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1

Fourth standard model family neutrino at future linear colliders  

SciTech Connect

It is known that flavor democracy favors the existence of the fourth standard model (SM) family. In order to give nonzero masses for the first three-family fermions flavor democracy has to be slightly broken. A parametrization for democracy breaking, which gives the correct values for fundamental fermion masses and, at the same time, predicts quark and lepton Cabibbo-Kobayashi-Maskawa (CKM) matrices in a good agreement with the experimental data, is proposed. The pair productions of the fourth SM family Dirac ({nu}{sub 4}) and Majorana (N{sub 1}) neutrinos at future linear colliders with {radical}(s)=500 GeV, 1 TeV, and 3 TeV are considered. The cross section for the process e{sup +}e{sup -}{yields}{nu}{sub 4}{nu}{sub 4}(N{sub 1}N{sub 1}) and the branching ratios for possible decay modes of the both neutrinos are determined. The decays of the fourth family neutrinos into muon channels ({nu}{sub 4}(N{sub 1}){yields}{mu}{sup {+-}}W{sup {+-}}) provide cleanest signature at e{sup +}e{sup -} colliders. Meanwhile, in our parametrization this channel is dominant. W bosons produced in decays of the fourth family neutrinos will be seen in detector as either di-jets or isolated leptons. As an example, we consider the production of 200 GeV mass fourth family neutrinos at {radical}(s)=500 GeV linear colliders by taking into account di-muon plus four jet events as signatures.

Ciftci, A.K.; Ciftci, R.; Sultansoy, S. [Physics Department, Faculty of Sciences, Ankara University, 06100 Tandogan, Ankara (Turkey); Physics Department, Faculty of Sciences and Arts, Gazi University, 06500 Teknikokullar, Ankara (Turkey)

2005-09-01

2

Phenomenology of FourthPhenomenology of Fourth Generation NeutrinosGeneration Neutrinos  

E-print Network

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

California at Santa Cruz, University of

3

The Naturalness of the Fourth SM Family  

E-print Network

The necessity of the fourth family follows from the SM basics. According to flavor democracy the Dirac masses of the fourth SM family fermions are almost equal with preferable value 450 GeV, which corresponds to common (for all fundamental fermions) Yukawa coupling equal to SU(2) gauge coupling gW. In principle, one expect u4 a little bit lighter than d4, while nu4 could be essentially lighter than l4 due to Majorana mass terms for right-handed components of neutrinos. Obviously, the fourth family quarks will be copiously produced at the LHC. However, the first indication of the fourth SM family may be provided by early Higgs boson observation due to almost an order enhancement of the gluon fusion to Higgs cross-section. For the same reason the Tevatron still has a chance to observe the Higgs boson before the LHC. Concerning the fourth family leptons, in general, best place will be NLC/CLIC. However, for some mass regions and MNS matrix elements double discovery of both the nu4 and H could be possible at the LHC.

S. Sultansoy

2009-05-18

4

Diquarks from a fourth family  

E-print Network

If fourth family condensates are responsible for electroweak symmetry breaking then they may also break approximate global symmetries. Among the resulting pseudo-Goldstone bosons are those that can have diquark quantum numbers. We describe the variety of diquarks and their decay modes, and we find aspects that are particular to the fourth family framework. Spectacular signatures at the LHC appear and are explored for color sextet diquarks with 600 GeV mass. We consider a simple search strategy which avoids diquark reconstruction. We also consider 350 GeV mass diquarks that are accessible at the Tevatron.

Bob Holdom

2011-09-06

5

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

6

Bounding CKM Mixing with a Fourth Family  

E-print Network

CKM mixing between third family quarks and a possible fourth family is constrained by global fits to the precision electroweak data. The dominant constraint is from nondecoupling oblique corrections rather than the Zbb vertex correction used in previous analyses. The possibility of large mixing suggested by some recent analyses of FCNC processes is excluded, but 3-4 mixing of the same order as the Cabbibo mixing of the first two families is allowed.

Michael S. Chanowitz

2009-04-27

7

A New Family with a Fourth Lepton Flavour  

E-print Network

We present here arguments in favor of the existence of the most lightest lepton and its neutrino. This new family with a fourth lepton flavour in the first turn must uncover so far unobserved universal properties of matter. The unity of their laws predicts the flavour symmetrical schemes for the decays of the electron and the proton. Thereby, it admits the new modes in the decays of the muon, tau lepton and the neutron. At the same time, in all these transitions no conservation laws are violated.

Sharafiddinov, Rasulkhozha S

2012-01-01

8

A New Family with a Fourth Lepton Flavour  

E-print Network

We present here arguments in favor of the existence of the most lightest lepton and its neutrino. This new family with a fourth lepton flavour in the first turn must uncover so far unobserved universal properties of matter. The unity of their laws predicts the flavour symmetrical schemes for the decays of the electron and the proton. Thereby, it admits the new modes in the decays of the muon, tau lepton and the neutron. At the same time, in all these transitions no conservation laws are violated.

Rasulkhozha S. Sharafiddinov

2012-03-15

9

Searching for the fourth family quarks through anomalous decays  

SciTech Connect

The flavor democracy hypothesis predicts the existence of the fourth standard model family. Because of the high masses of the fourth family quarks, their anomalous decays could be dominant if certain criteria are met. This will drastically change the search strategy at hadron colliders. We show that the fourth standard model family down quarks with masses up to 400-450 GeV can be observed (or excluded) via anomalous decays by Tevatron.

