in incorporating finer details into the model without making further assumptions or adding a large scalar sector. In the second part of my thesis, the interaction of high energy neutrinos with weak gravitational fields is explored. The form of the graviton-neutrino vertex is motivated from Lorentz and gauge invariance and the non-relativistic interpretations of the neutrino gravitational form factors are obtained. We comment on the renormalization conditions, the preservation of the weak equivalence principle and the definition of the neutrino mass radius. We associate the neutrino gravitational form factors with specific angular momentum states. Based on Feynman diagrams, spin-statistics, CP invariance and symmetries of the angular momentum states in the neutrino-graviton vertex, we deduce differences between the Majorana and Dirac cases. It is then proved that in spite of the theoretical differences between the two cases, as far as experiments are considered, they would be virtually indistinguishable for any space-time geometry satisfying the weak field condition. We then calculate the transition gravitational form factors for the neutrino by evaluating the relevant Feynman diagrams at 1-loop and estimate a neutrino transition mass radius. The form factor is seen to depend on the momentum transfer very weakly. It is also seen that the neutrino transition mass radius is smaller than the typical neutrino charge radius by a couple of orders of magnitude. In the final part of my thesis, some of the recent neutrino observations and anomalies are revisited, in the context of sterile neutrinos. Among our aims is to understand more clearly some of the analytic implications of the current global neutrino fits from short baseline experiments. Of particular interest to us are the neutrino disappearance measurements from MINOS and the recent indications of a possibly non-vanishing angle, theta13 , from T2K, MINOS and Double-CHOOZ. Based on a general parametrization motivated in the presence of sterile neutrinos, the consistency of the MINOS disappearance data with additional sterile neutrinos is discussed. We also explore the implications of sterile neutrinos for the measurement of | Umu3| in this case. We then turn our attention to the study of |Ue3| extraction in electron neutrino disappearance and appearance measurements. In particular, we study the effects of some of the additional CP phases that appear when there are sterile neutrinos. We observe that the existence of sterile neutrinos may induce a significant modification of the theta13 angle in neutrino appearance experiments like T2K and MINOS, over and above the ambiguities and degeneracies that are already present in 3-neutrino parameter extractions. There are reactor experiments, for instance those measuring nu e disappearance like Double-CHOOZ, Daya Bay and RENO, where this modification is less signific

Thalapillil, Arun Madhav

246

High energy neutrino astrophysics  

NASA Astrophysics Data System (ADS)

Astroparticle physics is a field rich in perspectives in investigating the ultra high energy region which will never be accessible to man-made machines. Many efforts are underway in order to detect the first cosmic neutrinos, messengers of the unobserved universe. The motivations of this field of research, and the current and next future experimental status are reviewed.

Montaruli, Teresa

2005-01-01

247

Experimental Neutrino Physics  

ScienceCinema

In this talk, I will review how a set of experiments in the last decade has given us our current understanding of neutrino properties.  I will show how experiments in the last year or two have clarified this picture, and will discuss how new experiments about to start will address remaining questions.  I will particularly emphasize the relationship between various experimental techniques.

Chris Walter

2010-01-08

248

Low energy neutrinos  

NASA Astrophysics Data System (ADS)

Low energy neutrino investigation has been one of the most active fields of particle physics research over the past decades, accumulating important and sometimes unexpected achievements. In this work some of the most recent impressive successes will be reviewed, as well as the future perspectives of this exciting area of study.

Ranucci, G.; Bellini, G.; Benziger, J.; Bick, D.; Bonfini, G.; Bravo, D.; Buizza Avanzini, M.; Caccianiga, B.; Cadonati, L.; Calaprice, F.; Cavalcante, P.; Chavarria, A.; Chepurnov, A.; D'Angelo, D.; Davini, S.; Derbin, A.; Empl, A.; Etenko, A.; Fomenko, K.; Franco, D.; Galbiati, C.; Gazzana, S.; Ghiano, C.; Giammarchi, M.; Goeger-Neff, M.; Goretti, A.; Grandi, L.; Hagner, C.; Hungenford, E.; Ianni, Al.; Ianni, An.; Kobychev, V.; Korablev, D.; Korga, G.; Kryn, D.; Laubenstein, M.; Lewke, T.; Litvinovich, E.; Loer, B.; Lombardi, F.; Lombardi, P.; Ludhova, L.; Lukyanchenko, G.; Machulin, I.; Manecki, S.; Maneschg, W.; Manuzio, G.; Meindl, Q.; Meroni, E.; Miramonti, L.; Misiaszek, M.; Mllenberg, R.; Mosteiro, P.; Muratova, V.; Oberauer, L.; Obolensky, M.; Ortica, F.; Otis, K.; Pallavicini, M.; Papp, L.; Perasso, L.; Perasso, S.; Pocar, A.; Raghavan, R. S.; Ranucci, G.; Razeto, A.; Re, A.; Romani, A.; Rossi, N.; Saldanha, R.; Salvo, C.; Schönert, S.; Simgen, H.; Skorokhvatov, M.; Smirnov, O.; Sotnikov, A.; Sukhotin, S.; Suvorov, Y.; Tartaglia, R.; Testera, G.; Vignaud, D.; Vogelaar, R. B.; von Feilitzsch, F.; Winter, J.; Wojcik, M.; Wright, A.; Wurm, M.; Xu, J.; Zaimidoroga, O.; Zavatarelli, S.; Zuzel, G.

2014-05-01

249

Lepton family number violation  

SciTech Connect

At present there is evidence from neutrino oscillation searches that the neutrinos are in fact massive particles and that they mix. If confirmed, this would imply that the conservation of LFN is not exact. Lepton family number violation (LFNV) has been searched for with impressive sensitivities in many processes involving charged leptons. The present experimental limits on some of them (those which the author shall consider here) are shown in Table 1. These stringent limits are not inconsistent with the neutrino oscillation results since, given the experimental bounds on the masses of the known neutrinos and the neutrino mass squared differences required by the oscillation results, the effects of LFNV from neutrino mixing would be too small to be seen elsewhere (see Section 2). The purpose of experiments searching for LFNV involving the charged leptons is to probe the existence of other sources of LFNV. Such sources are present in many extensions of the SM. In this lecture the author shall discuss some of the possibilities, focusing on processes that require muon beams. Other LFNV processes, such as the decays of the kaons and of the {tau}, provide complementary information. In the next Section he shall consider some sources of LFNV that do not require an extension of the gauge group of the SM (the added leptons or Higgs bosons may of course originate from models with extended gauge groups). In Section 3 he discusses LFNV in left-right symmetric models. In Section 4 he considers LFNV in supersymmetric models, first in R-parity conserving supersymmetric grand unified models, and then in the minimal supersymmetric standard model with R-parity violation. The last section is a brief summary of the author`s conclusions.

Herczeg, P.

1999-03-01

250

Cloning and characterization of a fourth human somatostatin receptor.  

PubMed Central

We have isolated a gene coding for a fourth human somatostatin (somatotropin release-inhibiting factor) receptor. This additional somatostatin receptor (hSSTR4) is specifically expressed in human fetal and adult brain and lung tissue. The deduced amino acid sequence of the receptor displays both sequence and structural homology to three cloned somatostatin receptors as well as to other members of the family of GTP-binding-protein-coupled seven-helix transmembrane-spanning receptors. Pharmacological characterization of the expressed receptor reveals specific, high-affinity binding of somatostatin 14 and somatostatin 28. Surprisingly, several well-characterized synthetic somatostatin analogs fail to exhibit high-affinity binding to hSSTR4, indicating the existence of pharmacologically different receptor subtypes. Our data suggest that the diverse biological effects exerted by somatostatin are mediated by a family of receptors with discrete patterns of expression and different pharmacological properties. Images Fig. 4

Rohrer, L; Raulf, F; Bruns, C; Buettner, R; Hofstaedter, F; Schule, R

1993-01-01

251

Testing atmospheric mixing sum rules at precision neutrino facilities  

NASA Astrophysics Data System (ADS)

We study the prospects for testing classes of atmospheric mixing sum rules at precision neutrino facilities. Such sum rules, which correlate the atmospheric mixing angle ?23 with the recently measured reactor angle ?13 and the cosine of the oscillation phase ?, are predicted by a variety of semidirect models based on discrete family symmetry classified in terms of finite von Dyck groups. We perform a detailed simulation of the performance of the next generation of oscillation experiments, including the wideband superbeam and low-energy neutrino factory proposals, and compare their discriminating power for testing atmospheric mixing sum rules.

Ballett, Peter; King, Stephen F.; Luhn, Christoph; Pascoli, Silvia; Schmidt, Michael A.

2014-01-01

252

The search for Majorana neutrinos  

NASA Astrophysics Data System (ADS)

In the Standard Model of strong and electroweak interactions, neutrinos are strictly massless due to the absence of the right-handed chiral states and the requirement of gauge invariance and renormalizability. However, recent neutrino oscillation experiments have provided strong evidence that neutrinos are massive and their flavors defined with respect to the charged leptons oscillate, presenting a pressing need for physics beyond the Standard Model. We do not know the nature of mass generation; in particular, we do not know if neutrinos are of Dirac or Majorana type-the former preserves lepton number and the latter violates it by two units. Although the prevailing theoretical prejudice prefers Majorana neutrinos, experimentally testing the Dirac or Majorana nature of neutrinos is of fundamental importance. The unambiguous proof of the existence of a Majorana neutrino is the observation of a lepton number violating process. Since neutrinos interact so weakly and leave no trace in ordinary detectors, the only appropriate signatures must involve two like-sign charged leptons for a process that violates lepton number by two units. To establish the Majorana nature of neutrinos definitively many low energy and collider processes that probe Majorana neutrino masses over many orders of magnitude, from sub-electron-volt to hundreds of giga-electron-volt have been studied.

Atre, Anupama

253

Laboratory Limits on Neutrino Masses  

NASA Astrophysics Data System (ADS)

The recent neutrino oscillation experiments have obtained nonzero differences of squared neutrino masses and therefore proven that neutrinos are massive particles. The values of the neutrino masses have to be determined in a different way. There are two classes of laboratory experiments, both of which have yielded up to now only upper limits on neutrino masses. The direct mass experiments investigate the kinematics of weak decays, obtaining information about the neutrino mass without further requirements. Here, the tritium ? decay experiments give the most stringent results. The search for neutrinoless double ? decay is also very sensitive to the neutrino mass states. However, this search is complementary to direct neutrino mass experiments, since it requires neutrinos to be identical to their antiparticles and probes a linear combination of neutrino masses including complex phases. This chapter is structured as follows. After an introduction in Sect. 2.1, the two approaches are discussed together with the current experimental results in Sects. 2.2 and 2.3, followed by consideration of the outlook for future activities in Sect. 2.4.

Weinheimer, Christian

254

Measurement of atmospheric neutrino oscillations with the ANTARES neutrino telescope  

NASA Astrophysics Data System (ADS)

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 maximal mixing, a mass difference of ?m322=(3.1±0.9)?10-3 eV is obtained, in good agreement with the world average value.

Adrián-Martínez, S.; Al Samarai, I.; Albert, A.; André, 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.; Cârloganu, 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.; Enzenhöfer, A.; Ernenwein, J.-P.; Escoffier, S.; Fehn, K.; Fermani, P.; Ferri, M.; Ferry, S.; Flaminio, V.; Folger, F.; Fritsch, U.; Fuda, J.-L.; Galatà, S.; Gay, P.; Geyer, K.; Giacomelli, G.; Giordano, V.; Gleixner, A.; Gómez-González, J. P.; Graf, K.; Guillard, G.; Hallewell, G.; Hamal, M.; van Haren, H.; Heijboer, A. J.; Hello, Y.; Hernández-Rey, J. J.; Herold, B.; Hößl, 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.; Lefèvre, D.; Lim, G.; Lo Presti, D.; Loehner, H.; Loucatos, S.; Louis, F.; Mangano, S.; Marcelin, M.; Margiotta, A.; Martínez-Mora, J. A.; Meli, A.; Montaruli, T.; Morganti, M.; Moscoso, L.; Motz, H.; Neff, M.; Nezri, E.; Palioselitis, D.; P?v?la?, G. E.; Payet, K.; Petrovic, J.; Piattelli, P.; Popa, V.; Pradier, T.; Presani, E.; Racca, C.; Reed, C.; Riccobene, G.; Richardt, C.; Richter, R.; Rivière, C.; Robert, A.; Roensch, K.; Rostovtsev, A.; Ruiz-Rivas, J.; Rujoiu, M.; Russo, G. V.; Samtleben, D. F. E.; Sánchez-Losa, A.; Sapienza, P.; Schmid, J.; Schnabel, J.; Schöck, F.; Schuller, J.-P.; Schüssler, 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.; Vallée, 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.; Zúñiga, J.; ANTARES Collaboration

2012-08-01

255

Global status of neutrino oscillation parameters after Neutrino-2012  

NASA Astrophysics Data System (ADS)

Here we update the global fit of neutrino oscillations in Refs. [T. Schwetz, M. Tortola, and J. W. F. Valle, New J. Phys. 13, 063004 (2011); T. Schwetz, M. Tortola, and J. W. F. Valle, New J. Phys. 13, 109401 (2011)] including the recent measurements of reactor antineutrino disappearance reported by the Double Chooz, Daya Bay, and RENO experiments, together with latest MINOS and T2K appearance and disappearance results, as presented at the Neutrino-2012 conference. We find that the preferred global fit value of ?13 is quite large: sin?2?13?0.025 for normal and inverted neutrino mass ordering, with ?13=0 now excluded at more than 10?. The impact of the new ?13 measurements over the other neutrino oscillation parameters is discussed as well as the role of the new long-baseline neutrino data and the atmospheric neutrino analysis in the determination of a non-maximal atmospheric angle ?23.

Forero, D. V.; Tórtola, M.; Valle, J. W. F.

2012-10-01

256

Four-neutrino oscillations and the solar neutrino problem  

NASA Astrophysics Data System (ADS)

We perform a fit of solar neutrino data in the framework of the two four-neutrino schemes that are compatible with the results of all neutrino oscillation experiments. These schemes allow simultaneous transitions of solar ? e's into active ? ?'s, ? ?'s and sterile ? s. The data imply that the SMA solution is valid for any combination of ? e? active and ? e? sterile transitions, whereas the LMA, LOW and VO solutions disappear when ? e?? s transitions are dominant.

Giunti, C.; Gonzalez-Garcia, M. C.; Peña-Garay, C.

2001-10-01

257

Neutrino sector with Majorana mass terms and Friedberg-Lee symmetry  

SciTech Connect

We examine a recently proposed symmetry/condition by Friedberg and Lee in a framework where three right-handed neutrinos are added to the spectrum of the three-family minimal standard model. It is found that the right-handed neutrinos are very special, with respect to this symmetry. In the symmetry limit the neutrinos are massless, which could possibly be a hint about why they are light. Imposed as a condition and not as a full symmetry, we find that one of the three right-handed neutrinos simply decouples (has only gravitational interactions) and one of the interacting neutrinos is massless. The possible relation of the model to the seesaw mechanism is briefly discussed.

Jarlskog, C. [Division of Mathematical Physics, LTH, Lund University, Box 118, S-22100 Lund (Sweden)

2008-04-01

258

Neutrino Masses, where do we stand?  

Microsoft Academic Search

I review the status of neutrino physics post-Neutrino~98, including the\\u000aimplications of solar and atmospheric neutrino data, which strongly indicate\\u000anonzero neutrino masses. LSND and the possible role of neutrinos as hot dark\\u000amatter (HDM) are also mentioned. The simplest schemes proposed to reconcile\\u000athese requirements invoke a light sterile neutrino in addition to the three\\u000aactive ones, two of

E W. F. VALLE

1998-01-01

259

When neutrinos attack - the impact of agressive neutrinos in astrophysics.  

NASA Astrophysics Data System (ADS)

Of all the constituents within the standard model of particle physics our understanding of the neutrino has benefited the most from the interaction of astrophysics and `terraphysics'. Much has been learned about the properties of the neutrino from each: experiments here on Earth temper our appreciation of the role that neutrinos play in the cosmos while astrophysics can provide the densities and temperatures in which the neutrinos do more than simply flee. But their reluctance to interact means that it is not until we venture into the most extreme environments of astrophysics that we observe neutrinos pushing back' as hard as they are being pushed'. We review two sites where this occurs: the early Universe and the accretion disk, engines' of gamma ray bursts. Neutrinos play an important role in the evolution of the early Universe with a particular focus upon the electron neutrino in determining the primordial elemental composition via its participation in the most important reaction at that time. Within gamma ray burst accretion disks we again see the electron neutrinos at work in the nuclear reactions and through their function as the coolant' for the disk. Removal of the disk energy, and its deposition into the remnants of the massive star surrounding the disk, may lead to the formation of highly relativistic jets that will later be observed as the burst. We show what has been learned so far about the neutrino and its properties from the study of such environments and discuss where future research is heading.

Kneller, James

2004-11-01

260

Decaying neutrinos and implications from the supernova relic neutrino observation  

NASA Astrophysics Data System (ADS)

We propose that supernova relic neutrino (SRN) observation can be used to set constraints on the neutrino decay models. Because of the long distance scale from cosmological supernovae to the Earth, SRN have possibility to provide much stronger limit than the present one obtained from solar neutrino observation. Since the currently available data are only the upper limit on the flux integrated over E?¯e>19.3 MeV, the decay models on which we can set constraints is quite restricted; they must satisfy specific conditions such that the daughter neutrinos are active species, the neutrino mass spectrum is quasi-degenerate, and the neutrino mass hierarchy is normal. Our numerical calculation clearly indicates that the neutrino decay model with (?2/m,?3/m)<~(1010,1010) [s//eV], where ?i represents the lifetime of mass eigenstates ?¯i, appears to give the SRN flux that is larger than the current upper limit. However, since the theoretical SRN prediction contains many uncertainties concerning a supernova rate in the universe or simulation of supernova explosions, we cannot conclude that there exists the excluded parameter region of the neutrino lifetime. In the near future, further reduced upper limit is actually expected, and it will provide more severe constraints on the neutrino decay models.

Ando, Shin'ichiro

2003-09-01

261

Electron-neutrino survival probability from solar-neutrino data  

NASA Astrophysics Data System (ADS)

With SNO data [SNO Collaboration, nucl-ex/0106015] on electron-neutrino flux from the sun, it is possible to derive the ?e survival probability Pee(E) from existing experimental data of Super-Kamiokande, gallium experiments and Homestake. The combined data of SNO and Super-Kamiokande provide boron ?e flux and the total flux of all active boron neutrinos, giving thus Pee(E) for boron neutrinos. The Homestake detector, after subtraction of the signal from boron neutrinos, gives the flux of Be/+CNO neutrinos, and Pee for the corresponding energy interval, if the produced flux is taken from the Standard Solar Model (SSM). Gallium detectors, GALLEX, SAGE and GNO, detect additionally /pp-neutrinos. The /pp flux can be calculated subtracting from the gallium signal the rate due to boron, beryllium and CNO neutrinos. The ratio of the measured /pp-neutrino flux to that predicted by the SSM gives the survival probability for /pp-neutrinos. Comparison with theoretical survival probabilities shows that the best (among known models) fit is given by LMA and LOW solutions.