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)

2010-09-01

10

Fourth International Conference on Families with Parental Mental Health Challenges  

E-print Network

Fourth International Conference on Families with Parental Mental Health Challenges Sponsored by Conference Information Online: interprofessional.ubc.ca/MentalHealth2014 Addressing the Needs of the Whole Education #12;Fourth International Conference on Families with Parental Mental Health Challenges 2 G E N E R

Michelson, David G.

11

Mass limits for fourth generation sequential neutrinos from dark matter experiments  

E-print Network

Current mass limits for fourth generation sequential neutrinos come from dark matter experiments assuming $\\rho_{DM}=0.2-0.8$ g/ cm$^3$. We show that the latest results from the CDMS II experiment exclude Dirac neutrinos with masses below 500 GeV assuming only that they are produced as expected by the Big Bang model and clump in the same manner as baryons. We also show the next generation of nuclear recoil experiments will be sensitive to fourth generation Majorana nuetrinos. Finally, we consider the case in which the neutrino interacts with the nucleus via the exchange of a Higgs boson.

Gray Rybka; Peter Fisher

2005-07-21

12

Proposed search for a fourth neutrino with a PBq antineutrino source.  

PubMed

Several observed anomalies in neutrino oscillation data can be explained by a hypothetical fourth neutrino separated from the three standard neutrinos by a squared mass difference of a few eV(2). We show that this hypothesis can be tested with a PBq (ten kilocurie scale) (144)Ce or (106)Ru antineutrino beta source deployed at the center of a large low background liquid scintillator detector. In particular, the compact size of such a source could yield an energy-dependent oscillating pattern in event spatial distribution that would unambiguously determine neutrino mass differences and mixing angles. PMID:22181722

Cribier, Michel; Fechner, Maximilien; Lasserre, Thierry; Letourneau, Alain; Lhuillier, David; Mention, Guillaume; Franco, Davide; Kornoukhov, Vasily; Schönert, Stefan

2011-11-11

13

Neutrino dark matter candidate in fourth generation scenarios  

E-print Network

We overview the constraints on the 4th-generation neutrino dark matter candidate and investigate a possible way to make it a viable dark matter candidate. Given the LEP constraints tell us that the 4th-generation neutrino has to be rather heavy (> M_Z/2), in sharp contrast to the other three neutrinos, the underlying nature of the 4th-generation neutrino is expected to be different. We suggest that an additional gauge symmetry B-4L_4 distinguishes it from the Standard Model's three lighter neutrinos and this also facilitates promotion of the 4th-generation predominantly right-handed neutrino to a good cold dark matter candidate. It provides distinguishable predictions for the dark matter direct detection and the Large Hadron Collider experiments.

Hye-Sung Lee; Zuowei Liu; Amarjit Soni

2011-09-02

14

Searches for the $t^\\prime$ of a fourth family  

E-print Network

We study the detection of the $t^\\prime$ of a fourth family during the early running of LHC with 7 TeV collision energy and 1 fb$^{-1}$ integrated luminosity. By use of a neural network we show that it is feasible to search for the $t'$ even with a mass close to the unitarity upper bound, which is in the 500 to 600 GeV range. We also present results for the Tevatron with $10 \\,\\, \\textrm{fb}^{-1}$. In both cases the search for a fourth family quark doublet can be significantly enhanced if one incorporates the contribution that the $b'$ can make to a $t'$-like signal. Thus the bound on the mass of a degenerate quark doublet should be stronger than the bounds obtained by treating $t'$ and $b'$ in isolation.

Bob Holdom; Qi-Shu Yan

2011-06-20

15

The United Families of Massive Neutrinos of the Different Nature  

E-print Network

At the availability of a non - zero mass, the same neutrino regardless of whether it refers to Dirac or Majorana fermions, must possess simultaneously each of the anapole and electric dipole moments. Their interaction with field of emission can also lead to the longitudinal polarized neutrinos elastic scattering on a spinless nucleus. Using the process cross section, the united equation has been obtained between the anapole and electric dipole form factors of Dirac and Majorana neutrinos. It corresponds in the nature to the coexistence of neutrinos of both types. As a consequence, each of Dirac neutrinos testifies in favor of the existence of a kind of the Majorana neutrino. They constitute herewith the united families of massive neutrinos of a different nature. Therefore, any of earlier measured properties of neutrinos may serve as a certain indication to the existence simultaneously both of Dirac and of Majorana neutrinos. All findings are confirmed also by the comparatively new laboratory restrictions on t...

Sharafiddinov, R S

2004-01-01

16

From the Fourth Color to Spin-charge Separation - Neutrinos and Spinons  

E-print Network

We introduce the spin-charge separation mechanism to the quark-lepton unification models which consider the lepton number as the fourth color. In certain finite-density systems, quarks and leptons are decomposed into spinons and chargons, which carry the spin and charge degrees of freedom respectively. Neutrinos can be related to the spinons with respect to the electric-charge and spin separation in the early universe or other circumstances. Some effective, probably universal couplings between the spinon sector and the chargon sector are derived and a phenomenological description for the chargon condensate is proposed. It is then demonstrated that the spinon current can induce vorticity in the chargon condensate, and spinon zero modes are trapped in the vortices, forming spinon-vortex bound states. In cosmology this configuration may lead to the emission of extremely high energy neutrinos when vortices split and reconnect.

Xiong, Chi

2015-01-01

17

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

18

The United Families of Massive Neutrinos of a Different Nature  

E-print Network

At the availability of a nonzero mass, the same neutrino regardless of whether it refers to Dirac or Majorana fermions, must possess simultaneously each of the anapole and electric dipole moments. Their interaction with the field of emission can also lead to the elastic scattering of the longitudinal polarized neutrinos on a spinless nucleus. Using the cross section of a process, the united equation has been obtained between the anapole and electric dipole form factors of Dirac and Majorana neutrinos. It corresponds in nature to the coexistence of neutrinos of both types. As a consequence, each Dirac neutrino testifies in favor of the existence of a kind of Majorana neutrino. They constitute herewith the united families of massive neutrinos of a different nature. Therefore, any of the earlier measured properties of neutrinos may serve as a certain indication of the existence simultaneously of both Dirac and Majorana neutrinos. All findings are also confirmed by the comparatively new laboratory restrictions on the self-masses of these fermions. Thereby they state that electromagnetic gauge invariance must have a new structure, which depends on nature of the inertial mass and says that P-symmetry of a particle is basically violated at the expense of its rest mass.

Rasulkhozha S. Sharafiddinov

2010-09-24

19

THE UNITED FAMILIES OF MASSIVE NEUTRINOS OF THE DIFFERENT NATURE  

E-print Network

At the availability of a non- zero mass, the same neutrino regardless of whether it refers to Dirac or Majorana fermions, must possess simultaneously each of the anapole and electric dipole moments. Their interaction with field of emission can also lead to the longitudinal polarized neutrinos elastic scattering on a spinless nucleus. Using the process cross section, the united equation has been obtained between the anapole and electric dipole form factors of Dirac and Majorana neutrinos. It corresponds in the nature to the coexistence of neutrinos of both types. As a consequence, each of Dirac neutrinos testifies in favor of the existence of a kind of the Majorana neutrino. They constitute herewith the united families of massive neutrinos of a different nature. Therefore, any of earlier measured properties of neutrinos may serve as a certain indication to the existence simultaneously both of Dirac and of Majorana neutrinos. All findings are confirmed also by the comparatively new laboratory restrictions on these fermions self masses. Thereby they state that electromagnetic gauge invariance must have a new structure

Rasulkhozha S. Sharafiddinov

2005-01-01

20

Fourth SM family, breaking of mass democracy, and the CKM mixings  

SciTech Connect

We consider the violation of the democratic mass matrix in the framework of the four-family standard model. Predictions of fourth-family fermion masses as well as quark and lepton CKM mixings are presented. Production and decay modes of new fermions are discussed. {copyright} {ital 1996 The American Physical Society.}

Atag, S.; Celikel, A.; Ciftci, A.K. [Physics Department, Faculty of Sciences, Ankara University, 06100 Tandogan-Ankara (Turkey); Sultansoy, S. [Physics Department, Faculty of Sciences, Ankara University, 06100 Tandogan-Ankara (Turkey)]|[Institute of Physics, Academy of Sciences, Baku (Azerbaijan); Yilmaz, U.O. [Physics Department, Faculty of Arts and Sciences, METU, Ankara (Turkey)

1996-11-01

21

Developing Cross-Cultural Competence: A Guide for Working with Children and Their Families. Fourth Edition  

ERIC Educational Resources Information Center

As the U.S. population grows more and more diverse, how can professionals who work with young children and families deliver the best services while honoring different customs, beliefs, and values? The answers are in the fourth edition of this bestselling textbook, fully revised to reflect nearly a decade of population changes and best practices in…

Lynch, Eleanor W., Ed.; Hanson, Marci J., Ed.

2011-01-01

22

Thinking beyond Measurement, Description and Judgment: Fourth Generation Evaluation in Family-Centered Pediatric Healthcare Organizations  

ERIC Educational Resources Information Center

Background: Although pediatric healthcare organizations have widely implemented the philosophy of family-centered care (FCC), evaluators and health professionals have not explored how to preserve the philosophy of FCC in evaluation processes. Purpose: To illustrate how fourth generation evaluation, in theory, could facilitate collaboration between…

Moreau, Katherine Ann; Clarkin, Chantalle Louise

2012-01-01

23

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

24

The United Families of Massive Neutrinos of a Different Nature  

Microsoft Academic Search

At the availability of a nonzero mass, the same neutrino regardless of whether it refers to Dirac or Majorana fermions, must possess simultaneously each of the anapole and electric dipole moments. Their interaction with the field of emission can also lead to the elastic scattering of the longitudinal polarized neutrinos on a spinless nucleus. Using the cross section of a

Rasulkhozha S. Sharafiddinov

2006-01-01

25

Neutrinos  

E-print Network

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

J. Bernabeu

2000-12-22

26

The United Families of Massive Neutrinos of a Different Nature  

Microsoft Academic Search

At the availability of a nonzero mass, the same neutrino regardless of\\u000awhether it refers to Dirac or Majorana fermions, must possess simultaneously\\u000aeach of the anapole and electric dipole moments. Their interaction with the\\u000afield of emission can also lead to the elastic scattering of the longitudinal\\u000apolarized neutrinos on a spinless nucleus. Using the cross section of a

Rasulkhozha S. Sharafiddinov

2006-01-01

27

Neutrinos  

E-print Network

This document represents the response of the Intensity Frontier Neutrino Working Group to the Snowmass charge. We summarize the current status of neutrino physics and identify many exciting future opportunities for studying the properties of neutrinos and for addressing important physics and astrophysics questions with neutrinos.