Berezinsky, V.; Lissia, M.

2001-11-01

262

Low Energy Neutrino Cross Sections  

NASA Astrophysics Data System (ADS)

Present atmospheric and accelerator based neutrino oscillation experiments operate at low neutrino energies (Ev ~ 1 GeV) to access the relevant regions of oscillation parameter space. As such, they require precise knowledge of the cross sections for neutrino-nucleon interactions in the sub-to-few GeV range. At these energies, neutrinos predominantly interact via quasi-elastic (QE) or single pion production processes, which historically have not been as well studied as the deep inelastic scattering reactions that dominate at higher energies. Data on low energy neutrino cross sections come mainly from bubble chamber, spark chamber, and emulsion experiments that collected their data decades ago. Despite relatively poor statistics and large neutrino flux uncertainties, these measurements provide an important and necessary constraint on Monte Carlo models in present use. The following sections discuss the current status of QE, resonant single pion, coherent pion, and single kaon production cross section measurements at low energy.

Zeller, G. P.

2004-10-01

263

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

264

The number of neutrino species  

Microsoft Academic Search

The authors review the methods used before the operation of the high energy Stanford and CERN e+e- colliders to determine the number of neutrino species Nnu, or an upper limit on this number, within the framework of the Standard Model of light stable neutrinos interacting according to the SU(2)×U(1) universal couplings. The astrophysical limit based on the neutrino burst from

Daniel Denegri; Bernard Sadoulet; Michel Spiro

1990-01-01

265

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

266

An Overview of Neutrino Mixing  

NASA Astrophysics Data System (ADS)

We present a concise review of the recent important experimental developments on neutrino mixing (hints for sterile neutrinos, large ?13, possible non maximal ?23, approaching sensitivity on ?) and their implications on models of neutrino mixing. The new data disfavour many models but the surviving ones still span a wide range going from Anarchy (no structure, no symmetry in the lepton sector) to a maximum of symmetry, as for the models based on discrete non-abelian flavour groups.

Altarelli, G.

2013-08-01

267

Neutrino emission from neutron stars  

Microsoft Academic Search

We review the main neutrino emission mechanisms in neutron star crusts and cores. Among them are the well-known reactions such as the electron–positron annihilation, plasmon decay, neutrino bremsstrahlung of electrons colliding with atomic nuclei in the crust, as well as the Urca processes and neutrino bremsstrahlung in nucleon–nucleon collisions in the core. We emphasize recent theoretical achievements, for instance, band

D. G. Yakovlev; A. D. Kaminker; O. Y. Gnedin; P. Haensel

2001-01-01

268

Quantum coherence of relic neutrinos.  

PubMed

We argue that in at least a portion of the history of the Universe the relic background neutrinos are spatially extended, coherent superpositions of mass states. We show that an appropriate quantum mechanical treatment affects the neutrino mass values derived from cosmological data. The coherence scale of these neutrino flavor wave packets can be an appreciable fraction of the causal horizon size, raising the possibility of spacetime curvature-induced decoherence. PMID:19519016

Fuller, George M; Kishimoto, Chad T

2009-05-22

269

Neutrino Flavor Tagging in a Four-Neutrino Mixing and Oscillation Model  

Microsoft Academic Search

A neutrino mass dominance quantity is introduced for tagging the neutrino\\u000aflavor in the phenomenological two-parameter four neutrino mixing matrix with\\u000atwo neutrino mass doublets and thorough maximal neutrino doublet mixing. While\\u000athere is no hierarchy of the neutrino masses in the neutrino flavor eigenstates\\u000aof this model, it may rather be a special hierarchy of the mass dominance\\u000aratios

E. M. Lipmanov

1999-01-01

270

MINOS atmospheric neutrino contained events  

SciTech Connect

The Main Injector Neutrino Oscillation Search (MINOS) experiment has continued to collect atmospheric neutrino events while doing a precision measurement of NuMI beam {nu}{sub {mu}} disappearance oscillations. The 5.4 kton iron calorimeter is magnetized to provide the unique capability of discriminating between {nu}{sub {mu}} and {bar {nu}}{sub {mu}} interactions on an event-by-event basis and has been collecting atmospheric neutrino data since July 2003. An analysis of the neutrino events with interaction vertices contained inside the detector will be presented.

Habig, A.; /Minnesota U.

2007-10-01

271

Supernova neutrinos and explosive nucleosynthesis  

NASA Astrophysics Data System (ADS)

Core-collapse supernovae eject huge amount of flux of energetic neutrinos. We studied the explosive nucleosyn-thesis in supernovae and found that several isotopes 7Li, 11B, 92Nb, 138La and 180Ta 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 ?13, simultaneously. There is recent evidence that SiC X grains from the Murchison meteorite may contain supernova-produced light elements 11B and 7Li encapsulated in the presolar grains. Combining the recent experimental constraints on ?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.; Aoki, W.; Cheoun, M.-K.; Hayakawa, T.; Hidaka, J.; Hirai, Y.; Mathews, G. J.; Nakamura, K.; Shibagaki, S.; Suzuki, T.

2014-05-01

272

Solar Neutrino Results from Sage  

NASA Astrophysics Data System (ADS)

Since January of 1990, the Russian-American Solar neutrino Experiment has carried out measurements of the capture rate of solar neutrinos on metallic gallium in a radiochemical experiment at the Baksan Neutrino Observatory. The measured capture rate from the 71Ge K- and L-peak counting data through December 2000 is 77.0 +7.1/-6.9 SNU, where the uncertainties statistical and systematic, respectively. This result represents a 6 depression in the neutrino flux compared with predicted Standard Solar Model rates. The experimental procedures and data analysis are presented.

Gavrin, Vladimir N.

2003-02-01

273

Review of Neutrino Mass Measurements  

SciTech Connect

After a brief summary of the recent achievements of neutrino physics, the concept of neutrino mass scale is clarified. The methods for the determination of the neutrino mass values are summarized and critically compared, in particular in the different and complementary contexts of cosmology, double and single beta decay. The attention is then focussed on the laboratory approaches to investigate neutrino mass. The role of neutrinoless double beta decay is explained and a short review of the present and most promising future experiments in this field is given. Single beta decay sensitivity is discussed, with brief descriptions of the KATRIN tritium experiment and of the recently proposed MARE rhenium project.

Giuliani, A. [Universita dell' Insubria, Via Valleggio 11, I-22100 Como (Italy); INFN-Milano, Via Valleggio 11, I-22100 Como (Italy)

2006-02-08

274

Phenomenology of pseudo Dirac neutrinos  

NASA Astrophysics Data System (ADS)

We formulate general conditions on /3×3 neutrino mass matrices under which a degenerate pair of neutrinos at a high scale would split at low scale by radiative corrections involving only the standard model fields. This generalizes the original observations of Wolfenstein on pseudo Dirac neutrinos to three generations. A specific model involving partially broken discrete symmetry and solving the solar and atmospheric anomalies is proposed. The symmetry pattern of the model naturally generates two large angles one of which can account for the large angle MSW solution to the solar neutrino problem.

Joshipura, A. S.; Rindani, S. D.

2000-11-01

275

Non-thermal leptogenesis from the heavier Majorana neutrinos  

NASA Astrophysics Data System (ADS)

We investigate a scheme for making leptogenesis by means of the /CP violating decays of the seesaw Majorana neutrinos proposed by Fukugita and Yanagida. However, in order to avoid the wash-out of the produced lepton number we propose the production of the Majorana neutrinos to occur non-thermally and sufficiently late. After this time, in consequence, the /B-L (baryon minus lepton) quantum number becomes a good ``accidental symmetry'' protecting the asymmetry produced. This non-thermal leptogenesis at late time is realized by a boson decaying into the Majorana neutrinos with a long lifetime. Suggestively this boson could correspond to a scalar field which causes the cosmic inflation, the inflaton, and thus its decay means really the reheating of the Universe. We find that this mechanism works well even if the lightest Majorana neutrinos are not produced sufficiently or not present, and the decays of the heavier seesaw Majorana neutrinos can be responsible to the baryon asymmetry in the present Universe, as we illustrate by the example of the family replicated gauge group model.

Asaka, T.; Nielsen, H. B.; Takanishi, Y.

2002-12-01

276

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

277

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

278

Coherent Neutrino Scattering  

NASA Astrophysics Data System (ADS)

We present a microscopic model for coherent pion production off nuclei induced by neutrinos. This model is built upon a model for single nucleon processes that goes beyond the usual Delta dominance by including non resonant background contributions. We include nuclear medium effects: medium corrections to Delta properties and outgoing pion absorption via an optical potential. This results in major modifications to cross-sections for low energy experiments when compared with phenomenological models like Rein-Sehgal's.

Valverde, M.; Amaro, J. E.; Hernandez, E.; Nieves, J.

2009-09-01

279

Baryogenesis via Neutrino Oscillations  

Microsoft Academic Search

We propose a new mechanism of leptogenesis in which the asymmetries in lepton\\u000anumbers are produced through the CP-violating oscillations of ``sterile''\\u000a(electroweak singlet) neutrinos. The asymmetry is communicated from singlet\\u000aneutrinos to ordinary leptons through their Yukawa couplings. The lepton\\u000aasymmetry is then reprocessed into baryon asymmetry by electroweak sphalerons.\\u000aWe show that the observed value of baryon asymmetry

E. Kh; V. A. Rubakov; A. Yu. Smirnov

1998-01-01

280

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

281

Neutrino Mass MSW Oscillations & Seesaw Mechanism  

NASA Astrophysics Data System (ADS)

In the Hugs 2002 student seminar sessions, I treat a number of topical issues in neutrino physics: the phenomenology of the MSW mechanism; a brief discussion of global analysis of atmospheric and solar neutrinos; Dirac and Majorana neutrino masses and the Seesaw mechanism as an explanation for the smallness of the neutrino mass. MSW model assumes that neutrinos are created in flavor eigenstates without any definite mass but they evolve in mass eigenstates with definite mass. Latest experiments confirms the neutrino oscillations. Considering MSW oscillations in calculations provides an acceptable solution for measured neutrino flux deficiency in solar and atmospheric neutrinos. Neutrinos do not have mass in the standard model. Experimentally, it is known that neutrino mass is exceedingly small, if not zero. The seesaw mechanism predicts left handed light neutrinos with right handed heavy partners.

Yüksel, Hasan

2004-03-01

282

Probing New Physics With Neutrino Interactions At The Pierre Auger Observatory  

SciTech Connect

The energy of the shower produced through neutrino-nucleon interactions depends on the neutrino flavor and the type of interaction. Electron neutrinos undergoing CC interactions produce a shower with both an electromagnetic and hadronic component: Esh,em=(1-y)Ev, Esh,had=yEv. Muon neutrinos undergoing CC interactions, along with all neutrino flavors undergoing NC interactions, produce a hadronic shower with an energy, Esh,had=Ev. Charged current interactions of tau neutrino are somewhat more complicated. The tau lepton produced in the initial CC neutrino interaction with sufficiently high energy generate a second hadronic shower from the tau decay spatially separated from the initial one, identifiable as a ''double bang'' event. The Auger capability for seeing these events allows to restrict models where non-perturbative effects are present, which induce an enhancement in the neutrino-nucleon cross-section (e.g. low-scale Quantum Gravity, EW instantons). We are interested to study EW-instantons, both the Standard Model as well as in an extension of the type SU(2)1 x SU(2)2 x U(1)Y, where the influence of new physics is only in the third family.

Diaz-Cruz, L.; Salazar, H. [Fac. de Ciencias Fisico-Matematicas, BUAP. Apdo. Postal 1364, C.P. 72000 Puebla, Pue. (Mexico); Pedraza-Morales, M. I.; Rosado, A. [Instituto de Fisica, BUAP. Apdo. Postal J-48 Col. San Manuel, C.P. 72570 Puebla, Pue. (Mexico)

2006-09-25

283

Neutrino physics at LAMPF  

SciTech Connect

There are three neutrino experiments at LAMPF in various stages of completion or development. E225, the study of electron-neutrino electron scattering, which completed data taking in December 1986 and has just about completed all its analysis. E645, a search for /bar /nu///sub ..mu../ ..-->.. /bar /nu///sub e/ oscillation, is in its third and final year of data taking. The Large Cerenkov Detector (LCD), associated with E1015, has undergone extensive scientific and technical review and we are presently trying to obtain the necessary funds to build the detector, beam line, and target. In the following, each of these experiments will be briefly discussed. Before doing so, it is useful to show the characteristics of the neutrino spectrum resulting from the decay of ..pi../sup +/ at rest. It is also useful to realize that, on average, an 800-MeV proton from LAMPF produces about 0.1 ..pi../sup +/ decaying at rest. 16 refs., 5 figs., 4 tabs.

Garvey, G.T.

1989-01-01

284

Neutrino Oscillations:. Hierarchy Question  

NASA Astrophysics Data System (ADS)

The only experimentally observed phenomenon that lies outside the standard model of the electroweak interaction is neutrino oscillations. A way to try to unify the extensive neutrino oscillation data is to add a phenomenological mass term to the Lagrangian that is not diagonal in the flavor basis. The goal is then to understand the world's data in terms of the parameters of the mixing matrix and the differences between the squares of the masses of the neutrinos. An outstanding question is what is the correct ordering of the masses, the hierarchy question. We point out a broken symmetry relevant to this question, the symmetry of the simultaneous interchange of hierarchy and the sign of ?13. We first present the results of an analysis of data that well determine the phenomenological parameters but are not sensitive to the hierarchy. We find ?13 = 0.152±0.014, ? 23 = 0.25{ - 0.05}{ + 0.03} ? and ?32 = 2.45±0.14×10-3 eV2, results consistent with others. We then include data that are sensitive to the hierarchy and the sign of ?13. We find, unlike others, four isolated minimum in the ?2-space as predicted by the symmetry. Now that Daya Bay and RENO have determined ?13 to be surprisingly large, the Super-K atmospheric data produce meaningful symmetry breaking such that the inverse hierarchy is preferred at the 97.2 % level.

Ernst, D. J.; Cogswell, B. K.; Burroughs, H. R.; Escamilla-Roa, J.; Latimer, D. L.

2014-09-01

285

Boxing with neutrino oscillations  

NASA Astrophysics Data System (ADS)

We develop a characterization of neutrino oscillations based on the coefficients of the oscillating terms. These coefficients are individually observable; although they are quartic in the elements of the unitary mixing matrix, they are independent of the conventions chosen for the angle and phase parametrization of the mixing matrix. We call these reparametrization-invariant observables ``boxes'' because of their geometric relation to the mixing matrix, and because of their association with the Feynman box diagram that describes oscillations in field theory. The real parts of the boxes are the coefficients for the CP- or T-even oscillation modes, while the imaginary parts are the coefficients for the CP- or T-odd oscillation modes. Oscillation probabilities are linear in the boxes, so measurements can straightforwardly determine values for the boxes (which can then be manipulated to yield magnitudes of mixing matrix elements). We examine the effects of unitarity on the boxes and discuss the reduction of the number of boxes to a minimum basis set. For the three-generation case, we explicitly construct the basis. Using the box algebra, we show that CP violation may be inferred from measurements of neutrino flavor mixing even when the oscillatory factors have averaged. The framework presented here will facilitate general analyses of neutrino oscillations among n>=3 flavors.

Wagner, D. J.; Weiler, Thomas J.

1999-06-01

286

Neutrino self-energy operator and neutrino magnetic moment  

SciTech Connect

A simple method for calculating the magnetic moment of a massive neutrino on the basis of its self-energy operator is presented. An expression for the magnetic moment of a massive neutrino in an external electromagnetic field is obtained in the R{sub {xi}} gauge for the case of an arbitrary ratio of the lepton and W-boson masses.

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

2013-11-15

287

Neutrino Oscillations and the Anomalous Atmospheric Neutrino Flux.  

National Technical Information Service (NTIS)

We re-analyze the constraints on atmospheric nu /sub e/ and nu /sub mu / fluxes due to three-neutrino oscillations and investigate the anomalous neutrino fluxes recently observed at Kamiokande. We find that it is difficult to explain the data by nu /sub e...

K. Hidaka M. Honda S. Midorikawa

1988-01-01

288

Neutrino self-energy operator and neutrino magnetic moment  

NASA Astrophysics Data System (ADS)

A simple method for calculating the magnetic moment of a massive neutrino on the basis of its self-energy operator is presented. An expression for the magnetic moment of a massive neutrino in an external electromagnetic field is obtained in the R ? gauge for the case of an arbitrary ratio of the lepton and W-boson masses.

Dobrynina, A. A.; Mikheev, N. V.; Narynskaya, E. N.

2013-11-01

289

Resonant solar neutrino oscillation versus laboratory neutrino oscillation experiments  

SciTech Connect

The interplay between resonant solar neutrino oscillations and neutrino oscillations in laboratory experiments is investigated in a 3 generation model. Due to the assumed hierarchy of neutrino masses, together with our choice of a convenient parameterization of the 3 generation mixing matrix, we can derive a simple analytic formula which reduces the solar neutrino problem to an effective 2 generation problem. The reduction makes it apparent that the allowed range of mixing and mass parameters crucially depend on whether the survival probability of solar neutrinos S satisfies S greater than or equal to 1/3 or not. The formulae for probabilities of laboratory neutrino oscillations are also greatly simplified. We argue that a combination of the observed solar neutrino depletion and data obtained from reactor experiments seems to rule out some range of neutrino masses. If a sizable nu/sub ..mu../ ..-->.. nu/sub e/ oscillation is observed at accelerators, as suggested at this Workshop, it severely restricts the range of 2 mixing angles.

Lim, Chong-Sa

1987-02-01

290

A minimal model of neutrino flavor  

NASA Astrophysics Data System (ADS)

Models of neutrino mass which attempt to describe the observed lepton mixing pattern are typically based on discrete family symmetries with a non-Abelian and one or more Abelian factors. The latter so-called shaping symmetries are imposed in order to yield a realistic phenomenology by forbidding unwanted operators. Here we propose a supersymmetric model of neutrino flavor which is based on the group T 7 and does not require extra {Z} N or U(1) factors in the Yukawa sector, which makes it the smallest realistic family symmetry that has been considered so far. At leading order, the model predicts tribimaximal mixing which arises completely accidentally from a combination of the T 7 Clebsch-Gordan coefficients and suitable flavon alignments. Next-to-leading order (NLO) operators break the simple tribimaximal structure and render the model compatible with the recent results of the Daya Bay and Reno collaborations which have measured a reactor angle of around 9°. Problematic NLO deviations of the other two mixing angles can be controlled in an ultraviolet completion of the model. The vacuum alignment mechanism that we use necessitates the introduction of a hidden flavon sector that transforms under a {Z} 6 symmetry, thereby spoiling the minimality of our model whose flavor symmetry is then T 7 × {Z} 6.