A. de Gouvea; K. Pitts; K. Scholberg; G. P. Zeller; J. Alonso; A. Bernstein; M. Bishai; S. Elliott; K. Heeger; K. Hoffman; P. Huber; L. J. Kaufman; B. Kayser; J. Link; C. Lunardini; B. Monreal; J. G. Morfin; H. Robertson; R. Tayloe; N. Tolich; K. Abazajian; T. Akiri; C. Albright; J. Asaadi; K. S Babu; A. B. Balantekin; P. Barbeau; M. Bass; A. Blake; A. Blondel; E. Blucher; N. Bowden; S. J. Brice; A. Bross; B. Carls; F. Cavanna; B. Choudhary; P. Coloma; A. Connolly; J. Conrad; M. Convery; R. L. Cooper; D. Cowen; H. da Motta; T. de Young; F. Di Lodovico; M. Diwan; Z. Djurcic; M. Dracos; S. Dodelson; Y. Efremenko; T. Ekelof; J. L. Feng; B. Fleming; J. Formaggio; A. Friedland; G. Fuller; H. Gallagher; S. Geer; M. Gilchriese; M. Goodman; D. Grant; G. Gratta; C. Hall; F. Halzen; D. Harris; M. Heffner; R. Henning; J. L. Hewett; R. Hill; A. Himmel; G. Horton-Smith; A. Karle; T. Katori; E. Kearns; S. Kettell; J. Klein; Y. Kim; Y. K. Kim; Yu. Kolomensky; M. Kordosky; Yu. Kudenko; V. A. Kudryavtsev; K. Lande; K. Lang; R. Lanza; K. Lau; H. Lee; Z. Li; B. R. Littlejohn; C. J. Lin; D. Liu; H. Liu; K. Long; W. Louis; K. B. Luk; W. Marciano; C. Mariani; M. Marshak; C. Mauger; K. T. McDonald; K. McFarland; R. McKeown; M. Messier; S. R. Mishra; U. Mosel; P. Mumm; T. Nakaya; J. K. Nelson; D. Nygren; G. D. Orebi Gann; J. Osta; O. Palamara; J. Paley; V. Papadimitriou; S. Parke; Z. Parsa; R. Patterson; A. Piepke; R. Plunkett; A. Poon; X. Qian; J. Raaf; R. Rameika; M. Ramsey-Musolf; B. Rebel; R. Roser; J. Rosner; C. Rott; G. Rybka; H. Sahoo; S. Sangiorgio; D. Schmitz; R. Shrock; M. Shaevitz; N. Smith; M. Smy; H. Sobel; P. Sorensen; A. Sousa; J. Spitz; T. Strauss; R. Svoboda; H. A. Tanaka; J. Thomas; X. Tian; R. Tschirhart; C. Tully; K. Van Bibber; R. G. Van de Water; P. Vahle; P. Vogel; C. W. Walter; D. Wark; M. Wascko; D. Webber; H. Weerts; C. White; H. White; L. Whitehead; R. J. Wilson; L. Winslow; T Wongjirad; E. Worcester; M. Yokoyama; J. Yoo; E. D. Zimmerman

2013-10-16

28

Three-family SU(5) GUT and inverted neutrino mass hierarchy  

NASA Astrophysics Data System (ADS)

Supersymmetric SU(5) GUT augmented with anomaly-free U(1)F flavor symmetry is presented. A very economical field content and U(1)F charge assignment are obtained by specific construction. In particular, three families of 10+5¯ chiral matter, along with the SU(5) singlet states (some of which serve as right-handed neutrinos) are obtained. Appealing texture zero Yukawa matrices provide a natural understanding of hierarchies between charged fermion masses and mixings. The model predicts an inverted hierarchical neutrino mass scenario with interesting implications.

Tavartkiladze, Zurab

2013-04-01

29

Higgs boson mass bounds in the presence of a heavy fourth quark family  

E-print Network

We present Higgs boson mass bounds in a lattice regularization allowing thus for non-perturbative investigations. In particular, we employ a lattice modified chiral invariant Higgs-Yukawa model using the overlap operator. We show results for the upper and lower Higgs boson mass bounds in the presence of a heavy mass-degenerate quark doublet with masses ranging up to 700 GeV. We perform infinite volume extrapolations in most cases, and examine several values of the lattice cutoff. Furthermore, we argue that the lower Higgs boson mass bound is stable with respect to the addition of higher dimensional operators to the scalar field potential. Our results have severe consequences for the phenomenology of a fourth generation of quarks if a light Higgs boson is discovered at the LHC.

John Bulava; Philipp Gerhold; Karl Jansen; Jim Kallarackal; Attila Nagy

2013-01-16

30

Lepton Family Symmetry and the Neutrino Mixing Matrix  

E-print Network

I review some of the recent progress (up to September 2005) in applying non-Abelian discrete symmetries to the family structure of leptons, with particular emphasis on the tribimaximal mixing ansatz of Harrison, Perkins, and Scott.

Ernest Ma

2006-06-01

31

Neutrinos  

PubMed Central

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

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

1999-01-01

32

Indirect search for the fourth genration of quarks and leptons  

SciTech Connect

It is known that the Standard Model (SM) does not predict the number of fermion families; N. The only restriction comes from the asymptotic freedom of QCD which requires the number of quarks to be less than 17 and, therefore, the number of SM families to be N{<=}8. Before 1990A-circumflex Ss, many authors published articles related to the extra SM families and their phenomenological consequences. In early 1990A-circumflex Ss, the LEP data yields N is almost 3 where the neutral lepton mass for each family is less than half the mass of the Z boson. Generally, this result is interpreted as the exact value of N, since one assumes that the neutrinos must have very small masses. If we disregard this incorrect assumption, the LEP data does not exclude the existence of extra SM families with heavy neutrinos. Meanwhile, few papers arguing the existence of the fourth SM family have been publishing. These arguments are based on the A-circumflex Sflavor democracyA-circumflex S hypothesis. The study of FCNC in B decays can indirectly shed light on the SM4 family in quark sector and LFV is a good candidate to indirect search for 4th generation of leptons.

Bashiry, Vali [Engineering Faculty, Cyprus International University, Via Mersin 10 (Turkey)

2008-04-21

33

Family and Community Studies (FACS) Fourth Interim Report, Phase I and Activities and Timelines for Phase II.  

ERIC Educational Resources Information Center

Discussed in this paper is a preliminary analysis of findings from data gathered during the first phase of a research project exploring the processes whereby the nature of the mother's occupation affects her family life, especially (1) her partnership in decisions about housework, child care and education and (2) the negotiation of the allocation…

Espinoza, Renato; And Others

34

Light-neutrino masses and the strong CP problem  

NASA Astrophysics Data System (ADS)

A minimal extension of the standard model is proposed to incor- porate the light-neutrino masses and the resolution of the strong CP problem. A unique light pseudo-Goldstone boson, whose coupling to the electron is 1 or 2 orders of magnitude greater than that of the conventional hadronic axion, arises from the model. The scale of Peccei-Quinn symmetry breaking is shown to be greater than 1010 GeV through its connection to the light-neutrino masses, and is further constrained if the (hypothetical) fourth family of quarks and leptons exist.

Shin, Michael

1987-11-01

35

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

36

Neutrino physics  

Microsoft Academic Search

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

E. Kh

37

Massive neutrinos and neutrino oscillations  

Microsoft Academic Search

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

S. M. Bilenky; S. T. Petcov

1987-01-01

38

Neutrino Experiments  

SciTech Connect

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

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

2010-08-04

39

The isolated fourth ventricle  

PubMed Central

Isolated enlargement of the fourth ventricle, or ‘encysted’ fourth ventricle is a rare late complication following shunt insertion of the lateral ventricles for hydrocephalus. Caudal and rostral obstruction of the fourth ventricle and its subsequent dilation results in compression of adjacent cerebellum and brain stem structures; treatment with further shunt insertion directly to the fourth ventricle is invariably successful. There is potential for diagnostic delay, when clinical symptoms and signs of cerebellar and brain stem compromise are unrecognised or attributed to other factors, and attention on the CT is focused on the lateral ventricular system and the already existing  ventriculoperitoneal shunt, which will appear unchanged from previous scans. We report two cases with isolated fourth ventricular obstruction and review the literature to highlight the importance of recognising this condition. PMID:23559656

Ali, Khalid; Nannapaneni, Ravindra; Hamandi, Khalid

2013-01-01

40

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

41

Neutrino Oscillations with Reactor Neutrinos  

E-print Network

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

Anatael Cabrera

2007-02-22

42

Neutrino Physics  

E-print Network

The fundamental properties of neutrinos are reviewed in these lectures. The first part is focused on the basic characteristics of neutrinos in the Standard Model and how neutrinos are detected. Neutrino masses and oscillations are introduced and a summary of the most important experimental results on neutrino oscillations to date is provided. Then, present and future experimental proposals are discussed, including new precision reactor and accelerator experiments. Finally, different approaches for measuring the neutrino mass and the nature (Majorana or Dirac) of neutrinos are reviewed. The detection of neutrinos from supernovae explosions and the information that this measurement can provide are also summarized at the end.

Gil-Botella, I

2013-01-01

43

Analysis of the CDHSW Neutrino Oscillation Experiment  

NASA Astrophysics Data System (ADS)

Analysis of the world's neutrino oscillation data in terms of a phenomenology that employs the three known neutrinos allows extraction of the five parameters that determine the model, three mixing angles and two mass-squared differences. However, two existing experiments, LSND and MiniBooNE do not fit within this model. These experiments lead to the suggestion that the addition of a fourth neutrino, called a sterile neutrino, might accommodate them. Two publications which use various approximations say that this suggestion does not work. The group with which I worked will do a full four neutrino analysis to further investigate this hypothesis. An additional experiment, CERN Dortmund Heidelberg Saclay Warsaw (CDHSW) will impact this investigation in the region of a larger mass-squared difference, the region where a fourth neutrino is expected to lie. I constructed a computational tool that analyzes the CDHSW experiment by calculating the probability for mu neutrinos to not oscillate in the CDHSW experiment. It was calibrated to reproduce the two-neutrino results given by the experimentalists and then will be generalized to four neutrinos. It will be used in the larger analysis which will include all of the world's data.

Mandalou, Jocelyn; Ernst, David

2010-10-01

44

Sterile neutrinos?  