Luhn, Christoph; Parattu, Krishna Mohan; Wingerter, Ak?n

2012-12-01

291

Excited neutrino production by ultrahigh energy neutrinos traversing the Earth  

NASA Astrophysics Data System (ADS)

We focus on the production of excited neutrinos by ultra high energy (UHE, E?>104GeV) neutrinos traversing the Earth. The surviving neutrino fluxes are calculated using the complete system of transport equations for ordinary neutrinos and their excited states, and we compare these results with the obtained using only Standard Model (SM) interactions. We extend the analysis by including the neutral current (NC) and decay regeneration effects, and computing the surviving flux for different values of f/?, where ? is the compositeness scale and f a coupling factor representing non-perturbative physics. Finally, we analyze the possibilities of detecting such fluxes in a neutrino telescope such as IceCube showing the allowed regions in the (m*,f/?) plane for two possible initial fluxes. We have considered the IC80 configuration of IceCube for an operation time of ten years.

Reynoso, Matías M.; Romero, Ismael; Sampayo, Oscar A.

2012-12-01

292

Neutrino-nucleus coherent scattering as a probe of neutron density distributions  

NASA Astrophysics Data System (ADS)

Neutrino-nucleus coherent elastic scattering provides a theoretically appealing way to measure the neutron part of the associated form factor. We show, using an expansion of the form factor into moments, that neutrinos from stopped muons can probe not only the second moment of the form factor (the neutron radius) but also the fourth moment. Using simple Monte Carlo techniques for Argon, Germanium, and Xenon detectors of 25 tonnes, 10 tonnes, and 3 tonnes, respectively, we show that the neutron radii could be found with an uncertainty of a few percent. If the luminosity of the neutrino flux is known independently, it is possible to discriminate between the predictions of various Skyme models as well.

Patton, Kelly; Engel, Jon; McLaughlin, Gail

2011-10-01

293

Overview of neutrino mixing results from accelerator-based neutrino experiments  

NASA Astrophysics Data System (ADS)

Over the past fifteen years, many experiments have provided definitive evidence for neutrino flavor change. This talk briefly highlighted the experimental results and what constraints they place on neutrino masses and mixing. While the observed effects can often be described by mixing between two neutrino flavors, the current generation neutrino oscillation experiments are becoming increasingly sensitive to the mixing between all three neutrino flavors.

Marino, A. D.

2013-10-01

294

NESTOR: Deep underwater neutrino astronomy.  

National Technical Information Service (NTIS)

NESTOR is the first step toward the construction of a neutrino telescope using the depth of the sea both as a shield against atmospheric muons and as detector material. The experiment is based on the detection of Cerenkov radiation produced by neutrino mu...

L. Trasatti

1997-01-01

295

The emergence of neutrino astronomy  

NASA Astrophysics Data System (ADS)

This paper is a brief historical review of the quest to find neutrinos of extraterrestrial origin. In the context of the Victor Hess centenary, it is interesting to consider how the development of detectors for neutrinos from space relates to developments in cosmic-ray and particle physics over the same time span.

Gaisser, Thomas K.

2013-02-01

296

The Mystery of Neutrino Mixings  

NASA Astrophysics Data System (ADS)

In the last years we have learnt a lot about neutrino masses and mixings. Neutrinos are not all massless but their masses are very small. Probably masses are small because neutrinos are Majorana particles with masses inversely proportional to the large scale M of lepton number (L) violation, which turns out to be compatible with the GUT scale. We have understood that there is no contradiction between large neutrino mixings and small quark mixings, even in the context of GUTs and that neutrino masses fit well in the SUSY GUT picture. Out of equilibrium decays with CP and L violation of heavy RH neutrinos can produce a B-L asymmetry, then converted near the weak scale by instantons into an amount of B asymmetry compatible with observations (baryogenesis via leptogenesis). It appears that active neutrinos are not a significant component of Dark Matter in the Universe. A long list of models have been formulated over the years to understand neutrino masses and mixings. With the continuous improvement of the data most of the models have been discarded by experiment. The surviving models still span a wide range going from a maximum of symmetry, with discrete non-abelian flavour groups, to the opposite extreme of anarchy.

Altarelli, Guido

2013-07-01

297

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

298

Neutrino astronomy: Present and future  

NASA Astrophysics Data System (ADS)

I briefly review the present and future status of the burgeoning field of neutrino astronomy. I outline the astrophysics and particle physics goals, design, and performance of the various current and proposed neutrino telescopes. Also described are present results and future expectations.

McCauley, Thomas

2006-10-01

299

Coherent lunar effect on solar neutrino  

Microsoft Academic Search

Coherent interaction of solar neutrino with the moon and its implication are investigated. We solve the Dirac equation with the moon potential and show that a phase shift of the neutrino wave function becomes almost one unit if the neutrino penetrates the moon. Spatial interference is generated for the neutrino wave packets during eclipse and possibility of observing interference effect

K. Ishikawa; T. Shimomura

2005-01-01

300

Probing thermonuclear supernova explosions with neutrinos  

Microsoft Academic Search

Aims: We present neutrino light curves and energy spectra for two representative type Ia supernova explosion models: a pure deflagration and a delayed detonation. Methods: We calculate the neutrino flux from beta processes using nuclear statistical equilibrium abundances convoluted with approximate neutrino spectra of the individual nuclei and the thermal neutrino spectrum (pair+plasma). Results: Although the two considered thermonuclear supernova

A. Odrzywolek; T. Plewa

2011-01-01

301

Neutrino-helium ionizing collisions: Electromagnetic contribution  

NASA Astrophysics Data System (ADS)

In terrestrial experiments searching for neutrino magnetic moments one investigates the ionization channel in the neutrino-atom scattering. We present numerical calculations that disprove the recent theoretical claim about large enhancement of the electromagnetic-interaction contribution to the neutrino impact ionization of helium relative to the case of the neutrino scattering on free electrons.

Kouzakov, Konstantin A.; Rodina, Yulia A.; Studenikin, Alexander I.

2014-04-01

302

Neutrino mass models and CP violation  

SciTech Connect

Theoretical ideas on the origin of (a) neutrino masses (b) neutrino mass hierarchies and (c) leptonic mixing angles are reviewed. Topics discussed include (1) symmetries of neutrino mass matrix and their origin (2) ways to understand the observed patterns of leptonic mixing angles and (3)unified description of neutrino masses and mixing angles in grand unified theories.

Joshipura, Anjan S. [Physical Research Laboratory, Navarangpura, Ahmedabad, 380 009 (India)

2011-10-06

303

Neutrino oscillation results from MINOS  

SciTech Connect

The Main Injector Neutrino Oscillation Search (MINOS) long-baseline experiment has been actively collecting beam data since 2005, having already accumulated 3 x 10{sup 20} protons-on-target (POT). MINOS uses the Neutrinos at the Main Injector (NuMI) neutrino beam measured in two locations: at Fermilab, close to beam production, and 735 km downstream, in Northern Minnesota. By observing the oscillatory structure in the neutrino energy spectrum, MINOS can precisely measure the neutrino oscillation parameters in the atmospheric sector. These parameters were determined to be |{Delta}m{sub 32}{sup 2}| = 2.74{sub -0.26}{sup +0.44} x 10{sup -3} eV{sup 2}/c{sup 4} and sin{sup 2}(2{theta}{sub 23}) > 0.87 (68% C.L.) from analysis of the first year of data, corresponding to 1.27 x 10{sup 20} POT.

Sousa, Alexandre; /Oxford U.

2007-08-01

304

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

305

Review of Reactor Neutrino Oscillation Experiments  

NASA Astrophysics Data System (ADS)

In this document we will review the current status of reactor neutrino oscillation experiments and present their physics potentials for measuring the ?13 neutrino mixing angle. The neutrino mixing angle ?13 is currently a high-priority topic in the field of neutrino physics. There are currently three different reactor neutrino experiments, DOUBLE CHOOZ, DAYA BAY and RENO and a few accelerator neutrino experiments searching for neutrino oscillations induced by this angle. A description of the reactor experiments searching for a nonzero value of ?13 is given, along with a discussion of the sensitivities that these experiments can reach in the near future.

Mariani, C.

306

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

307

A fourth planet orbiting upsilo Andromedae  

Microsoft Academic Search

We present a 4-planet Keplerian fit for the radial velocity curve of the F8V star upsilo Andromeda, indicating the presence of a fourth planet in the system. We detect an additional fifth coherent signal in the radial velocity curve which we attribute to stellar activity. The discovery of a new planet around upsilo Andromedae makes this system the fifth to

S. Curiel; J. Cantó; L. Georgiev; C. E. Chávez; A. Poveda

2011-01-01

308

Fourth Annual Clinical Diabetes Technology Meeting.  

National Technical Information Service (NTIS)

The Fourth Annual Clinical Diabetes Technology Meeting was presented by the Diabetes Technology Society at the Orlando Florida Hyatt Regency Hotel on April 11-12 2008. The first day covered Technologies for Diabetes Monitoring and the second day covered T...

D. C. Klonoff

2008-01-01

309

Singapore: The Fourth Way in Action?  

ERIC Educational Resources Information Center

This article has two main objectives. It first outlines the first three waves of change termed by Hargreaves and Shirley (The Fourth Way: The inspiring future for educational change. Thousand Oaks, CA: Corwin Press, "2009") as the First, Second and Third Way that defined global educational policy and practice since the 1960s. It then introduces…

Hargreaves, Andy

2012-01-01

310

A fourth hominin skull from Dmanisi, Georgia  

Microsoft Academic Search

Newly discovered Homo remains, stone artifacts, and animal fossils from Dmanisi, Republic of Georgia, provide a basis for better understand- ing patterns of hominin evolution and behavior in Eurasia ca. 1.77 mil- lion years ago. Here we describe a fourth skull that is nearly complete, lacking all but one of its teeth at the time of death. Both the maxillae

David Lordkipanidze; Abesalom Vekua; Reid Ferring; G. Philip Rightmire; Christoph P. E. Zollikofer; Marcia S. Ponce de León; Jordi Agusti; Gocha Kiladze; Alexander Mouskhelishvili; Medea Nioradze; Martha Tappen

2006-01-01

311

Business Management for Independent Schools. Fourth Edition.  

ERIC Educational Resources Information Center

This fourth edition of a guide for independent school business managers has been produced in looseleaf format so that changes may be made promptly as decisions of regulatory bodies require modifications in current practice. Fourteen chapters are organized under three broad topic headings. Chapters in part 1, Accounting and Financial Reporting,…

National Association of Independent Schools, Boston, MA.

312

Vocabulary Strategies for a Fourth Grade Classroom  

ERIC Educational Resources Information Center

For this project I worked with twelve of my fourth grade students from a local school in the southwestern part of Stokes County, North Carolina on increasing their vocabulary skills through the development and implementation of seven vocabulary strategies. During the Literature Review I came across the following seven strategies: Prediction;…

Howell, Gina

2012-01-01

313

Survey of Instructional Development Models. Fourth Edition.  

ERIC Educational Resources Information Center

This text, now in its fourth edition, provides an understanding of the diversity and use of models used to portray the instructional development (ID) process, while reflecting the many changes in the field that have occurred since publication of the last edition in 1997. Beginning with the belief that an ID model should be selected based on the…

Gustafson, Kent L.; Branch, Robert Maribe

314

Gross Domestic Product: Fourth Quarter 1999  

NSDL National Science Digital Library

A news release from the BEA reports that, in the fourth quarter of 1999, real gross domestic product continued to increase at an annual rate of 5.8 percent. Factors contributing to the rise included increases in personal consumption expenditures, government spending, inventory investment, and exports.

315

Sex Differences in Cognitive Abilities. Fourth Edition  

ERIC Educational Resources Information Center

The fourth edition of "Sex Differences in Cognitive Abilities" critically examines the breadth of research on this complex and controversial topic, with the principal aim of helping the reader to understand where sex differences are found--and where they are not. Since the publication of the third edition, there have been many exciting and…

Halpern, Diane F.

2011-01-01

316

Children, Play, and Development. Fourth Edition  

ERIC Educational Resources Information Center

Children, Play, and Development, Fourth Edition, discusses the relationship of play to the physical, social, intellectual, and emotional growth of the child. Author Fergus P. Hughes focuses on the historical, sociocultural, and ethological context of play; the role of development in play; and the wide range of theories that provide a framework for…

Hughes, Fergus P.

2010-01-01

317

Extended Mass Layoffs, Fourth Quarter 1998  

NSDL National Science Digital Library

Data from the fourth quarter 1998 release from the BLS, Extended Mass Layoffs, reveals that 1,660 mass layoff actions by employers resulted in 342,010 worker-job separations of more than 30 days from October through December of 1998.

318

Collective neutrino oscillations in turbulent backgrounds  

SciTech Connect

Using a Kolmogorov turbulence model, we investigate the effects of fluctuations in matter and neutrino density in the region near a supernova core on the flavor oscillations of neutrinos emitted in the core collapse in a single-angle, two-flavor approximation. Deviation from a smooth background neutrino density causes significant alterations in the final flavor state of the neutrino ensemble after 400 km, but even very large fluctuations in the matter density do not strongly affect the state of the neutrinos after the collective phase. In both cases, there is a strong effect on the neutrino flavor evolution at intermediate radii, with the flavor evolution becoming much more chaotic. The effect of fluctuations also depends strongly on the initial neutrino spectra. We conclude that the true neutrino fluxes arriving at Earth from core-collapse supernova could differ considerably from predictions of neutrino fluxes based on approximate models with smoothly decreasing matter and neutrino densities.

Reid, Giles; Adams, Jenni; Seunarine, Suruj [University of Canterbury, Christchurch (New Zealand); University of the West Indies, Bridgetown (Barbados)

2011-10-15

319

Family Policies and Children's School Achievement in Single- versus Two-Parent Families.  

ERIC Educational Resources Information Center

Investigates the gap in math and science achievement of third- and fourth-graders who live with a single parent versus those who live with two parents in 11 countries. Finds single parenthood to be less detrimental when family policies equalize resources between single- and two-parent families. Concludes that national family policies can offset…

Pong, Suet-Ling; Dronkers, Jaap; Hampden-Thompson, Gillian

2003-01-01

320

A search for supernova neutrinos with the Sudbury Neutrino Observatory  

NASA Astrophysics Data System (ADS)

The Sudbury Neutrino Observatory (SNO) is an underground Cerenkov detector designed to detect neutrinos from astrophysical sources. The fiducial mass of the detector consists of 1000 tonnes of D2O, which provides sensitivity to all neutrino flavours. Since much of the energy released in the supernova burst is expected to be carried by the muon and tau neutrinos, the supernova signal recorded by the SNO detector is of particular importance. In addition, SNO is also sensitive to the prompt electron neutrino signal expected from capture processes during core collapse. Various supernova models are investigated and predictions of the SNO supernova signal are studied using simulated Monte Carlo data. A data analysis program to identify neutrinos from a galactic supernova burst has been installed in the online system at SNO. The program automatically analyzes burst data and it is anticipated that a manual alert to the Supernova Early Warning System could be issued within 20--30 minutes with negligible possibility of a false alarm. The burst identification algorithm currently in use both online and offline provides detection sensitivity beyond the far edge of our galaxy. A search for supernova neutrinos was performed using 241.0 days of data collected over the time period between November 2, 1999 and January 4, 2001. No candidate bursts were observed over this period, which places a 90% confidence level upper limit of <3.5 galactic supernovae per year.

Heise, Jaret Curt

321

Why do Majorana Neutrinos Run Faster than Dirac Neutrinos?  

NASA Astrophysics Data System (ADS)

The ?-lepton dominance in the one-loop renormalization-group equations (RGEs) of neutrinos sets a cute criterion to parametrize the 3x3 lepton flavor mixing matrix U: its elements U_{3i} (for i=1,2,3) should be as simple as possible. Such a novel parametrization is different from the ``standard" one used in the literature and can lead to greatly simplified RGEs for three mixing angles and the physical CP-violating phase(s), no matter whether neutrinos are Dirac or Majorana particles. We show that the RGEs of Dirac neutrinos are not identical with those of Majorana neutrinos even if two Majorana CP-violating phases vanish. As the latter can keep vanishing from the electroweak scale to the typical seesaw scale, it makes sense to explore the similarities and differences between the RGE running effects of Dirac and Majorana neutrinos. We conclude that Majorana neutrinos are in general expected to run faster (i.e., more significantly) than Dirac neutrinos.

Xing, Zhi-Zhong Zhang, He

2006-05-01

322

Summary of the Fourth AIAA CFD Drag Prediction Workshop  

NASA Technical Reports Server (NTRS)

Results from the Fourth AIAA Drag Prediction Workshop (DPW-IV) are summarized. The workshop focused on the prediction of both absolute and differential drag levels for wing-body and wing-body-horizontal-tail configurations that are representative of transonic transport air- craft. Numerical calculations are performed using industry-relevant test cases that include lift- specific flight conditions, trimmed drag polars, downwash variations, dragrises and Reynolds- number effects. Drag, lift and pitching moment predictions from numerous Reynolds-Averaged Navier-Stokes computational fluid dynamics methods are presented. Solutions are performed on structured, unstructured and hybrid grid systems. The structured-grid sets include point- matched multi-block meshes and over-set grid systems. The unstructured and hybrid grid sets are comprised of tetrahedral, pyramid, prismatic, and hexahedral elements. Effort is made to provide a high-quality and parametrically consistent family of grids for each grid type about each configuration under study. The wing-body-horizontal families are comprised of a coarse, medium and fine grid; an optional extra-fine grid augments several of the grid families. These mesh sequences are utilized to determine asymptotic grid-convergence characteristics of the solution sets, and to estimate grid-converged absolute drag levels of the wing-body-horizontal configuration using Richardson extrapolation.

Vassberg, John C.; Tinoco, Edward N.; Mani, Mori; Rider, Ben; Zickuhr, Tom; Levy, David W.; Brodersen, Olaf P.; Eisfeld, Bernhard; Crippa, Simone; Wahls, Richard A.; Morrison, Joseph H.; Mavriplis, Dimitri J.; Murayama, Mitcuhiro

2010-01-01

323

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

324

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

325

Models and Phenomenology of Neutrino Masses circa 2010  

NASA Astrophysics Data System (ADS)

We review recent developments in models of neutrino masses and mixing. Emphases are given to models based on finite group family symmetries from which the tri-bimaximal neutrino mixing can arise. In particular, we describe one recent model based on SUSY SU(5) combined with a family symmetry based on the double tetrahedral group, T'. All 22 observable fermion masses and mixing angles and CP violating measures are fitted with only 9 parameters. In this model, a near tri-bimaximal MNS matrix and a realistic CKM matrix are simultaneously generated; the MNS matrix gets slightly modified by virtue of having the Georgi-Jarlskog relations. Due to the presence of complex Clebsch-Gordan coefficients in T', CP violation in this model is entirely geometrical in origin. The prediction of the model for the leptonic Dirac CP phase is 227°, which turns out to be very close to the current best fit value of 220° from SuperK.