E-print Network

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

S. M. Bilenky; C. Giunti

1999-05-05

45

Solar Neutrinos  

E-print Network

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

A. B. McDonald

2002-09-21

46

Fourth Graders' Literature Preferences  

Microsoft Academic Search

A regionally balanced sample of fourth graders (253 girls and 239 boys) expressed their literature preferences on a 68-item fictitious annotated titles inventory. The inventory was constructed using 26 categories of fiction and nonfiction based on Schulte's (1968) and Huck and Young's (1961) children's literature classifications. Half of each subject's survey consisted of items that he or she was to

Carol Haynes; Donald J. Richgels

1992-01-01

47

Fourth ventricle ependymomas  

Microsoft Academic Search

Summary Twenty patients with fourth ventricle ependymoma were treated surgically at our Neurosurgery Division between January 1976 und December 1990. Ependymoblastomas and mixed gliomas operated on in the same period have not been considered. A statistical analysis of our cases and a review of the largest published series show that favourable prognostic factors are: age over 16, post-operative radiotherapy to

L. Ferrante; L. Mastronardi; G. Schettini; P. Lunardi; A. Fortuna

1994-01-01

48

Neutrino physics  

SciTech Connect

The field of neutrino physics has expanded greatly in recent years with the discovery that neutrinos change flavor and therefore have mass. Although there are many neutrino physics results since the last DIS workshop, these proceedings concentrate on recent neutrino physics results that either add to or depend on the understanding of Deep Inelastic Scattering. They also describe the short and longer term future of neutrino DIS experiments.

Harris, Deborah A.; /Fermilab

2008-09-01

49

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

50

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" ...

Ms. Boissonnault

2005-06-23

51

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

52

Neutrino unification.  

PubMed

Present neutrino data are consistent with neutrino masses arising from a common seed at some "neutrino unification" scale M(X). Such a simple theoretical ansatz naturally leads to quasidegenerate neutrinos that could lie in the electron-volt range with neutrino mass splittings induced by renormalization effects associated with supersymmetric thresholds. In such a scheme the leptonic analog of the Cabibbo angle straight theta(middle dot in circle) describing solar neutrino oscillations is nearly maximal. Its exact value is correlated with the smallness of straight theta(reactor). The two leading mass-eigenstate neutrinos present in nu(e) form a pseudo-Dirac neutrino, avoiding conflict with neutrinoless double beta decay. PMID:11328005

Chankowski, P H; Ioannisian, A N; Pokorski, S; Valle, J W

2001-04-16

53

May heavy neutrinos solve underground and cosmic-ray puzzles?  

NASA Astrophysics Data System (ADS)

Primordial heavy neutrinos of the fourth generation might explain different astrophysical puzzles. The simplest fourth-neutrino scenario is consistent with known fourth-neutrino physics, cosmic ray antimatter, cosmic gamma fluxes, and positive signals in underground detectors for a very narrow neutrino mass window (46 47 GeV). However, accounting for the constraint of underground experiment CDMS prohibits solution of cosmic-ray puzzles in this scenario. We have analyzed extended heavy-neutrino models related to the clumpiness of neutrino density, new interactions in heavy-neutrino annihilation, neutrino asymmetry, and neutrino decay. We found that, in these models, the cosmic-ray imprint may fit the positive underground signals in DAMA/Nal experiment in the entire mass range 46 70 GeV allowed from uncertainties of electroweak parameters, while satisfaction of the CDMS constraint reduces the mass range to around 50 GeV, where all data can come to consent in the framework of the considered hypothesis.

Belotsky, K. M.; Fargion, D.; Khlopov, M. Yu.; Konoplich, R. V.

2008-01-01

54

Search for fourth generation neutral heavy leptons  

SciTech Connect

A search for fourth generation neutral heavy leptons ({nu}{sub 4}) in W decays was carried out the D0 detector at the Fermilab Tevatron at {radical}{bar s} = 1.8 TeV. The {nu}{sub 4} is assumed to be produced via mixing with the first generation neutrino only. We looked for a three electron final state event topology. The data used in this analysis represent 12.2 pb{sup {minus}1} taken during the 1992--1993 run. No candidates were found. We set a preliminary limit beyond the LEP limit for the considered mixing case on the {vert_bar}U{sub e4}{vert_bar}{sup 2} {minus} m{sub {nu}4} plane.

Abachi, S.; Abbott, B.; Abolins, M. [and others; D0 Collaboration

1995-07-01

55

Neutrino Detectors  

NASA Astrophysics Data System (ADS)

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

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

56

Neutrino Lensing  

E-print Network

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

Luo Xin-Lian

2009-09-28

57

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

PubMed

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

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

2014-04-01

58

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

59

Neutrino factory  

NASA Astrophysics Data System (ADS)

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

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

2014-12-01

60

Solar neutrinos before and after Neutrino 2004  

Microsoft Academic Search

We compare, using a three neutrino analysis, the allowed neutrino oscillation parameters and solar neutrino ?uxes determined by the experimental data available Before and After Neutrino 2004. New data available after Neutrino 2004 include reflned Kam- LAND and gallium measurements. We use six difierent approaches to analyzing the Kam- LAND data. We present detailed results using all the available neutrino

John N. Bahcall; Maria C. Gonzalez-Garciabc; C. N. Yang

61

Quark masses and mixing angles in a four-generation model with a naturally heavy neutrino  

SciTech Connect

It is argued with the help of an illustrative model with some interesting predictions that the interspecies hierarchy among the fermion masses and the quark mixing angles can be accommodated naturally in the standard model with approximately equal Yukawa couplings for all the fermions, provided there are four sequential quark-lepton families with all members of the fourth family having roughly equal masses. The special problem of very light neutrino masses (if any) and possible solutions are also discussed. In the quark sector, the model is shown to be consistent with the observed neutral meson mixing data and has a few interesting predictions. It is also shown that the existence of precisely four generations is strongly favored within a wide class of models with a few very reasonable assumptions about naturalness.

Datta, A. (Department of Physics, Jadavpur University, Calcutta 700 032 (India)); Raychaudhuri, S. (Department of Pure Physics, University of Calcutta, 92 Acharya Prafulla Chandra Road, Calcutta 700 009 (India))

1994-05-01

62

Atmospheric neutrinos and discovery of neutrino oscillations  

PubMed Central

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

Kajita, Takaaki

2010-01-01

63

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.

64

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

65

Solar Neutrinos Before and After Neutrino 2004  

Microsoft Academic Search

We compare, using a three neutrino analysis, the allowed neutrino oscillation parameters and solar neutrino fluxes determined by the experimental data available Before and After Neutrino 2004. New data available after Neutrino 2004 include refined KamLAND and gallium measurements. We use six different approaches to analyzing the KamLAND data. We present detailed results using all the available neutrino and anti-neutrino

John N. Bahcall; Maria C. Gonzalez-Garcia; Carlos Pena-Garay

2004-01-01

66

Understanding the Fourth-Grade Slump: Our Point of View  

ERIC Educational Resources Information Center

Educators know that an achievement gap exists between students of low-income and middle-income families, a gap that is especially evident in fourth grade and beyond. This essay explores issues related to this gap, including primary-level children being immersed in narrative text and, therefore, unprepared for the challenges of informational text…

Sanacore, Joseph; Palumbo, Anthony

2009-01-01

67

Unveiling neutrino mixing and leptonic CP violation  

SciTech Connect

We review the present understanding of neutrino masses and mixings, discussing what are the unknowns in the three family oscillation scenario. Despite the anticipated success coming from the planned long baseline neutrino experiments in unraveling the leptonic mixing sector, there are two important unknowns which may remain obscure: the mixing angle {theta}{sub 13} and the CP-phase {delta}. The measurement of these two parameters has led us to consider the combination of superbeams and neutrino factories as the key to unveil the neutrino oscillation picture.

Mena, Olga; /Fermilab

2005-01-01

68

Fourth World Conference On Women  

NSDL National Science Digital Library

The Fourth World Conference On Women (4-15 September, Beijing, China) Web page offers general news, late breaking news, background information and more, updated daily. In French and English. Also available via gopher.

69

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

70

Neutrino and Extra World  

E-print Network

The neutrino speed measurement experiments are the continuations of the classic light speed measurement experiments have been done in range of the solar planet system (Ole Roemer, 1676), in star system (James Braidely, 1728) and, at last, on the Earth (Lois Fizeau, 1849),.... The finite light speed measurement has led to the revolution in the humanity consciousness and eventually led to a new understanding of the visible universe. In 1998-2005, we had a lot of excited discussions at CERN about the possibilities to perform the neutrino experiments to test the superluminal neutrino hypothesis and to find new phenomena beyond the SM. From one hand the idea of such experiments was associated with the hope to understand the role of the V-A- weak interactions, the quark-lepton family symmetry, the neutrino space-time properties and to observe some indications on a new vacuum structure existence outside of the Weak Scale, i.e. in the region 1/R ~ (0.1-20) TeV. From another hand the general trends of this idea has be...

Baranov, D S

2012-01-01

71

Ultrahigh Energy Tau Neutrinos  

E-print Network

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

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

2005-07-30

72

Phenomenology of neutrino oscillations  

Microsoft Academic Search

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

W. Grimus; C. Giunti

1999-01-01

73

Is cosmology compatible with sterile neutrinos?  

SciTech Connect

By combining data from cosmic microwave background (CMB) experiments (including the recent BOOMERANG-2K2 results), large scale structure (LSS) and Lyman-{alpha} forest observations, we constrain the hypothesis of a fourth, sterile, massive neutrino. For the 3 massless + 1 massive neutrino case we bound the mass of the sterile neutrino to m{sub s} < 0.55eV at 95% c.l.. These results exclude at high significance the sterile neutrino hypothesis as an explanation of the LSND anomaly. We then generalize the analysis to account for active neutrino masses (which tightens the limit to m{sub s} < 0.51eV) and the possibility that the sterile abundance is not thermal. In the latter case, the constraints in the (mass, density) plane are non-trivial. For a mass of > 1eV or < 0.05eV the cosmological energy density in sterile neutrinos is always constrained to be {omega}{sub {nu}} < 0.005 at 95% c.l.. However, for a sterile neutrino mass of {approx} 0.25 eV, {omega}{sub {nu}} can be as large as 0.015.

Dodelson, Scott; /Fermilab; Melchiorri, Alessandro; /Rome U. /INFN, Rome; Slosar, Anze; /Ljubljana U.

2005-11-01

74

Fourth sound of holographic superfluids  

E-print Network

We compute fourth sound for superfluids dual to a charged scalar and a gauge field in an AdS_4 background. For holographic superfluids with condensates that have a large scaling dimension (greater than approximately two), we find that fourth sound approaches first sound at low temperatures. For condensates that a have a small scaling dimension it exhibits non-conformal behavior at low temperatures which may be tied to the non-conformal behavior of the order parameter of the superfluid. We show that by introducing an appropriate scalar potential, conformal invariance can be enforced at low temperatures.