Chen, Mu-Chun; Mahanthappa, K. T.

2012-08-01

326

Neutrino-nucleus interactions  

NASA Astrophysics Data System (ADS)

Inclusive electron scattering cross-sections in the quasielastic and resonance regions for few GeV electrons are well represented in terms of scaling functions and scaling variables, the so-called superscaling analysis (SuSA). The concepts of scaling of the first and second kinds and superscaling are discussed, as are several mechanisms which are known to yield scaling violations. Given the high quality of scaling for cross-sections at appropriate kinematics, it is shown how the ideas can be turned around to provide predictions for both charge-changing and neutral current neutrino reactions with nuclei at comparable kinematics.

Donnelly, T. W.

2007-03-01

327

Neutrino and Anti-neutrino Cross Sections at MiniBooNE  

SciTech Connect

The MiniBooNE experiment has reported a number of high statistics neutrino and anti-neutrino cross sections -among which are the charged current quasi-elastic (CCQE) and neutral current elastic (NCE) neutrino scattering on mineral oil (CH{sub 2}). Recently a study of the neutrino contamination of the anti-neutrino beam has concluded and the analysis of the anti-neutrino CCQE and NCE scattering is ongoing.

Dharmapalan, Ranjan [University of Alabama Department of Physics and Astronomy, Tuscaloosa, AL-35487 (United States)

2011-10-06

328

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

329

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

330

Neutrino oscillation based on the mixings with a heavy right-handed neutrino  

NASA Astrophysics Data System (ADS)

We study a consistent explanation for both deficits of solar neutrino and atmospheric neutrino due to the neutrino oscillation induced by the mixing of light neutrinos with a heavy right-handed neutrino. We propose such a phenomenological neutrino mass matrix that realizes this scenario in the simple three generation left- and right- handed neutrino framework. Although this model contains only one nonzero mass eigenvalue ~ 10 eV for these light neutrino states at the first approximation level, it can be expected to explain consistently both deficiencies due to the appropriate higher order corrections. A suitable hot dark matter candidate is naturally included in it as its own feature.

Suematsu, Daijiro

1997-02-01

331

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

332

LSND neutrino oscillation results  

SciTech Connect

The LSND (Liquid Scintillator Neutrino Detector) experiment at Los Alamos has conducted a search for muon antineutrino {r_arrow} electron antineutrino oscillations using muon neutrinos from antimuon decay at rest. The electron antineutrinos are detected via the reaction electron antineutrino + proton {r_arrow} positron + neutron, correlated with the 2.2-MeV gamma from neutron + proton {r_arrow} deuteron + gamma. The use of tight cuts to identify positron events with correlated gamma rays yields 22 events with positron energy between 36 and 60 MeV and only 4.6 {+-} 0.6 background events. The probability that this excess is due entirely to a statistical fluctuation is 4.1 {times} 10{sup -8}. A chi-squared fit to the entire positron sample results in a total excess of 51.8 {sup +18.7}{sub -16.9} {+-} 8.0 events with positron energy between 20 and 60 MeV. If attributed to muon antineutrino {r_arrow} electron antineutrino oscillations, this corresponds to an oscillation probability (averaged over the experimental energy and spatial acceptance) of (0.31 {+-} 0.12 {+-} 0.05){percent}. 10 refs., 7 figs., 1 tab.

Louis, W.C.; LSND Collaboration

1996-10-01

333

Report on solar neutrino experiments  

SciTech Connect

A summary is given of the status of solar neutrino research that includes results of the Brookhaven chlorine detector, a discussion of the development of the gallium, bromine, and lithium radiochemical detectors. The gallium and bromine radiochemical detectors are developed and are capable of giving critical information of interest about neutrino physics and the fusion reactions in the interior of the sun. A plan for building these detectors is outlined and a rough cost estimate is given. A review is given of the plans in the Soviet Union in solar neutrino research.

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

1984-11-15

334

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

335

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

336

Current MINOS neutrino oscillation results  

NASA Astrophysics Data System (ADS)

The MINOS experiment is now making precise measurements of the ?? disappearance oscillations seen in atmospheric neutrinos, tests possible disappearance to sterile ? by measuring the neutral current flux, and has extended our reach towards the so far unseen ?13 by looking for ?e appearance in the ?? beam. It does so by using the intense, well-understood NuMI neutrino beam created at Fermilab and observing it 735km away at the Soudan Mine in Northeast Minnesota. High-statistics studies of the neutrino interactions themselves and the cosmic rays seen by the MINOS detectors have also been made. Results from MINOS' first three years of operations will be presented.

Habig, Alec; Minos Collaboration

2010-01-01

337

Study of Salt Neutrino Detector  

NASA Astrophysics Data System (ADS)

Rock salt is studied as a radio wave transmission medium in an ultra high energy (UHE) cosmic neutrino detector. The radio wave would be generated by Askar'yan effect (coherent Chrenkov radiation from negative excess charges in the electromagnetic shower) in the UHE neutrino interaction in the rock salt. We collected the samples of the rock salts from various rock salt mines in order to investigate whether they have a possibility as a Salt Neutrino Detector (SND) sites or not. As a tentative result, the absorption length of the rock salt samples was measured to be between 40 m and400 m at 1 GHz. .

Chiba, Masami; Kamijo, Toshio; Kawaki, Miho; Husain, Athar; Inuzuka, Masahide; Ikeda, Maho; Yasuda, Osamu

2001-07-01

338

THE DOMINANCE OF NEUTRINO-DRIVEN CONVECTION IN CORE-COLLAPSE SUPERNOVAE  

SciTech Connect

Multi-dimensional instabilities have become an important ingredient in core-collapse supernova (CCSN) theory. Therefore, it is necessary to understand the driving mechanism of the dominant instability. We compare our parameterized three-dimensional CCSN simulations with other buoyancy-driven simulations and propose scaling relations for neutrino-driven convection. Through these comparisons, we infer that buoyancy-driven convection dominates post-shock turbulence in our simulations. In support of this inference, we present four major results. First, the convective fluxes and kinetic energies in the neutrino-heated region are consistent with expectations of buoyancy-driven convection. Second, the convective flux is positive where buoyancy actively drives convection, and the radial and tangential components of the kinetic energy are in rough equipartition (i.e., K{sub r} {approx} K{sub {theta}} + K{sub {phi}}). Both results are natural consequences of buoyancy-driven convection, and are commonly observed in simulations of convection. Third, buoyant driving is balanced by turbulent dissipation. Fourth, the convective luminosity and turbulent dissipation scale with the driving neutrino power. In all, these four results suggest that in neutrino-driven explosions, the multi-dimensional motions are consistent with neutrino-driven convection.

Murphy, Jeremiah W.; Dolence, Joshua C.; Burrows, Adam, E-mail: jmurphy@astro.princeton.edu, E-mail: jdolence@astro.princeton.edu, E-mail: burrows@astro.princeton.edu [Princeton University, Princeton, NJ (United States)

2013-07-01

339

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

340

An Analysis of Recent Solar Neutrino Data  

NASA Astrophysics Data System (ADS)

Recent solar neutrino data from the Sudbury Neutrino Observatory (SNO) and from the Borexino experiment reach relatively low neutrino energies of several MeV. At these energies, the matter-enhanced neutrino oscillations via the so-called Mikheev-Smirnov-Wolfenstein (MSW) resonance manifest. Neutrinos originating near the center of the sun will feel this resonance as they propagate at these energies, modifying their oscillation away from the standard MSW effect. We examine these solar data in the context of effects that could be larger at the resonance than elsewhere in the solar neutrino spectrum. We explore the potential for the electron neutrino survival probability measured by these experiments to reveal those effects. We look for evidence of nonzero values for the neutrino mixing angle ?13, for evidence of sterile neutrinos and for interactions beyond the Standard Model of particle physics among these data

Malkus, Annelise

341

The many aspects of neutrino physics  

SciTech Connect

In mid-November, over seventy physicists gathered at Fermilab for an informal workshop on the Many Aspects of Neutrino Physics, which dovetailed with and also helped lay the groundwork for the succeeding more narrowly focused conference on Long Baseline Neutrino Oscillations. The workshop indeed covered many of the interrelated aspects of neutrino physics: 17 keV neutrinos (experiments, theoretical models, and astrophysical constraints), neutrino properties (double beta decay experiments, neutrino magnetic moments), neutrinos from/as weakly interacting massive particles (WIMPs) in cosmology and astrophysics, atmospheric neutrinos, and solar neutrinos. In the following, I provide a brief and thoroughly biased account of only some of the many interesting developments discussed at the workshop.

Frieman, J.A.

1992-01-01

342

Electron Neutrino Appearance in the MINOS Experiment  

SciTech Connect

MINOS is a long-baseline neutrino oscillation experiment tasked to make a precision measurement of the neutrino mixing parameters associated with the atmospheric neutrino mass splitting. Using a high powered neutrino beam from the Main Injector (NuMI) facility at Fermilab, it compares the neutrino energy spectrum for neutrino interactions observed in two large detectors located at Fermilab and in the Soudan mine in northern Minnesota at a distance of 735 km. We have recently presented muon-neutrino disappearance results after two years of data taking. Beyond those results there is the possibility that for a mixing angle related to electron-neutrino appearance in the vicinity of the current experimental limit, MINOS could make an initial measurement of this parameter. We present a method for particle identification of electron neutrinos and show several techniques being used to study the background contributions for this analysis in the non-oscillated data at the Near Detector.

Sanchez, Mayly C. [Department of Physics, Harvard University, Cambridge, MA 02138 (United States)

2008-02-21

343

Electron Neutrino Appearance in the MINOS Experiment  

NASA Astrophysics Data System (ADS)

MINOS is a long-baseline neutrino oscillation experiment tasked to make a precision measurement of the neutrino mixing parameters associated with the atmospheric neutrino mass splitting. Using a high powered neutrino beam from the Main Injector (NuMI) facility at Fermilab, it compares the neutrino energy spectrum for neutrino interactions observed in two large detectors located at Fermilab and in the Soudan mine in northern Minnesota at a distance of 735 km. We have recently presented muon-neutrino disappearance results after two years of data taking. Beyond those results there is the possibility that for a mixing angle related to electron-neutrino appearance in the vicinity of the current experimental limit, MINOS could make an initial measurement of this parameter. We present a method for particle identification of electron neutrinos and show several techniques being used to study the background contributions for this analysis in the non-oscillated data at the Near Detector.

Sanchez, Mayly C.

2008-02-01

344

Documentation of the fourth order band model  

NASA Technical Reports Server (NTRS)

A general circulation model is presented which uses quadratically conservative, fourth order horizontal space differences on an unstaggered grid and second order vertical space differences with a forward-backward or a smooth leap frog time scheme to solve the primitive equations of motion. The dynamic equations for motion, finite difference equations, a discussion of the structure and flow chart of the program code, a program listing, and three relevent papers are given.

Kalnay-Rivas, E.; Hoitsma, D.

1979-01-01

345

Fourth NASA Langley Formal Methods Workshop  

NASA Technical Reports Server (NTRS)

This publication consists of papers presented at NASA Langley Research Center's fourth workshop on the application of formal methods to the design and verification of life-critical systems. Topic considered include: Proving properties of accident; modeling and validating SAFER in VDM-SL; requirement analysis of real-time control systems using PVS; a tabular language for system design; automated deductive verification of parallel systems. Also included is a fundamental hardware design in PVS.

Holloway, C. Michael (Compiler); Hayhurst, Kelly J. (Compiler)

1997-01-01

346

Fourth-generation quarks and leptons  

Microsoft Academic Search

We study the production, decay, and detection of fourth-generation quarks and leptons at present and future hadron colliders. We use a plausible extension of the quark-mixing systematics of three generations. We consider a range of heavy-quark masses that include overlapping generations and superheavy quarks that decay to the W boson. One particularly intriguing possibility is a new charge -13 quark

V. Barger; H. Baer; K. Hagiwara; R. J. N. Phillips

1984-01-01

347

Recognition and Management of Pesticide Poisonings. Fourth Edition.  

National Technical Information Service (NTIS)

The fourth edition of Recognition and Management of Pesticide Poisonings is an update and expansion of the 1982 third edition. The purpose of the fourth edition is to provide health professionals with recently available information on the health hazards o...

D. P. Morgan

1989-01-01

348

22. THIRD FLOOR, 202 EAST FOURTH STREET LOOKING SOUTHEAST, PARTITION ...  

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

22. THIRD FLOOR, 202 EAST FOURTH STREET LOOKING SOUTHEAST, PARTITION SCAR MARKED BY CONTRASTING WALLPAPER TREATMENTS - Phillips-Thompson Building, 200-206 East Fourth Street, Wilmington, New Castle County, DE

349

7 CFR 51.2296 - Three-fourths half kernel.  

Code of Federal Regulations, 2010 CFR

...PRODUCTS 1,2 (INSPECTION, CERTIFICATION, AND STANDARDS) United States Standards for Shelled English Walnuts (Juglans Regia) Definitions § 51.2296 Three-fourths half kernel. Three-fourths half kernel means a portion of...

2009-01-01

350

Neutrino Experiments at the SNS  

SciTech Connect

This talk describes planned neutrino physics experiments at the Spallation Neutron Source in Oak Ridge, Tennessee, with a focus on the proposed CLEAR (Coherent Low Energy Nuclear(A) Recoils) experiment.

Scholberg, Kate [Duke University Physics Department, Durham, NC, 27708 (United States)

2009-12-17

351

The Diffuse Supernova Neutrino Background  

NASA Astrophysics Data System (ADS)

The diffuse supernova neutrino background (DSNB) is the weak glow of megaelectronvolt neutrinos and antineutrinos from distant core-collapse supernovae. The DSNB has not been detected yet, but the Super-Kamiokande (SK) 2003 upper limit on the [Formula: see text] flux is close to predictions, now quite precise, that are based on astrophysical data. If SK is modified with dissolved gadolinium to reduce detector backgrounds and increase the energy range for analysis, then it should detect the DSNB at a rate of a few events per year, providing a new probe of supernova neutrino emission and the cosmic core-collapse rate. If the DSNB is not detected, then new physics will be required. Neutrino astronomy, although uniquely powerful, has proven extremely difficult—only the Sun and the nearby Supernova 1987A have been detected to date—so the promise of detecting new sources soon is exciting indeed.

Beacom, John F.

2010-11-01

352

LENA: Low Energy Neutrino Astronomy  

NASA Astrophysics Data System (ADS)

We focus on the physics potential of a large liquid scintillation detector in the field of low energy neutrino astrophysics. Proton decay search and long baseline oscillations will be discussed briefly at the end.

Oberauer, L.; Hellgartner, D.; Lewke, T.; Marrodán Undagoitia, T.; Meindl, Q.; Möllenstedt, R.; Potzel, W.; Tippmann, M.; von Feilitzsch, F.; Winter, J.; Wurm, M.

2011-08-01

353

AMANDA and ICECUBE Neutrino Telescopes  

Microsoft Academic Search

However, also particle physics proper may profit, e.g. in the area of neutrino properties and ultra-high energy cross section, in the search for supersymmetric particles that may constitute part of the \\

J. Ahrens; T. Becka; T. Feser; O. Franzen; R. Gozzini; M. Hellwig; L. Kopke; T. Kowarik; T. Neunhoffer; A. Piegsa; H. G. Sander; U. Schafer; N. Sidro; J. Stegmeier

354

The effective neutrino charge radius  

NASA Astrophysics Data System (ADS)

It is shown that at one-loop order a neutrino charge radius (NCR) may be defined, which is ultraviolet finite, does not depend on the gauge-fixing parameter, nor on properties of the target other than its electric charge. This is accomplished through the systematic decomposition of physical amplitudes into effective self-energies, vertices, and boxes, which separately respect electroweak gauge invariance. In this way the NCR stems solely from an effective proper photon-neutrino one-loop vertex, which satisfies a naive, QED-like Ward identity. The NCR so defined may be extracted from experiment, at least in principle, by expressing a set of experimental electron-neutrino cross-sections in terms of the finite NCR and two additional gauge- and renormalization-group-invariant quantities, corresponding to the electroweak effective charge and mixing angle. PACS: 13.15.+g Neutrino interactions - 13.40.Gp Electromagnetic form factors

Papavassiliou, J.; Bernabéu, J.; Binosi, D.; Vidal, J.

355

Unparticle effects in neutrino telescopes  

SciTech Connect

Recently H. Georgi has introduced the concept of unparticles in order to describe the low energy physics of a nontrivial scale invariant sector of an effective theory. We investigate its physical effects on the neutrino flux to be detected in a kilometer cubic neutrino telescope such as IceCube. We study the effects, on different observables, of the survival neutrino flux after through the Earth, and the regeneration originated in the neutral currents. We calculate the contribution of unparticle physics to the neutrino-nucleon interaction and, then, to the observables in order to evaluate detectable effects in IceCUbe. Our results are compared with the bounds obtained by other nonunderground experiments. Finally, the results are presented as an exclusion plot in the relevant parameters of the new physics stuff.

Gonzalez-Sprinberg, G.; Martinez, R.; Sampayo, Oscar A. [Instituto de Fisica, Facultad de Ciencias, Universidad de la Republica, Igua 4225, 11400 Montevideo (Uruguay); Departamento de Fisica, Universidad Nacional, Bogota (Colombia); Departamento de Fisica, Universidad Nacional de Mar del Plata, Funes 3350, (7600) Mar del Plata (Argentina)

2009-03-01

356

Neutrino mass and mixing, and non-accelerator experiments  

SciTech Connect

We review the current status of experimental knowledge about neutrinos derived from kinematic mass measurements, neutrino oscillation searches at reactors and accelerators, solar neutrinos, atmospheric neutrinos, and single and double beta decay. The solar neutrino results yield fairly strong and consistent indication that neutrino oscillations are occurring. Other evidence for new physics is less consistent and convincing.

Robertson, R.G.H.

1992-10-01

357

Neutrino mass and mixing, and non-accelerator experiments  

SciTech Connect

We review the current status of experimental knowledge about neutrinos derived from kinematic mass measurements, neutrino oscillation searches at reactors and accelerators, solar neutrinos, atmospheric neutrinos, and single and double beta decay. The solar neutrino results yield fairly strong and consistent indication that neutrino oscillations are occurring. Other evidence for new physics is less consistent and convincing.

Robertson, R.G.H.

1992-01-01

358

Family Arguments  

MedlinePLUS

... Healthy Children > Family Life > Family Dynamics > Family Arguments Family Life Listen Family Arguments Article Body We seem to have a lot of arguments in our family. Is this normal? Disputes between you and your ...

359

N Resonances in Neutrino Interactions  

NASA Astrophysics Data System (ADS)

The role of N* resonances in neutrino interactions with nucleons is discussed, stressing the relevance for neutrino cross-section and oscillation experiments. The cross section for single N* weak excitation is expressed in terms of vector and axial transition form factors, which can be partially constrained using the available experimental information from photon, electron and pion reactions on the nucleon. New measurements on hydrogen and deuterium are necessary to reduce further the uncertainties.

Alvarez-Ruso, L.

2014-01-01

360

The Antares Undersea Neutrino Telescope  

NASA Astrophysics Data System (ADS)

Neutrino astronomy is a very promising field of investigation representing a complementary source of information with respect to photon-astronomy. ANTARES, operating off the French Mediterranean coast, is the worlds largest operational underwater neutrino telescope. In these proceedings, in addition to a short detector description, the results of recent analysis will be discussed. The ANTARES project is an important physics experiment but also represents a bench mark for a future large detector of the km3 scale.

Anghinolfi, Marco

2013-11-01

361

Daya Bay Reactor Neutrino Experiment  

Microsoft Academic Search

The Daya Bay reactor neutrino experiment, currently under construction in China, will be the most sensitive experiments in the world searching for the yet unknown neutrino mixing parameters, theta-13(theta13). With a thermal power of 17.4GW by 2011, the Daya Bay site provides an intense electron antineutrino flux, which together with 3 years of data taking from 4 pairs of identical

Yuenkeung Hor

2009-01-01

362

Detection of massive supernova neutrinos  

Microsoft Academic Search

Neutrinos and antineutrinos of all three flavours are emitted during the post bounce phase of a core collapse supernova with numu\\/nutau(nu¯mu\\/nu¯tau) having average energies more than that of nue(nu¯e). The author presents the effect of flavour oscillations on the neutrino flux and their expected number of events at the detector. The author performs a three-generation analysis and for the mass

S. Choubey

1999-01-01

363

Solar Neutrinos: Status and Prospects  

NASA Astrophysics Data System (ADS)

We describe the current status of solar neutrino measurements and of the theory—both neutrino physics and solar astrophysics—employed in interpreting measurements. Important recent developments include Super-Kamiokande's determination of the ?-e elastic scattering rate for 8B neutrinos to 3%; the latest Sudbury Neutrino Observatory (SNO) global analysis in which the inclusion of low-energy data from SNO I and II significantly narrowed the range of allowed values for the neutrino mixing angle ?12; Borexino results for both the 7Be and proton-electron-proton (pep) neutrino fluxes, the first direct measurements constraining the rate of proton-proton (pp) I and pp II burning in the Sun; global reanalyses of solar neutrino data that take into account new reactor results on ?13; a new decadal evaluation of the nuclear physics of the pp chain and CNO cycle defining best values and uncertainties in the nuclear microphysics input to solar models; recognition of an emerging discrepancy between two tests of solar metallicity, helioseismological mappings of the sound speed in the solar interior, and analyses of the metal photoabsorption lines based on our best current description of the Sun's photosphere; a new round of standard solar model calculations optimized to agree either with helioseismology or with the new photospheric analysis; and, motivated by the solar abundance problem, the development of nonstandard, accreting solar models, in order to investigate possible consequences of the metal segregation that occurred in the proto-solar disk. We review this progress and describe how new experiments such as SNO+ could help us further exploit neutrinos as a unique probe of stellar interiors.

Haxton, W. C.; Hamish Robertson, R. G.; Serenelli, Aldo M.

2013-08-01

364

Lepton asymmetries from neutrino oscillations  

NASA Astrophysics Data System (ADS)

Reasonably large relic neutrino asymmetries can be generated by active-sterile neutrino oscillations. After briefly discussing possible applications, I describe the Quantum Kinetic Equation formalism used to compute the asymmetry growth curves. I then show how the basic features of these curves can be understood on the basis of the adiabatic limit approximation in the collision dominated epoch, and the pure MSW effect at lower temperatures.

Volkas, R. R.

365

New ideas in neutrino detection  

Microsoft Academic Search

What is new in the field of neutrino detection? In addition to new projects probing both the low and high ends of the neutrino\\u000a energy scale, an inexpensive, effective technique is being developed to allow tagging of antineutrinos in water Cherenkov\\u000a (WC) detectors via the addition to water of a solute with a large neutron cross-section and energetic ? daughters.

M. R. Vagins

2006-01-01

366

Invariants of collective neutrino oscillations  

NASA Astrophysics Data System (ADS)

We consider the flavor evolution of a dense neutrino gas by taking into account both vacuum oscillations and self-interactions of neutrinos. We examine the system from a many-body perspective as well as from the point of view of an effective one-body description formulated in terms of the neutrino polarization vectors. We show that, in the single angle approximation, both the many-body picture and the effective one-particle picture possess several constants of motion. We write down these constants of motion explicitly in terms of the neutrino isospin operators for the many-body case and in terms of the polarization vectors for the effective one-body case. The existence of these constants of motion is a direct consequence of the fact that the collective neutrino oscillation Hamiltonian belongs to the class of Gaudin Hamiltonians. This class of Hamiltonians also includes the (reduced) BCS pairing Hamiltonian describing superconductivity. We point out the similarity between the collective neutrino oscillation Hamiltonian and the BCS pairing Hamiltonian. The constants of motion manifest the exact solvability of the system. Borrowing the well established techniques of calculating the exact BCS spectrum, we present exact eigenstates and eigenvalues of both the many-body and the effective one-particle Hamiltonians describing the collective neutrino oscillations. For the effective one-body case, we show that spectral splits of neutrinos can be understood in terms of the adiabatic evolution of some quasiparticle degrees of freedom from a high-density region where they coincide with flavor eigenstates to the vacuum where they coincide with mass eigenstates. We write down the most general consistency equations which should be satisfied by the effective one-body eigenstates and show that they reduce to the spectral split consistency equations for the appropriate initial conditions.

Pehlivan, Y.; Balantekin, A. B.; Kajino, Toshitaka; Yoshida, Takashi

2011-09-01

367

Neutrinos from hell. [Detected from supernova  

SciTech Connect

The detection of neutrinos is studied. The use of the Kamiokande II detector, which is a cylindrical tank holding about 3000 tons of highly purified water, for neutrino detection is examined. The operation and capabilities of the Kamiokande II detector are described. The Kamiokande II and Irvine-Michigan-Brookhaven detector observed the neutrinos from SN 1987A. The relation between the supernova and the neutrinos is analyzed. Particular consideration is given to the shock wave and the energies of the neutrinos. Additional data provided by the neutrino observations are discussed.

Schorn, R.A.

1987-05-01

368

Supernova neutrino observations: What can we learn?  

NASA Astrophysics Data System (ADS)

Twenty years after SN 1987A, the vast international programme of experimental neutrino physics and neutrino astronomy suggests that large detectors will operate for a long time. It is realistic that a high-statistics neutrino signal from a galactic SN will be observed. I review some of the generic lessons from such an observation where neutrinos largely play the role of astrophysical messengers. In principle, the signal also holds valuable information about neutrino mixing parameters. I explain some recent developments about the crucial importance of collective neutrino oscillations in the SN environment.

Raffelt, Georg G.

2011-12-01

369

Quantum Gravity Effect on Neutrino Oscillation  

NASA Astrophysics Data System (ADS)

The quantum gravity may have strong consequence for neutrino oscillation phenemomenon over a large distance.We found a significant modification of neutrino oscillation due to quantum gravity effects. Quantum gravity (Planck scale effects) leads to an effective S U(2) L ×U(1) invariant dimension-5 Lagrangian involving, neutrino and Higgs fields. On symmetry breaking, this operator gives rise to correction to the neutrino masses and mixing. The gravitational interaction (M X =M p l ) demands that the element of this perturbation matrix should be independent of flavor indices. In this paper, we study the quantum gravity effects on neutrino oscillation, namely modified dispersion relation for neutrino oscillations parameter.

Koranga, Bipin Singh; Narayan, Mohan

2014-05-01

370

Solar mass-varying neutrino oscillations.  

PubMed

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 and with reactor antineutrino data at short and long baselines (from CHOOZ and KamLAND). We find that the survival probability of solar MaVaNs is independent of how the suppression of neutrino mass caused by the acceleron-matter couplings varies with density. Measurements of MeV and lower energy solar neutrinos will provide a rigorous test of the idea. PMID:16384133

Barger, V; Huber, Patrick; Marfatia, Danny

2005-11-18

371

High-energy neutrino astronomy  

NASA Astrophysics Data System (ADS)

Neutrino astronomy, conceptually conceived four decades ago, has entered an exciting phase for providing results on the quest for the sources of the observed highest energy particles. IceCube and ANTARES are now completed and are scanning in space and time possible signals of high energy neutrinos indicating the existence of such sources. DeepCore, inside IceCube, is a playground for vetoed neutrino measurement with better potential below 1 TeV. A larger and denser detector is now being discussed. ARA, now in test phase, will be composed by radio stations that could cover up to ~ 100 km2 and aims at the highest energy region of cosmogenic neutrinos. The non observation of cosmic events is on one side a source of disappointment, on the other it represents by itself an important result. If seen in the context of a multi-messenger science, the combination of photon and cosmic ray experiment results brings invaluable information. The experimental upper bounds of the cubic-kilometer telescope IceCube are now below the theoretical upper bounds for extragalactic fluxes of neutrinos from optically thin sources. These are responsible for accelerating the extragalactic cosmic rays. Such limits constrain the role of gamma-ray bursts, described by the fireball picture, as sources of ultra-high energy cosmic rays. Neutrino telescopes are exciting running multi-task experiments that produce astrophysics and particle physics results some of which have been illustrated at this conference and are summarized in this report.

Montaruli, Teresa

2012-07-01

372

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

373

Beta Beams for Neutrino Production  

NASA Astrophysics Data System (ADS)

To use accelerated beta active radioactive ions to produce collimated high energy neutrino beams was proposed by P. Zuchelli in 2002. Since then, several ideas related to how to design Beta Beam facilities have been studied. Design studies of an accelerator complex, based on CERN accelerators, have been supported by research programs within the European Commisison FP6 and FP7 frameworks (EURISOL Design Study and EUROnu). In these studies 6He and 18Ne are used as beta emitters to produce antineutrinos and neutrinos respectively. Alternative isotopes for neutrino beam production, 8Li and 8B, are investigated in the now ongoing study, EUROnu. Due to the higher reaction Q-value of these ions, the resulting neutrino energies are higher. The isotopes we need for neutrino beams have to be produced in large quantities using non conventional methods. Latest research on production of isotopes that are presently considered for Beta Beams will be discussed. The work achieved gives a good ground to propose the Beta Beam, which is based on known technology, for neutrino production. In this status review we concentrate on technical issues related to a possible Beta Beam facility using the CERN infrastructure.

Wildner, E.

2012-08-01

374

Dark energy from mass varying neutrinos  

NASA Astrophysics Data System (ADS)

We show that mass varying neutrinos (MaVaNs) can behave as a negative pressure fluid which could be the origin of the cosmic acceleration. We derive a model independent relation between the neutrino mass and the equation of state parameter of the neutrino dark energy, which is applicable for general theories of mass varying particles. The neutrino mass depends on the local neutrino density and the observed neutrino mass can exceed the cosmological bound on a constant neutrino mass. We discuss microscopic realizations of the MaVaN acceleration scenario, which involve a sterile neutrino. We consider naturalness constraints for mass varying particles, and find that both eV cut-offs and eV mass particles are needed to avoid fine-tuning. In microscopic realizations of this scenario with a sterile neutrino, these considerations give the sterile neutrino a maximum mass today of order an eV, which could be detectable at MiniBooNE. Because the sterile neutrino was much heavier at earlier times, constraints from big bang nucleosynthesis on additional states are not problematic. We consider regions of high neutrino density and find that the most likely place today to find neutrino masses which are significantly different from the neutrino masses in our solar system is in a supernova. The possibility of different neutrino mass in different regions of the galaxy and the local group could be significant for Z-burst models of ultra-high energy cosmic rays. We also consider the cosmology of and the constraints on the 'acceleron', the scalar field which is responsible for the varying neutrino mass, and briefly discuss neutrino density dependent variations in other constants, such as the fine structure constant.

Fardon, Rob; Nelson, Ann E.; Weiner, Neal

2004-10-01

375

Neutrino factories: Realization and physics potential  

NASA Astrophysics Data System (ADS)

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 (i) an overview is given of the technical ingredients needed for a Neutrino Factory, (ii) beam properties are described, (iii) the resulting neutrino oscillation physics potential is summarized, (iv) a more detailed description is given for one representative Neutrino Factory design, and (v) the ongoing R&D program is summarized, and future plans briefly described.

Geer, S.; Zisman, M. S.

2007-10-01

376

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

377

Supernova neutrinos: Earth matter effects and neutrino mass spectrum  

NASA Astrophysics Data System (ADS)

We perform a detailed study of the Earth matter effects on supernova neutrinos. The dependences of these effects on the properties of the original neutrino fluxes, on the trajectory of the neutrinos inside the Earth and on the oscillation parameters are described. We show that, for a large fraction (/~60%) of the possible arrival times of the signal, the neutrino flux crosses a substantial amount of the matter of the Earth at least for one of the existing detectors. For oscillation parameters from the LMA solution of the solar neutrino problem the Earth matter effect consists in an oscillatory modulation of the ?¯e and/or ?e energy spectra. The relative deviation with respect to the undistorted spectra can be as large as 20-30% for /E>~20 MeV and 70-100% for /E>~40 MeV. For parameters from the SMA and LOW solutions the effect is localized at low energies (/E<~10 MeV) and is not larger than /~10%. The Earth matter effects can be revealed (i) by the observation of oscillatory distortions of the energy spectra in a single experiment and (ii) by the comparison between the spectra at different detectors. For a supernova at distance /D=10 Kpc, comparing the results of SuperKamiokande (SK), SNO and LVD experiments one can establish the effect at (2-3)/? level, whereas larger statistical significance ((4-5)/?) is obtained if two experiments of SK-size or larger are available. Studies of the Earth matter effect will select or confirm the solution of the solar neutrino problem, probe the mixing Ue3 and identify the hierarchy of the neutrino mass spectrum.

Lunardini, C.; Smirnov, A. Yu.

2001-11-01

378

nu-K0 Analogy, Dirac-Majorana Neutrino Duality and the Neutrino Oscillations  

Microsoft Academic Search

The intent of this paper is to convey a new primary physical idea of a Dirac-Majorana neutrino duality in relation to the topical problem of neutrino oscillations. In view of the new atmospheric, solar and the LSND neutrino oscillation data, the Pontecorvo nu - K0 oscillation analogy is generalized to the notion of neutrino duality with substantially different physical meaning

E. M. Lipmanov

2001-01-01

379

Los Alamos Science, Number 25 -- 1997: Celebrating the neutrino  

SciTech Connect

This issue is devoted to the neutrino and its remaining mysteries. It is divided into the following areas: (1) The Reines-Cowan experiment -- detecting the poltergeist; (2) The oscillating neutrino -- an introduction to neutrino masses and mixing; (3) A brief history of neutrino experiments at LAMPF; (4) A thousand eyes -- the story of LSND (Los Alamos neutrino oscillation experiment); (5) The evidence for oscillations; (6) The nature of neutrinos in muon decay and physics beyond the Standard Model; (7) Exorcising ghosts -- in pursuit of the missing solar neutrinos; (8) MSW -- a possible solution to the solar neutrino problem; (8) Neutrinos and supernovae; and (9) Dark matter and massive neutrinos.

Cooper, N.G. [ed.] [ed.

1997-12-31

380

Detecting thermal neutrinos from supernovae with DUMAND  

SciTech Connect

The Deep Underwater Muon and Neutrino Detector (DUMAND) could be made sensitive to the thermal (about 10-MeV) neutrinos from a supernova, as well as the TeV neutrinos for which it was originally designed, by clustering the photomultiplier tubes used to detect the Cerenkov light produced by neutrino interactions into nodes of four tubes. Requiring coincident counts from three or four of the tubes at a node would reduce the background from bioluminescence enough to allow the detection of the neutrinos from a supernova. A modified DUMAND using quadruple coincidence would have detected roughly eight neutrinos from SN 1987A and would detect about 280 neutrinos from a Galactic supernova at a distance of 9 kpc. Triple coincidence could be used with a Galactic supernova and would detect about 1500 neutrinos. 26 references.

Pryor, C.; Roos, C.E.; Webster, M.S.

1988-06-01

381

The neutrino sky at very high energies  

NASA Astrophysics Data System (ADS)

Neutrino astronomy opens a new window for the observation and study of high-energy phenomena in our Universe. The emission of high-energy neutrinos in extragalactic sources or the cosmic environment is intimately related to that of ?-rays and cosmic rays. We will review the various indirect neutrino limits that arise from this cosmic connection and compare this to the present direct limits of neutrino observatories. Specific models of extragalactic TeV to PeV neutrino sources are already testable by large volume neutrino observatories like IceCube. At the EeV energy scale the flux of cosmogenic neutrinos associated with the propagation of ultra-high energy cosmic rays in the cosmic radiation background seems to be the most promising contribution to the diffuse neutrino background. We will discuss its model dependence w.r.t. chemical composition and evolution of the sources and provide simple bolometric scaling relations.

Ahlers, Markus

2013-10-01

382

Reactor neutrino experiments: ?13 and beyond  

NASA Astrophysics Data System (ADS)

We review the current-generation short-baseline reactor neutrino experiments that have firmly established the third neutrino mixing angle ?13 to be nonzero. The relative large value of ?13 (around 9°) has opened many new and exciting opportunities for future neutrino experiments. Daya Bay experiment with the first measurement of ? m2ee is aiming for a precision measurement of this atmospheric mass-squared splitting with a comparable precision as ? m2? ? from accelerator muon neutrino experiments. JUNO, a next-generation reactor neutrino experiment, is targeting to determine the neutrino mass hierarchy (MH) with medium baselines ( 50 km). Beside these opportunities enabled by the large ?13, the current-generation (Daya Bay, Double Chooz, and RENO) and the next-generation (JUNO, RENO-50, and PROSPECT) reactor experiments, with their unprecedented statistics, are also leading the precision era of the three-flavor neutrino oscillation physics as well as constraining new physics beyond the neutrino Standard Model.

Qian, Xin; Wang, Wei

2014-05-01

383

Observation of Electron Neutrino Appearance in a Muon Neutrino Beam  

NASA Astrophysics Data System (ADS)

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 ?m322 and a CP violating phase ?CP. In this neutrino oscillation scenario, assuming |?m322|=2.4×10-3 eV2, sin2?23=0.5, and ?m322>0 (?m322<0), a best-fit value of sin22?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.

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.; ?muda, J.; T2K Collaboration

2014-02-01

384

Evidence of electron neutrino appearance in a muon neutrino beam  

NASA Astrophysics Data System (ADS)

The T2K Collaboration reports evidence for electron neutrino appearance at the atmospheric mass splitting, |?m322|?2.4×10-3eV2. 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±0.4(syst) events is expected. The background-only hypothesis is rejected with a p value of 0.0009 (3.1?), and a fit assuming ????e oscillations with sin?22?23=1, ?CP=0 and |?m322|=2.4×10-3eV2 yields sin?22?13=0.088-0.039+0.049(stat+syst).

Abe, K.; Abgrall, N.; Aihara, H.; 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.; Caravaca Rodríguez, J.; Cartwright, S. L.; Castillo, R.; Catanesi, M. G.; Cervera, A.; Cherdack, D.; Christodoulou, G.; Clifton, A.; Coleman, J.; Coleman, S. J.; Collazuol, G.; Connolly, K.; Cremonesi, L.; Curioni, A.; Dabrowska, A.; Danko, I.; Das, R.; Davis, S.; Day, M.; de André, 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.; Pinzon Guerra, E. S.; 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.; Sánchez, 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.

2013-08-01

385

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

386

Ecological, Psychological, and Cognitive Components of Reading Difficulties: Testing the Component Model of Reading in Fourth Graders across 38 Countries  

ERIC Educational Resources Information Center

The authors tested the component model of reading (CMR) among 186,725 fourth grade students from 38 countries (45 regions) on five continents by analyzing the 2006 Progress in International Reading Literacy Study data using measures of ecological (country, family, school, teacher), psychological, and cognitive components. More than 91% of the…

Chiu, Ming Ming; McBride-Chang, Catherine; Lin, Dan

2012-01-01

387

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

388

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

389

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

390

Neutrino oscillations under gravity: mass independent oscillation  

Microsoft Academic Search

I discuss the possibility of neutrino oscillation in presence of gravity. In this respect I consider the propagation of neutrinos in the early phase of universe and around black holes. It is seen that whether the rest masses of a neutrino and corresponding anti-neutrino are considered to be same or not due to space-time curvature effect non-zero oscillation probability between

Banibrata Mukhopadhyay

2003-01-01

391

Atmospheric neutrino flux at INO site  

SciTech Connect

To illustrate the calculation of the atmospheric neutrino flux, we briefly explain our calculation scheme and important components, such as primary cosmic ray spectra, interaction model, and geomagnetic model. Then, we calculate the atmospheric neutrino flux at INO site in our calculation scheme. We compare the calculated atmospheric neutrino fluxes predicted at INO with those at other major neutrino detector sites, especially that at SK site.

Honda, Morihiro [Institute for Cosmic Ray Research, University of Tokyo, 5-1-5 Kashiwa-no-ha, Kashiwa, Chiba 277-8582 (Japan)

2011-11-23

392

Atmospheric neutrino flux at INO site  

NASA Astrophysics Data System (ADS)

To illustrate the calculation of the atmospheric neutrino flux, we briefly explain our calculation scheme and important components, such as primary cosmic ray spectra, interaction model, and geomagnetic model. Then, we calculate the atmospheric neutrino flux at INO site in our calculation scheme. We compare the calculated atmospheric neutrino fluxes predicted at INO with those at other major neutrino detector sites, especially that at SK site.

Honda, Morihiro

2011-11-01

393

Tribimaximal mixing, discrete family symmetries, and a conjecture connecting the quark and lepton mixing matrices  

Microsoft Academic Search

Neutrino oscillation experiments (excluding the Liquid Scintillator Neutrino Detector experiment) suggest a tribimaximal form for the lepton mixing matrix. This form indicates that the mixing matrix is probably independent of the lepton masses, and suggests the action of an underlying discrete family symmetry. Using these hints, we conjecture that the contrasting forms of the quark and lepton mixing matrices may

Catherine I Lowand; Raymond R. Volkas

2003-01-01

394

Fourth Meeting on CPT and Lorentz Symmetry  

NASA Astrophysics Data System (ADS)

Improved tests of Lorentz and CPT symmetry using noble-gas masers / A. Glenday, D. F. Phillips, and R. L. Walsworth -- A modern Michelson-Morley experiment using actively rotated optical resonators / S. Herrmann et al. -- Rotating experiments to test Lorentz invariance in the photon sector / M. E. Tobar et al. -- Lorentz violation, electrodynamics, and the cosmic microwave background / M. Mewes -- High energy astrophysical tests of Lorentz invariance / B. Altschul -- Fundamental physics experiments in space (within ESA) / T. J. Sumner -- The experimental foundations of the Dirac equation / C. Lämmerzahl -- Perspectives on Lorentz and CPT violation / V. A. Kostelecký -- Search for Lorentz and CPT violation effects in muon spin precession / B. L. Roberts -- Lorentz violation in a diffeomorphism-invariant theory / R. Jackiw -- Studies of CPT symmetry with ASACUSA / R. S. Hayano -- Neutrino oscillations and Lorentz violation with MiniBooNE / R. Tayloe and T. Katori -- Testing Lorentz and CPT invariance with MINOS near detector neutrinos / B. J. Rebel and S. L. Mufson -- Einstein-?ther gravity: theory and observational constraints / T. Jacobson -- Tests of Lorentz-invariance violation in neutrino oscillations / K. Whisnant -- Search for CPT violation in neutral kaons at KLOE: status and perspectives / A. Di Domenico et al. -- Search for CPT violation in B[symbol]-B¯[symbol] oscillations with BABAR / D. P. Stoker -- Theoretical topics in spacetime-symmetry violations / R. Lehnert -- A second-generation co-magnetometer for testing fundamental symmetries / S. J. Smullin et al. -- Nambu-Goldstone and massive modes in gravitational theories with spontaneous Lorentz breaking / R. Bluhm -- The ALPHA antihydrogen experiment / N. Madsen et al. -- Atom interferometry tests the isotropy of post-Newtonian gravity / H. Müller et al. -- Probing Lorentz symmetry with gravitationally coupled matter / J. D. Tasson -- Torsion balance test of preferred-frame and weak coupling to polarized electrons / B. R. Heckel et al. -- Seeking a solution of the pioneer anomaly / M. M. Nieto and J. D. Anderson -- Testing Lorentz symmetry with gravity / Q. C. Bailey -- Preferred frame effects in relativistic binary pulsars / M. Kramer and N. Wex -- APOLLO: next generation lunar laser ranging / T. W. Murphy, Jr. et al. -- Constraints on Lorentz violation from gravity Probe B / J. M. Overduin -- Preliminary results from a test of CPT and Lorentz symmetry using a K-[symbol]He co-magnetometer / T. W. Kornack, G. Vasilakis, and M. V. Rornalis -- Constraining quantum gravity with GLAST / F. Kuehn, R. Hughes, and B. Winer -- Renormalization of Lorentz-violating theories / D. Anselmi -- Renormalization of gauge theories with Lorentz violation / D. Colladay and P. McDonald -- A POEM-based test of the WEP using a Sounding Rocket (SR-POEM) / R. D. Reasenberg and J. D. Phillips -- Testing alternative oscillation scenarios with atmospheric neutrinos using AMANDA-II data from 2000 to 2003 / J. Ahrens and J. L. Kelley -- Measurement of the ground-state hyperfine splitting of antihydrogen / B. Juhász and E. Widmann -- Spontaneous Lorentz violation and baryogenesis / J. Shu -- Lorentz invariance tested with fast optical ion clocks in a storage ring / G. Gwinner et al. -- Bose-Einstein condensates and Lorentz violation / D. Colladay and P. McDonald -- Embedding geometry and decomposition of gravity / T. E. Clark et al. -- The first lunar laser ranging constraints on gravity sector SME parameters / J. B. R. Battat, J. F. Chandler, and C. W. Stubbs -- A theory of gravity from Lorentz violation / R. Potting -- Search for Lorentz violation in a high-frequency gravitational experiment below 50 microns / W. A. Jensen, S. M. Lewis, and J. C. Long -- Lorentz violation and torsion / N. Russell -- Probing Lorentz invariance using coherent optical phenomena / J. P. Cotter, M. P. Hill, and B. T. H. Varcoe -- Constraint analysis of bumblebee models / N. Gagne and A. Vrublevslcis -- Ives-Stilwell for the new millennium / M. A. Nohensee, D. F. Phillips, and R. L. Walsworth -- Test for

Kostelecký, V. Alan

2008-03-01

395

Contribution of Family Environment to Pediatric Cochlear Implant Users' Speech and Language Outcomes: Some Preliminary Findings  

ERIC Educational Resources Information Center

Purpose: To evaluate the family environments of children with cochlear implants and to examine relationships between family environment and postimplant language development and executive function. Method: Forty-five families of children with cochlear implants completed a self-report family environment questionnaire (Family Environment Scale-Fourth

Holt, Rachael Frush; Beer, Jessica; Kronenberger, William G.; Pisoni, David B.; Lalonde, Kaylah

2012-01-01

396

Studying Possibilities of the IHEP Neutrino Channel.  

National Technical Information Service (NTIS)

Given are the results of investigation of operating regimes of the IHEP neutrino channel which can ensure to conduct experiments with the required parameters of neutrino spectra. The muon distributions in the neutrino channel shield, where pi - and K-meso...

A. P. Bugorskii S. A. Knyazev V. I. Kotov V. I. Kochetkov V. I. Kurbakov

1980-01-01

397

Velocity and Distribution of Primordial Neutrinos  

Microsoft Academic Search

The cosmic neutrinos background (CNB) comprises primordial neutrinos that were decoupled when the Universe was very young. Its detection is complicated, especially if we take into account neutrino mass and a possible breaking of Lorentz invariance at high energy, but has a fundamental relevance to studying the Big Bang. In this paper, we will see that a Lorentz violation does

Jorge Alfaro; Pablo González

2008-01-01

398

Cosmology and neutrino masses - An update  

NASA Astrophysics Data System (ADS)

Present cosmological observations yield an upper bound on the neutrino mass which is significantly stronger than laboratory bounds. However, the exact value of the cosmological bound is model dependent and therefore less robust. Here, I review the current status of cosmological neutrino mass bounds and also discuss implications for sterile neutrinos and LSND in particular.

Hannestad, Steen

399

The neutrino mass window for baryogenesis  

Microsoft Academic Search

Interactions of heavy Majorana neutrinos in the thermal phase of the early universe may be the origin of the cosmological matter–antimatter asymmetry. This mechanism of baryogenesis implies stringent constraints on light and heavy Majorana neutrino masses. We derive an improved upper bound on the CP asymmetry in heavy neutrino decays which, together with the kinetic equations, yields an upper bound

Wilfried Buchmüller; P. Di Bari; Michael Plümacher

2003-01-01

400

The Neutrino Mass Window for Baryogenesis  

Microsoft Academic Search

Interactions of heavy Majorana neutrinos in the thermal phase of the early universe may be the origin of the cosmological matter-antimatter asymmetry. This mech- anism of baryogenesis implies stringent constraints on light and heavy Majorana neutrino masses. We derive an improved upper bound on the CP asymmetry in heavy neutrino decays which, together with the kinetic equations, yields an upper

W. Buchmuller; P. Di Bari

401

Quantum Gravity on Neutrino Mass Square Difference  

Microsoft Academic Search

We consider the non-renormalizable interaction term as a perturbation of the neutrino mass matrix. We assume that the neutrino masses and mixing arise through physics at a scale intermediate between Planck scale and the electroweak breaking scale. We also assume that, just above the electroweak breaking scale, neutrino masses are nearly degenerate and their mixing is bi-maximal. Quantum gravity (Planck

Bipin Singh Koranga

2010-01-01

402

THE SEARCH FOR MASSIVE NEUTRINOS - Short Contribution  

NASA Astrophysics Data System (ADS)

Double beta decay (DBD) has the potential to distinguish whether neutrinos are Majorana or Dirac particles. However, neutrinoless DBD (in violation of lepton number conservation) has not yet been observed. From the respective upper limits, limits on the neutrino restmass can be deduced if the neutrino is of Majorana type.

Kirsten, T.

403

Flipped heavy neutrinos. From the solar neutrino problem to baryogenesis  

NASA Astrophysics Data System (ADS)

We discuss baryogenesis using the flipped SU(5) model for lepton mass matrices. We show that the generalized see-saw mechanism in this model cannot only provide MSW neutrino mixing suitable for solving the solar neutrino problem, and supply a hot dark matter candidate (v?) with mass O(10)eV as indicated by recent COBE results, but can also naturally account for the baryon asymmetry of the universe. Heavy singlet neutrino decay generates a net lepton asymmetry which is subsequently reprocessed by non-perturbative electroweak interactions. We evaluate the baryon asymmetry so produced in light of the constraints that the COBE observations put on inflationary cosmologies, finding it comfortably consistent with observation.

Ellis, John; Nanopoulos, D. V.; Olive, Keith A.

1993-02-01

404

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

405

Solar neutrinos: Interpretation of results  

NASA Astrophysics Data System (ADS)

Recent SNO results give strong evidence that the solar neutrinos undergo flavor conversion. The main issue now is the identification of the mechanism of conversion. The LMA MSW solution with ?m2 = (5-7)·10 -5 eV 2, tan 2? = 0.35-0.45 looks rather plausible: it fits well the experimental data and our new theoretical prejudices. In the LMA case, KamLAND should see (0.5 - 0.7) reduced signal. VAC-QVO and LOW are accepted at about 3?-level. The SMA solution is practically excluded. No sub-leading effects produced by Ue3 and admixture of sterile neutrino have been found. The fit becomes worse with an increase of Ue3 (for LMA) and a ?s admixture. Still a (30 - 50)% presence of the sterile neutrino is allowed. Solutions based on the neutrino spin-flip in the magnetic fields of the Sun as well as on non-standard neutrino interactions give a good fit of the data. If KamLAND confirms LMA MSW, the spin-flip and non-standard interactions can be considered (and will be searched for) as sub-leading effects.

Smirnov, A. Yu.

2003-04-01

406

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

407

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

408

The Low Energy Neutrino Factory  

SciTech Connect

We show that a low energy neutrino factory with a baseline of 1300 km and muon energy of 4.5 GeV has an excellent physics reach. The results of our optimisation studies demonstrate that such a setup can have remarkable sensitivity to theta{sub 13} and delta for sin{sup 2}(2theta{sub 13})>10{sup -4}, and to the mass hierarchy for sin{sup 2}(2theta{sub 13})>10{sup -3}. We also illustrate the power of the unique combination of golden and platinum channels accessible to the low energy neutrino factory. We have considered both a 20 kton totally active scintillating detector and a 100 kton liquid argon detector as possible detector technologies, finding that a liquid argon detector with very good background rejection can produce sensitivity to theta{sub 13} and delta with that of the International Design Study neutrino factory.

Bross, Alan; Geer, Steve [Fermi National Accelerator Laboratory, Batavia (United States); Ellis, Malcolm [Brunel University, London (United Kingdom); Fernandez Martinez, Enrique [Max-Planck-Institut fuer Physik (Werner-Heisenberg-Institut), Muenchen (Germany); Li, Tracey; Pascoli, Silvia [Institute for Particle Physics Phenomenology, Durham University (United Kingdom); Mena, Olga [Instituto de Fisica Corpuscular, IFIC CSIC and Universidad de Valencia (Spain)

2010-03-30

409

Status of neutrino mass experiments  

SciTech Connect

In 1980 two experiments ignited a fertile field of research the determination of the neutrino masses. Subsequently, over 35 experiments using a variety of techniques have probed or are probing this question. Primarily I will discuss electron antineutrino (hereafter referred to as neutrino) mass experiments. However, let me begin in Section I to discuss astronomical and terrestrial observations which motivated these experiments. In Section II, I will quote limits from muon and tau mass determinations. These limits are more thoroughly discussed in other papers. I will continue by describing the four approaches used to measure the electron neutrino mass. In Section III, tritium beta decay mass determinations will be reviewed. This section includes a general summary of previous experimental results, and discussion of the major ongoing experiments. Section IV offers concluding remarks. 24 refs., 24 figs.

Fackler, O.

1985-12-01

410

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

411

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

412

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

413

The antares neutrino detector instrumentation  

NASA Astrophysics Data System (ADS)

ANTARES is actually the fully operational and the largest neutrino telescope in the Northern hemisphere. Located in the Mediterranean Sea, it consists of a 3D array of 885 photomultiplier tubes (PMTs) arranged in 12 detection lines (25 storeys each), able to detect the Cherenkov light induced by upgoing relativistic muons produced in the interaction of high energy cosmic neutrinos with the detector surroundings. Among its physics goals, the search for neutrino astrophysical sources and the indirect detection of dark matter particles coming from the sun are of particular interest. To reach these goals, good accuracy in track reconstruction is mandatory, so several calibration systems for timing and positioning have been developed. In this contribution we will present the design of the detector, calibration systems, associated equipment and its performance on track reconstruction.

Yepes-Ramírez, H.

2012-01-01

414

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

415

Neutrino oscillations in noisy media  

SciTech Connect

The authors develop the Redfield equation for delta-correlated gaussian noise and apply it to the case of two neutrino flavor or spin precession in the presence of a noisy matter density or magnetic field, respectively. The criteria under which physical fluctuations can be well approximated by the delta-correlated gaussian noise for the above cases are examined. Current limits on the possible neutrino magnetic moment and solar magnetic field suggest that a reasonably noisy solar magnetic field would not appreciably affect the solar electron neutrino flux. However, if the solar electron density has fluctuations of a few percent of the local density and a small enough correlation length, the MSW effect is suppressed for a range of parameters.

Loreti, F.N.; Balantekin, A.B.

1994-05-27

416

Determining neutrino mass hierarchy by precise measurements of two delta m**2 in electron-neutrino and muon-neutrino disappearance experiments.  

National Technical Information Service (NTIS)

In this talk, we discuss the possibility of determining the neutrino mass hierarchy by comparing the two effective atmospheric neutrino mass squared differences measured, respectively, in electron, and in muon neutrino disappearance oscillation experiment...

H. Minakata H. Nunokawa R. Z. Funchal S. Parke

2006-01-01

417

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

418

Contributed report: Flavor anarchy for Majorana neutrinos  

NASA Astrophysics Data System (ADS)

We argue that neutrino flavor parameters may exhibit features that are very different from those of quarks and charged leptons. Specifically, within the Froggatt--Nielsen (FN) framework, charged fermion parameters depend on the ratio between two scales, while for neutrinos a third scale -- that of lepton number breaking -- is involved. Consequently, the selection rules for neutrinos may be different. In particular, if the scale of lepton number breaking is similar to the scale of horizontal symmetry breaking, neutrinos may become flavor-blind even if they carry different horizontal charges. This provides an attractive mechanism for neutrino flavor anarchy.

Nir, Yosef; Shadmi, Yael

2004-12-01

419

Measuring Neutrinos with the ANTARES Telescope  

SciTech Connect

The ANTARES underwater neutrino telescope has been taking data since construction began in 2006. The telescope, completed in May of 2008, detects the Cerenkov radiation of charged leptons produced by high energy neutrinos interacting in or around the detector. The lepton trajectory is reconstructed with high precision, revealing the direction of the incoming neutrino. The performance of the detector will be discussed and recent data showing muons, electromagnetic showers and atmospheric neutrinos will be presented. Studies have been underway to search for neutrino point sources in the ANTARES data since 2007. Results from these studies will be presented, and the sensitivity of the telescope will be discussed.

Reed, Corey [National Institute for Subatomic Physics (Nikhef), Amsterdam (Netherlands)

2009-12-17

420

Generic lepton mass matrices and neutrino oscillations  

NASA Astrophysics Data System (ADS)

Several intriguing aspects of neutrino oscillation phenomenology like the origin of small neutrino masses, the absolute neutrino mass scale, the neutrino mass hierarchy, i.e., normal or inverted, and the nature of neutrinos, i.e., Dirac or Majorana, etc. have been addressed from a general perspective. We show how the fundamental considerations of unitary transformations, naturalness, and the seesaw mechanism suffice to determine the texture structure of fermion Yukawa couplings and discuss the significance of the effective mass in 0??? decay for the texture structure of these couplings.

Verma, Rohit

2014-03-01

421

Neutrino mass from beta decay  

NASA Astrophysics Data System (ADS)

The investigation of the endpoint spectrum of the tritium ? decay is still the most sensitive direct method to determine the neutrino mass scale. The KATRIN experiment currently being set up at the Forschungszentrum Karlsruhe will improve the neutrino mass sensitivity compared to the previous Mainz and Troitsk experiments by one order of magnitude down to 0.2 eV/c 2. The first generation of cryobolometric experiments at Genova and Milan using the isotope 187Re will be followed up by the MARE experiment which aims to eventually reach a similar sensitivity.

Weinheimer, Ch.

2007-06-01

422

Baryon asymmetry and neutrino mixing  

NASA Astrophysics Data System (ADS)

In theories where B - L is a spontaneously broken local symmetry, the cosmological baryon asymmetry can be generated by the out-of-equilibrium decay of heavy Majorana neutrinos. We study this mechanism assuming a similar pattern of mixings and masses for leptons and quarks, as suggested by SO(10) unification. This implies that B - L is broken at the unification scale ?GUT ~ 1016 GeV, if m?? ~ 3 . 10-3eV as preferred by the MSW explanation of the solar neutrino deficit. The observed value of the baryon asymmetry, nB/(s ~ 10-10), is then obtained without any fine tuning of parameters.

Buchmüller, W.; Plümacher, M.

1996-02-01

423

Hierarchical neutrinos and supersymmetric inflation  

NASA Astrophysics Data System (ADS)

A moderate extension of MSSM based on a left-right symmetric gauge group, within which hybrid inflation is `naturally' realized, is discussed. The ? problem is solved via a Peccei-Quinn symmetry. Light neutrinos acquire hierarchical masses by the seesaw mechanism. They are taken from the small angle MSW resolution of the solar neutrino puzzle and the SuperKamiokande data. The range of parameters consistent with maximal ??-?? mixing and the gravitino constraint is determined. The baryon asymmetry of the universe is generated through a primordial leptogenesis. The subrange of parameters, where the baryogenesis constraint is also met, is specified. The required values of parameters are more or less `natural'.

Lazarides, G.; Vlachos, N. D.

1999-07-01

424

Fourth ventricle meningiomas: a rare entity.  

PubMed

Fourth ventricle meningiomas (FVMs) are rare, often misdiagnosed, lesions. To the best of our knowledge, 47 cases have been reported in the literature: we describe our series of three cases treated at our Institution, focusing on some diagnostic tips and intraoperative features of these tumours. Our three patients have a history of headache. Gait disturbances, vomiting and/or diplopia complicated the clinical picture before the referral at our Department. The operations were uneventful, and the patients fully recovered from neurological symptoms. They are free of recurrence at a median follow-up of 19 years. FVMs are rare lesions, which are difficult to differentiate preoperatively from the much more common ependymomas. A preoperative distinction would be extremely advantageous: indeed, although both tumours share similar radiological and clinical patterns, they clearly differ as to surgical difficulty and outcome. In fact, meningiomas are comparatively easier to remove, granting better clinical results. PMID:21707237

Pichierri, Angelo; Ruggeri, Andrea; Morselli, Carlotta; Delfini, Roberto

2011-08-01

425

FIRST NEUTRINO POINT-SOURCE RESULTS FROM THE 22-STRING ICECUBE DETECTOR  

SciTech Connect

We present new results of searches for neutrino point sources in the northern sky, using data recorded in 2007-08 with 22 strings of the IceCube detector (approximately one-fourth of the planned total) and 275.7 days of livetime. The final sample of 5114 neutrino candidate events agrees well with the expected background of atmospheric muon neutrinos and a small component of atmospheric muons. No evidence of a point source is found, with the most significant excess of events in the sky at 2.2 {sigma} after accounting for all trials. The average upper limit over the northern sky for point sources of muon-neutrinos with E{sup -2} spectrum is E{sup 2} {Phi}{sub {nu}{sub {mu}}} < 1.4 x 10{sup -1} TeV cm{sup -2}s{sup -1}, in the energy range from 3 TeV to 3 PeV, improving the previous best average upper limit by the AMANDA-II detector by a factor of two.

IceCube Collaboration; Klein, Spencer

2009-05-14

426

First Neutrino Point-Source Results from the 22 String Icecube Detector  

NASA Astrophysics Data System (ADS)

We present new results of searches for neutrino point sources in the northern sky, using data recorded in 2007-2008 with 22 strings of the IceCube detector (approximately one-fourth of the planned total) and 275.7 days of live time. The final sample of 5114 neutrino candidate events agrees well with the expected background of atmospheric muon neutrinos and a small component of atmospheric muons. No evidence of a point source is found, with the most significant excess of events in the sky at 2.2? after accounting for all trials. The average upper limit over the northern sky for point sources of muon-neutrinos with E -2 spectrum is E^{2} ?_{?_{?}} < 1.4 × 10^{-11} TeV cm^{-2} s^{-1}, in the energy range from 3 TeV to 3 PeV, improving the previous best average upper limit by the AMANDA-II detector by a factor of 2.

Abbasi, R.; Abdou, Y.; Ackermann, M.; Adams, J.; Aguilar, J.; Ahlers, M.; Andeen, K.; Auffenberg, J.; Bai, X.; Baker, M.; Barwick, S. W.; Bay, R.; Bazo Alba, J. L.; Beattie, K.; Beatty, J. J.; Bechet, S.; Becker, J. K.; Becker, K.-H.; Benabderrahmane, M. L.; Berdermann, J.; Berghaus, P.; Berley, D.; Bernardini, E.; Bertrand, D.; Besson, D. Z.; Bissok, M.; Blaufuss, E.; Boersma, D. J.; Bohm, C.; Bolmont, J.; Böser, S.; Botner, O.; Bradley, L.; Braun, J.; Breder, D.; Castermans, T.; Chirkin, D.; Christy, B.; Clem, J.; Cohen, S.; Cowen, D. F.; D'Agostino, M. V.; Danninger, M.; Day, C. T.; De Clercq, C.; Demirörs, L.; Depaepe, O.; Descamps, F.; Desiati, P.; de Vries-Uiterweerd, G.; De Young, T.; Diaz-Velez, J. C.; Dreyer, J.; Dumm, J. P.; Duvoort, M. R.; Edwards, W. R.; Ehrlich, R.; Eisch, J.; Ellsworth, R. W.; Engdegård, O.; Euler, S.; Evenson, P. A.; Fadiran, O.; Fazely, A. R.; Feusels, T.; Filimonov, K.; Finley, C.; Foerster, M. M.; Fox, B. D.; Franckowiak, A.; Franke, R.; Gaisser, T. K.; Gallagher, J.; Ganugapati, R.; Gerhardt, L.; Gladstone, L.; Goldschmidt, A.; Goodman, J. A.; Gozzini, R.; Grant, D.; Griesel, T.; Groß, A.; Grullon, S.; Gunasingha, R. M.; Gurtner, M.; Ha, C.; Hallgren, A.; Halzen, F.; Han, K.; Hanson, K.; Hasegawa, Y.; Heise, J.; Helbing, K.; Herquet, P.; Hickford, S.; Hill, G. C.; Hoffman, K. D.; Hoshina, K.; Hubert, D.; Huelsnitz, W.; Hülß, J.-P.; Hulth, P. O.; Hultqvist, K.; Hussain, S.; Imlay, R. L.; Inaba, M.; Ishihara, A.; Jacobsen, J.; Japaridze, G. S.; Johansson, H.; Joseph, J. M.; Kampert, K.-H.; Kappes, A.; Karg, T.; Karle, A.; Kelley, J. L.; Kenny, P.; Kiryluk, J.; Kislat, F.; Klein, S. R.; Klepser, S.; Knops, S.; Kohnen, G.; Kolanoski, H.; Köpke, L.; Kowalski, M.; Kowarik, T.; Krasberg, M.; Kuehn, K.; Kuwabara, T.; Labare, M.; Lafebre, S.; Laihem, K.; Landsman, H.; Lauer, R.; Leich, H.; Lennarz, D.; Lucke, A.; Lundberg, J.; Lünemann, J.; Madsen, J.; Majumdar, P.; Maruyama, R.; Mase, K.; Matis, H. S.; McParland, C. P.; Meagher, K.; Merck, M.; Mészáros, P.; Middell, E.; Milke, N.; Miyamoto, H.; Mohr, A.; Montaruli, T.; Morse, R.; Movit, S. M.; Münich, K.; Nahnhauer, R.; Nam, J. W.; Nießen, P.; Nygren, D. R.; Odrowski, S.; Olivas, A.; Olivo, M.; Ono, M.; Panknin, S.; Patton, S.; Pérez de los Heros, C.; Petrovic, J.; Piegsa, A.; Pieloth, D.; Pohl, A. C.; Porrata, R.; Potthoff, N.; Price, P. B.; Prikockis, M.; Przybylski, G. T.; Rawlins, K.; Redl, P.; Resconi, E.; Rhode, W.; Ribordy, M.; Rizzo, A.; Rodrigues, J. P.; Roth, P.; Rothmaier, F.; Rott, C.; Roucelle, C.; Rutledge, D.; Ryckbosch, D.; Sander, H.-G.; Sarkar, S.; Satalecka, K.; Schlenstedt, S.; Schmidt, T.; Schneider, D.; Schukraft, A.; Schulz, O.; Schunck, M.; Seckel, D.; Semburg, B.; Seo, S. H.; Sestayo, Y.; Seunarine, S.; Silvestri, A.; Slipak, A.; Spiczak, G. M.; Spiering, C.; Stamatikos, M.; Stanev, T.; Stephens, G.; Stezelberger, T.; Stokstad, R. G.; Stoufer, M. C.; Stoyanov, S.; Strahler, E. A.; Straszheim, T.; Sulanke, K.-H.; Sullivan, G. W.; Swillens, Q.; Taboada, I.; Tarasova, O.; Tepe, A.; Ter-Antonyan, S.; Terranova, C.; Tilav, S.; Tluczykont, M.; Toale, P. A.; Tosi, D.; Tur?an, D.; van Eijndhoven, N.; Vandenbroucke, J.; Van Overloop, A.; Voigt, B.; Walck, C.; Waldenmaier, T.; Walter, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.; Wiebusch, C. H.; Wiedemann, A.; Wikström, G.; Williams, D. R.; Wischnewski, R.; Wissing, H.; Woschnagg, K.; Xu, X. W.; Yodh, G.; Ice Cube Collaboration

2009-08-01

427

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

428

Mechanical characterization of fourth generation composite humerus.  

PubMed

Mechanical data on upper extremity surrogate bones, supporting use as biomechanical tools, is limited. The objective of this study was to characterize the structural behaviour of the fourth-generation composite humerus under simulated physiologic bending, specifically, stiffness, rigidity, and mid-diaphysial surface strains. Three humeri were tested in four-point bending, in anatomically defined anteroposterior (AP) and mediolateral (ML) planes. Stiffness and rigidity were derived using load-displacement data. Principal strains were determined at the anterior, posterior, medial, and lateral surfaces in the humeral mid-diaphysial transverse plane of one specimen using stacked rosettes. Linear structural behaviour was observed within the test range. Average stiffness and rigidity were greater in the ML (918 +/- 18 N/mm; 98.4 +/- 1.9 Nm2) than the AP plane (833 +/- 16 N/mm; 89.3 +/- 1.6 Nm2), with little inter-specimen variability. The ML/AP rigidity ratio was 1.1. Surface principal strains were similar at the anterior (5.41 micro epsilon/N) and posterior (5.43 micro epsilon/N) gauges for AP bending, and comparatively less for ML bending, i.e. 5.1 and 4.5 micro epsilon/N, at the medial and lateral gauges, respectively. This study provides novel strain and stiffness data for the fourth-generation composite humerus and also adds to published construct rigidity data. The presented results support the use of this composite bone as a tool for modelling and experimentation. PMID:22320056

Grover, P; Albert, C; Wang, M; Harris, G F

2011-12-01

429

Mass freezing in growing neutrino quintessence  

SciTech Connect

Growing neutrino quintessence solves the coincidence problem for dark energy by a growing cosmological value of the neutrino mass which emerges from a cosmon-neutrino interaction stronger than gravity. The cosmon-mediated attraction between neutrinos induces the formation of large-scale neutrino lumps in a recent cosmological epoch. We argue that the nonlinearities in the cosmon field equations stop the further increase of the neutrino mass within sufficiently dense and large lumps. As a result, we find the neutrino-induced gravitational potential to be substantially reduced when compared to linear extrapolations. We furthermore demonstrate that inside a lump the possible time variation of fundamental constants is much smaller than their cosmological evolution. This feature may reconcile current geophysical bounds with claimed cosmological variations of the fine structure constant.

Nunes, Nelson J.; Schrempp, Lily; Wetterich, Christof [Institut fuer Theoretische Physik, Universitaet Heidelberg, Philosophenweg 16, 69120 Heidelberg (Germany)

2011-04-15

430

A cosmological bound on radiative neutrino lifetime  

NASA Astrophysics Data System (ADS)

Neutrino oscillation experiments and direct bounds on absolute masses constrain neutrino mass differences to fall into the microwave energy range, for most of the allowed parameter space. As a consequence of these recent phenomenological advances, older constraints on radiative neutrino decays based on diffuse background radiations and assuming strongly hierarchical masses in the eV range are now outdated. We thus derive new bounds on the radiative neutrino lifetime using the high precision cosmic microwave background spectral data collected by the FIRAS instrument on board of COBE. The lower bound on neutrino lifetime is between a few ×1019 s and ~ 5 × 1020 s, depending on the neutrino mass ordering and on the absolute neutrino mass scale. However, due to phase space limitations, the upper bound on the effective magnetic moment mediating the decay is not better than ~10-8 ?B. We also comment about possible improvements of these limits, by means of recent diffuse infrared photon background data.

Mirizzi, A.; Montanino, D.; Serpico, P. D.

2008-07-01

431

Analysis of the solar neutrino data  

NASA Astrophysics Data System (ADS)

We analyse the solar neutrino data (pre-SNO) in the framework of two-neutrino, three-neutrino and four-neutrino schemes. We discuss the status of the different regimes that remain allowed (LMA, SMA and LOW-QVO). The solar and the atmospheric data are in good agreement with the CHOOZ data showing a preference for small ?13, where the stronger bound comes from the CHOOZ data. Also, we discuss the oscillations to active and sterile neutrinos in a unified picture: four-neutrino oscillations. Using the predictions for the next solar neutrino experiment, SNO, we discuss the questions that could be solved in the different frameworks. The data will be able to disfavour some of the solar regimes and also will be able to prove (or disprove) the 2+2 scenarios.

Peña-Garay, C.

2003-05-01

432

PREFACE: Neutrino physics at spallation neutron sources  

NASA Astrophysics Data System (ADS)

Unique because of their super-light masses and tiny interaction cross sections, neutrinos combine fundamental physics on the scale of the miniscule with macroscopic physics on the scale of the cosmos. Starting from the ignition of the primal p-p chain of stellar and solar fusion reactions that signal star-birth, these elementary leptons (neutrinos) are also critical players in the life-cycles and explosive deaths of massive stars and the production and disbursement of heavy elements. Stepping beyond their importance in solar, stellar and supernova astrophysics, neutrino interactions and properties influence the evolution, dynamics and symmetries of the cosmos as a whole. Further, they serve as valuable probes of its material content at various levels of structure from atoms and nuclei to valence and sea quarks. In the light of the multitude of physics phenomena that neutrinos influence, it is imperative to enhance our understanding of neutrino interactions and properties to the maximum. This is accentuated by the recent evidence of finite neutrino mass and flavour mixing between generations that reverberates on the plethora of physics that neutrinos influence. Laboratory experiments using intense neutrino fluxes would allow precision measurements and determination of important neutrino reaction rates. These can then complement atmospheric, solar and reactor experiments that have enriched so valuably our understanding of the neutrino and its repertoire of physics applications. In particular, intermediate energy neutrino experiments can provide critical information on stellar and solar astrophysical processes, along with advancing our knowledge of nuclear structure, sub-nuclear physics and fundamental symmetries. So where should we look for such intense neutrino sources? Spallation neutron facilities by their design are sources of intense neutrino pulses that are produced as a by-product of neutron spallation. These neutrino sources could serve as unique laboratories to enrich our knowledge of neutrino physics and the multifaceted science it interfaces. In fact, the neutrino energy spectra expected at spallation neutron facilities overlap remarkably with those emanating from distant supernovae and these sources seem `made to order' for terrestrial studies of supernova reactions. They are also in a suitable energy regime to pursue neutrino-mediated studies of nuclear structure, fundamental symmetries and solar reactions. Recent research indicates neutrino-nuclear reactions may be even more influential in supernova dynamics and detection than hitherto believed. The need for in-depth understanding of the individual neutrino-nuclear reactions that collectively have dramatic effects on the large-scale dynamics of evolving stars points to laboratory measurements of neutrino reactions on various nuclei as a premier requirement of neutrino-nuclear astrophysics. Such experimental data can improve our input to the extensive modelling projects that investigate the evolutionary stages of exploding supernovae and further our understanding of their internal physics. State-of-the-art simulations exploring the neutrino-reheating phases fail to produce explosions---yet clearly nature explodes her supernovae. Matters pertaining to the galactic abundance of very p-rich nuclei and the various isotope ratios are by no means well defined and demand further research, as do the intricacies of the nucleo-synthesis channels. Neutrino-nuclear experiments are also essential for proper development and calibration of appropriate supernova detectors. Solar neutrino research and detection have contributed vastly to our current understanding of neutrino science and have helped to validate the standard solar model. The chapter is by no means closed and experiments with intense neutrino fluxes could enrich valuably our understanding of both neutrino and solar physics. Neutrino nuclear reactions are not only important for their role in nuclear astrophysics, but also for the insight they provide on nuclear structure and the theoretical models used to calculat

Avignone, F. T.; Chatterjee, L.; Efremenko, Y. V.; Strayer, M.

2003-11-01

433

Supernova prompt neutronization neutrinos and neutrino magnetic moments  

Microsoft Academic Search

It is shown that the combined action of spin flavour conversions of supernova neutrinos due to the interactions of their Majorana-type transition magnetic moments with the supernova magnetic fields and flavour conversions due to the mass mixing can lead to the transformation of nue born in the neutronization process into their antiparticles bar nue. Such an effect would have a

Evgeny Kh Akhmedov; Takeshi Fukuyama

2003-01-01

434

Neutrino Charm Production and a Limit to Neutrino Oscillations  

Microsoft Academic Search

The production of charmed particles and a limit to tau lepton production have been measured using a hybrid emulsion spectrometer in the Fermilab wide-band neutrino beam. The relative cross section for charged current charmed particle production is. (DIAGRAM, TABLE OR GRAPHIC OMITTED...PLEASE SEE DAI). and the energy dependence of the cross section and the kinematic distributions of the charm events

David Charles Bailey

1983-01-01

435

Evaluation of a fourth-generation focal plane camera for use in plasma-source mass spectrometry  

SciTech Connect

A fourth-generation focal plane camera containing 1696 Faraday-strip detectors was fitted to a Mattauch-Herzog mass spectrograph and characterized for its performance with inductively coupled plasma ionization. The camera provides limits of detection in the single to tens of ng L-1 range for most elements and has a linear dynamic range of at least nine orders of magnitude. Isotope-ratio precision better than 0.02% has also been achieved with this device, and this fourth-generation system features the broadest simultaneous mass range obtainable to date with this family of focal plane camera detectors.

Felton, Jeremy A.; Schilling, G. D.; Ray, Steven J.; Sperline, Roger P.; Denton, M. Bonner; Barinaga, Charles J.; Koppenaal, David W.; Hieftje, Gary M.

2010-10-18

436

Black rings with fourth dipole cause less hair loss  

NASA Astrophysics Data System (ADS)

An example of entropy enigma with a controlled CFT dual was recently studied in [1]. The enigmatic bulk configurations, considered within the STU model, can be mapped under spectral flow into black rings with three monopole and dipole charges. Even though the bulk and CFT configurations existed in the same region of parameter space, the Bekenstein-Hawking entropy of the bulk configurations was found to be lower than the microscopic entropy from the CFT. While it is possible that the difference in entropy is due to the bulk and boundary configurations being at different points in the moduli space, it is also possible that the bulk configurations embeddable within the STU model are not the most entropic. New families of BPS black ring solutions with four electric and four dipole magnetic charges have recently been explicitly constructed in [2]. These black rings are not embeddable within the STU model. In this paper we investigate if these black rings can be entropically dominant over the STU model black rings. We find that the new black rings are always entropically subdominant to the STU-model black rings. However, for small fourth dipole charge these black rings continue to be dominant over the BMPV in a small region of parameters and are thus enigmatic.

Chowdhury, Borun D.

2012-07-01

437

California's population geography: lessons for a fourth grade class.  

PubMed

Purpose of this paper is to present a model for teaching fourth grade children some aspects of the population geography of California from a nontextual approach. The objective is to interest and instruct children in the mobility of the people, and on the reasons why so many families have moved to California from other states. Students should be alerted not only to internal migration problems, but to the excess of births over deaths. Materials necessary for the lessons are transparencies, overhead projector, marking pencils, chalk and chalkboard. After showing the students that California population has approximately doubled every 20 years, the students should be encouraged to find reasons explaining why people have moved to the state, should be able to categorize those reasons under the terms industrial/manufacturing, agricultural, urban or recreational, should learn how to plot population distribution on a California regional outline map, and should attempt to explain why certain parts of California are more popular than others. The teaching model described in this paper may be replicated with modfications for any grade level and area of study. PMID:12178554

Rushdoony, H A

1978-11-01

438

Symmetries in the fourth Painleve equation and Okamoto polynomials  

Microsoft Academic Search

We propose a new representation of the fourth Painlev\\\\'e equation in which the $A^{(1)}_2$-symmetries become clearly visible. By means of this representation, we clarify the internal relation between the fourth Painlev\\\\'e equation and the modified KP hierarchy. We obtain in particular a complete description of the rational solutions of the fourth Painlev\\\\'e equation in terms of Schur functions. This implies

Masatoshi Noumi; Yasuhiko Yamada

1997-01-01

439

Rosette-forming glioneuronal tumor of the fourth ventricle  

Microsoft Academic Search

Rosette-forming glioneuronal tumor (RGNT) of the fourth ventricle has been reported recently as a novel type of primary CNS neoplasm. We present the case of a 35-year-old male patient with RGNT of the fourth ventricle. The tumor was found incidentally; the patient did not suffer from any neurological symptoms. The tumor mass involved the caudal cerebellar vermis, filled the fourth

Matthias Preusser; Wolfgang Dietrich; Thomas Czech; Daniela Prayer; Herbert Budka; Johannes A. Hainfellner

2003-01-01

440

Even Start Family Literacy Program Evaluation, Oklahoma City Public Schools: A National Diffusion Network Approved Program, Family Intergenerational-Interaction Literacy Model 1993-94.  

ERIC Educational Resources Information Center

The Even Start Family Literacy Program, in its fourth year of operation, provides a literacy environment based on the Family Intergenerational-Interaction Literacy Model (FILM) in the southwest area of Oklahoma City. The FILM model is designed to provide a family literacy education program for parents, extended family, and their preschool children…

Oklahoma City Univ., OK.

441

4. RAMP FOR BENJAMIN FRANKLIN BRIDGE (FOURTH ST.) BETWEEN VINE ...  

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

4. RAMP FOR BENJAMIN FRANKLIN BRIDGE (FOURTH ST.) BETWEEN VINE AND RACE STS., LOOKING NORTHWEST - Independence National Historical Park, Walnut, Sixth, Chestnut & Second Streets, Philadelphia, Philadelphia County, PA

442

Charmed hadron production by neutrinos  

Microsoft Academic Search

Charmed hadron production has been studied using a hybrid emulsion spectrometer in the Fermilab wide-band neutrino beam. The relative rates of D0, D+, F+, and Lambda+c production have been measured - the fraction of D mesons is 69 +\\/- 810%. Momentum, transverse momentum, Feynman X, and fragmentation (Z) distributions are presented. The mean Z for charmed hadrons is 0.59 +\\/-

N. Ushida; T. Kondo; F. Fujioka; H. Fukushima; Y. Takahashi; S. Tatsumi; C. Yokohama; Y. Homma; Y. Tsuzuki; S. Bahk; C. Kim; J. Song; D. Bailey; S. Conetti; J. Fischer; J. Trischuk; H. Fuchi; K. Hoshino; M. Miyanashi; K. Niu; K. Niwa; H. Shibuya; Y. Yanagisawa; S. Errede; M. Gutzwiller; S. Kuramata; N. W. Reay; K. Reibel; T. A. Romanowski; R. Sidwell; N. R. Stanton; K. Moriyama; H. Shibata; T. Hara; O. Kusumoto; Y. Noguchi; M. Teranaka; H. Okabe; J. Yokota; J. Harnois; C. Hébert; J. Hébert; S. Lokanathan; B. McLeod; S. Tasaka; P. Davis; J. Martin; D. Pitman; J. D. Prentice; P. Sinervo; T. S. Yoon; H. Kimura; Y. Maeda

1983-01-01

443

The Case for Neutrino Oscillations  

Microsoft Academic Search

No abstract appeared in the Proceedings, but I am adding the following summary at the request of the X^3 people: The idea of neutrino masses is discussed in the context of grand unified theories., and various scenarios are presented, including the seesaw mechanism. At the end, preference is stated for maximal mixing between $\\\

P. Ramond

2000-01-01

444

A new solar neutrino detector  

Microsoft Academic Search

This paper describes the main features of the proposed low energy solar neutrino detector Borexino, planned to be installed at the Gran Sasso Laboratory. This real time detector is based on a massive, calorimetric, liquid scintillation spectroscopy technique, whose high luminosity is the base for the attempt to achieve a low signal detection threshold. After a description of the main

G. Alimonti; B. Alpat; C. Arpesella; G. Bellini; P. Benetti; S. Bonetti; F. P. Calaprice; M. Campanella; G. Cecchet; A. de Bari; M. Deutsch; A. Donati; F. Elisei; F. von Feilitzsch; D. Franciotti; M. G. Giammarchi; D. Giugni; A. Golubchikov; G. Husser; T. Kovacs; I. Manno; G. Mantovani; G. Manuzio; F. Masetti; U. Mazzucato; E. Meroni; J. Mitchell; L. Oberauer; S. Pakvasa; A. Perotti; A. Preda; P. Raghavan; R. S. Raghavan; F. Ragusa; G. Ranucci; R. Scardaoni; S. Schonert; O. Smirnov; R. Tartaglia; G. Testera; P. Ullucci; S. Vitale; O. Zaimidoroga

1993-01-01

445

Majorana Neutrinos and Magnetic Fields.  

National Technical Information Service (NTIS)

It is stressed that if neutrinos are massive they are probably of Majorana type. This implies that their magnetic moment form factor vanishes identically so that the previously discussed phenomenon of spin rotation in a magnetic field would not appear to ...

J. Schechter J. W. F. Valle

1981-01-01

446

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

447

Neutrino Event Generators: A Review  

SciTech Connect

Event generators play an important role in the design, optimization, and execution of neutrino experiments. In this paper I will review the status of event generators used in this field, focusing on advances since the start of the NuINT conference series in 2001.

Gallagher, Hugh R. [Tufts University, Medford, Massachusetts (United States)

2009-11-25

448

AMANDA South Pole neutrino detector.  

NASA Astrophysics Data System (ADS)

It is proposed to instrument the polar ice cap as a low-noise particle detector sensing the Cherenkov light from neutrino-induced muons. This paper describes the successful operation of a prototype string of optical modules that where deployed on January 17, 1992 at the South Pole.

Barwick, S. W.; Lynch, J.; Porrata, R.; Yodh, G.; Lowder, D.; Miller, T.; Price, B.; Richards, A.; Snowden-Ifft, D.; Westphal, A.; Halzen, F.; Jacobsen, J.; Kandhadai, V.; Liubarsky, I.; Morse, R.; Tilav, S.

449

New ideas in neutrino detection  

NASA Astrophysics Data System (ADS)

What is new in the field of neutrino detection? In addition to new projects probing both the low and high ends of the neutrino energy scale, an inexpensive, effective technique is being developed to allow tagging of antineutrinos in water Cherenkov (WC) detectors via the addition to water of a solute with a large neutron cross-section and energetic ? daughters. Gadolinium is an excellent candidate since in recent years it has become very inexpensive, now less than 8 per kilogram in the form of commercially available gadolinium trichloride. This non-toxic, non-reactive substance is highly soluble in water. Neutron capture on gadolinium yields an 8.0~MeV gamma cascade easily seen in detectors like Super-Kamiokande. The uses of GdCl_3 as a possible upgrade for the Super-Kamiokande detector -- with a view toward improving its performance as an antineutrino detector for supernova neutrinos and reactor neutrinos -- are discussed, as are the ongoing R&D efforts which aim to make this dream a reality within the next two years.

Vagins, M. R.

2006-10-01

450

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

451

Recent progress in neutrino - astrophysics connections  

NASA Astrophysics Data System (ADS)

Of all the constituents within the standard model of particle physics our understanding of the neutrino has benefited the most from the interaction of astrophysics and `terraphysics.' Much has been learned about the properties of the neutrino from each: experiments here on Earth temper our appreciation of the role that neutrinos play in the cosmos while astrophysics can provide the densities and temperatures in which the neutrinos do more than simply flee. But the reluctance of neutrinos to interact means that it is not until we venture into the most extreme environments of astrophysics that we observe neutrinos `pushing back' as hard as they are being `pushed'. We review two sites where this occurs: the early Universe and the accretion disk `engines' of gamma ray bursts. Neutrinos play an important role in the evolution of the early Universe with a particular focus upon the electron neutrino in determining the primordial elemental composition via its participation in the most important reaction at that time. Within gamma ray burst accretion disks we again see the electron neutrinos at work in the nuclear reactions and through their function as the `coolant' for the disk. Removal of the disk energy, and its deposition into the remnants of the massive star surrounding the disk, may lead to the formation of highly relativistic jets that will later be observed as the burst. We show what has been learned so far about the neutrino and its properties from the study of such environments.

Kneller, James

2005-04-01

452

Status of global fits to neutrino oscillations  

NASA Astrophysics Data System (ADS)

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 the robustness of the oscillation interpretation against departures from the Standard Solar Model and the possible existence of non-standard neutrino physics. Furthermore, we give the best-fit values and allowed ranges of the three-flavour oscillation parameters from the current worlds' global neutrino data sample and discuss in detail the status of the small parameters agr equiv DgrmSOL2/DgrmATM2 as well as sin2 thgr13, which characterize the strength of CP violating effects in neutrino oscillations. We also update the degree of rejection of four-neutrino interpretations of the LSND evidence in view of the most recent developments.

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

2004-09-01

453

Family Togetherness  

Microsoft Academic Search

Members of Florence Kaslow's family of procreation share their insights into the myriad ways in which her professional contributions in family psychology and international psychology have had an impact on their family life. Particular attention is paid to the family life of psychotherapists, healthy family functioning, healthy long-term marriages, sex therapy, military psychology, family business consulting and the use of

Nadine J. Kaslow; Solis Kaslow; Howard I. Kaslow

2004-01-01

454

Towards the resolution of the solar neutrino problem.  

National Technical Information Service (NTIS)

A number of experiments have accumulated over the years a large amount of solar neutrino data. The data indicate that the observed solar neutrino flux is significantly smaller than expected and, furthermore, that the electron neutrino survival probability...

A. Friedland

2000-01-01

455

Measurement of Neutrino Oscillation Parameters from Muon Neutrino Disappearance with an Off-Axis Beam  

NASA Astrophysics Data System (ADS)

The T2K Collaboration reports a precision measurement of muon neutrino disappearance with an off-axis neutrino beam with a peak energy of 0.6 GeV. Near detector measurements are used to constrain the neutrino flux and cross section parameters. The Super-Kamiokande far detector, which is 295 km downstream of the neutrino production target, collected data corresponding to 3.01×1020 protons on target. In the absence of neutrino oscillations, 205±17 (syst) events are expected to be detected while only 58 muon neutrino event candidates are observed. A fit to the neutrino rate and energy spectrum, assuming three neutrino flavors and normal mass hierarchy yields a best-fit mixing angle sin?2(?23)=0.514±0.082 and mass splitting |?m322|=2.44-0.15+0.17×10-3eV2/c4. Our result corresponds to the maximal oscillation disappearance probability.

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

2013-11-01

456

Right-handed neutrinos at CERN LHC and the mechanism of neutrino mass generation  

SciTech Connect

We consider the possibility to detect right-handed neutrinos, which are mostly singlets of the standard model gauge group, at future accelerators. Substantial mixing of these neutrinos with the active neutrinos requires a cancellation of different contributions to the light neutrino mass matrix at the level of 10{sup -8}. We discuss possible symmetries behind this cancellation and argue that for three right-handed neutrinos they always lead to conservation of total lepton number. Light neutrino masses can be generated by small perturbations violating these symmetries. In the most general case, LHC physics and the mechanism of neutrino mass generation are essentially decoupled; with additional assumptions, correlations can appear between collider observables and features of the neutrino mass matrix.

Kersten, Joern [Abdus Salam ICTP, Strada Costiera 11, 34014 Trieste (Italy); Smirnov, Alexei Yu. [Abdus Salam ICTP, Strada Costiera 11, 34014 Trieste (Italy); Institute for Nuclear Research, Russian Academy of Sciences, 60th October Anniversary Prospect 7A, 117 312 Moscow (Russian Federation)

2007-10-01

457

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 neutrino production target, collected data corresponding to 3.01×10(20) protons on target. In the absence of neutrino oscillations, 205±17 (syst) events are expected to be detected while only 58 muon neutrino event candidates are observed. A fit to the neutrino rate and energy spectrum, assuming three neutrino flavors and normal mass hierarchy yields a best-fit mixing angle sin2(?23)=0.514±0.082 and mass splitting |?m(32)(2)|=2.44(-0.15)(+0.17)×10(-3) eV2/c4. Our result corresponds to the maximal oscillation disappearance probability. PMID:24313479

Abe, K; Adam, J; Aihara, H; Akiri, T; Andreopoulos, C; Aoki, S; Ariga, A; Ariga, T; Assylbekov, S; Autiero, D; Barbi, M; Barker, G J; Barr, G; Bass, M; Batkiewicz, M; Bay, F; Bentham, S W; Berardi, V; Berger, B E; Berkman, S; Bertram, I; Bhadra, S; Blaszczyk, F D M; Blondel, A; Bojechko, C; Bordoni, S; Boyd, S B; Brailsford, D; Bravar, A; Bronner, C; Buchanan, N; Calland, R G; Caravaca Rodríguez, J; Cartwright, S L; Castillo, R; Catanesi, M G; Cervera, A; Cherdack, D; Christodoulou, G; Clifton, A; Coleman, J; Coleman, S J; Collazuol, G; Connolly, K; Cremonesi, L; Curioni, A; Dabrowska, A; Danko, I; Das, R; Davis, S; de Perio, P; De Rosa, G; Dealtry, T; Dennis, S R; Densham, C; Di Lodovico, F; Di Luise, S; Drapier, O; Duboyski, T; Duffy, K; Dufour, F; Dumarchez, J; Dytman, S; Dziewiecki, M; Emery, S; Ereditato, A; Escudero, L; Finch, A J; Frank, E; Friend, M; Fujii, Y; Fukuda, Y; Furmanski, A P; Galymov, V; Gaudin, A; Giffin, S; Giganti, C; Gilje, K; Golan, T; Gomez-Cadenas, J J; Gonin, M; Grant, N; Gudin, D; Hadley, D R; Haesler, A; Haigh, M D; Hamilton, P; Hansen, D; Hara, T; Hartz, M; Hasegawa, T; Hastings, N C; Hayato, Y; Hearty, C; Helmer, R L; Hierholzer, M; Hignight, J; Hillairet, A; Himmel, A; Hiraki, T; Hirota, S; Holeczek, J; Horikawa, S; Huang, K; Ichikawa, A K; Ieki, K; Ieva, M; Ikeda, M; Imber, J; Insler, J; Irvine, T J; Ishida, T; Ishii, T; Ives, S J; Iyogi, K; Izmaylov, A; Jacob, A; Jamieson, B; Johnson, R A; Jo, J H; Jonsson, P; Joo, K K; Jung, C K; Kaboth, A C; Kajita, T; Kakuno, H; Kameda, J; Kanazawa, Y; Karlen, D; Karpikov, I; Kearns, E; Khabibullin, M; Khotjantsev, A; Kielczewska, D; Kikawa, T; Kilinski, A; Kim, J; Kim, S B; Kisiel, J; Kitching, P; Kobayashi, T; Kogan, G; Kolaceke, A; Konaka, A; Kormos, L L; Korzenev, A; Koseki, K; Koshio, Y; Kreslo, I; Kropp, W; Kubo, H; Kudenko, Y; Kumaratunga, S; Kurjata, R