Amos Yarom

2009-05-08

75

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

76

227THE FOURTH PARADIGM Conclusions  

E-print Network

the metadata) and support integration with published literature. We believe that these challenges computing in this age of the Fourth Paradigm is a need for scientists and computer scientists to work the emergence of a global digital research library containing both the research literature and the research data

Narasayya, Vivek

77

Solar Neutrinos and the Decaying Neutrino Hypothesis  

E-print Network

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

Jeffrey M. Berryman; Andre de Gouvea; Daniel Hernandez

2014-11-02

78

Solar Neutrinos  

E-print Network

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

R. G. H. Robertson

2006-02-05

79

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

80

Overexpression, purification, crystallization and preliminary X-ray characterization of the fourth scaffoldin A cohesin from Acetivibrio cellulolyticus in complex with a dockerin from a family 5 glycoside hydrolase.  

PubMed

Cellulosomes are cell-bound multienzyme complexes secreted by anaerobic bacteria that play a crucial role in carbon turnover by degrading plant cell walls to simple sugars. Integration of cellulosomal components occurs via highly ordered protein-protein interactions between cohesin modules located in a molecular scaffold and dockerin modules found in cellulosomal enzymes. Acetivibrio cellulolyticus possesses a complex cellulosome arrangement which is organized by a primary enzyme-binding scaffoldin (ScaA), two anchoring scaffoldins (ScaC and ScaD) and an unusual adaptor scaffoldin (ScaB). A dockerin from a family 5 glycoside hydrolase (GH5), which was engineered to inactivate one of the two putative cohesin-binding interfaces, complexed with one of the ScaA cohesins from A. cellulolyticus has been purified and crystallized, and data were processed to a resolution of 1.57?Å in the orthorhombic space group P212121. PMID:25084383

Bule, Pedro; Correia, Ana; Cameron, Kate; Alves, Victor D; Cardoso, Vânia; Fontes, Carlos M G A; Najmudin, Shabir

2014-08-01

81

Light sterile neutrinos in particle physics: Experimental status  

NASA Astrophysics Data System (ADS)

Most of the neutrino oscillation results can be explained by the three-neutrino paradigm. However several anomalies in short baseline oscillation data, corresponding to an L/E of about 1 m/MeV, could be interpreted by invoking a hypothetical fourth neutrino. This new state would be separated from the three standard neutrinos by a squared mass difference ?mnew2 ˜ 0.1 - 1eV2 and would have mixing angles of sin2 2?ee ? 0.01 and sin2 2??e ? 0.001, in the electron disappearance and appearance channels, respectively. This new neutrino, often called sterile, would not feel standard model interactions but mix with the others. Such a scenario calling for new physics beyond the standard model has to be either ruled out or confirmed with new data. After a brief review of the anomalous oscillation results we discuss the forthcoming laboratory experiments aiming to clarify the situation.

Lasserre, Thierry

2014-09-01

82

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

83

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

84

Nefarious Neutrinos Alex George  

E-print Network

Nefarious Neutrinos Alex George University of Pittsburgh Nefarious Neutrinos Alex George University of Pittsburgh #12;Introduction · My research is conducted through the Neutrino Group at Pitt · Neutrino physics is a sub physics (particle lepton Introduction My research is conducted through the Neutrino physics

Fygenson, Deborah Kuchnir

85

Neutrinos and Symmetries  

E-print Network

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

A. B. Balantekin

2009-10-09

86

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

87

Neutrino and Extra World  

E-print Network

The neutrino speed measurement experiments are the continuations of the classic light speed measurement experiments have been done in range of the solar planet system (Ole Roemer, 1676), in star system (James Braidely, 1728) and, at last, on the Earth (Lois Fizeau, 1849),.... The finite light speed measurement has led to the revolution in the humanity consciousness and eventually led to a new understanding of the visible universe. In 1998-2005, we had a lot of excited discussions at CERN about the possibilities to perform the neutrino experiments to test the superluminal neutrino hypothesis and to find new phenomena beyond the SM. From one hand the idea of such experiments was associated with the hope to understand the role of the V-A- weak interactions, the quark-lepton family symmetry, the neutrino space-time properties and to observe some indications on a new vacuum structure existence outside of the Weak Scale, i.e. in the region 1/R ~ (0.1-20) TeV. From another hand the general trends of this idea has been related to the possible existence some extra space-time noncompact dimensions of the universe. In this context it would be first serious encounter with the dual conception between the physical phenomena of microcosmos and of universe. One of the main goals is to find some new space-time peculiarities and structures that might explain the formation of our visible D=(3+1)-universe with all its space-time and internal symmetries which could be only a part of a vast Universe filled with other kinds of matter. The main difficulties of such experiments related to the possible relativity principle paradoxes have been discussed.

D. S. Baranov; G. G. Volkov

2012-11-20

88

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

89

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

90

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

91

Electromagnetic properties of neutrinos  

E-print Network

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

Carlo Giunti; Alexander Studenikin

2010-06-08

92

Neutrinos: Theory and Phenomenology  

SciTech Connect

The theory and phenomenology of neutrinos will be addressed, especially that relating to the observation of neutrino flavor transformations. The current status and implications for future experiments will be discussed with special emphasis on the experiments that will determine the neutrino mass ordering, the dominant flavor content of the neutrino mass eigenstate with the smallest electron neutrino content and the size of CP violation in the neutrino sector. Beyond the neutrino Standard Model, the evidence for and a possible definitive experiment to confirm or refute the existence of light sterile neutrinos will be briefly discussed.

Parke, Stephen

2013-10-22

93

Fourth-order 2N-storage Runge-Kutta schemes  

NASA Technical Reports Server (NTRS)

A family of five-stage fourth-order Runge-Kutta schemes is derived; these schemes required only two storage locations. A particular scheme is identified that has desirable efficiency characteristics for hyperbolic and parabolic initial (boundary) value problems. This scheme is competitive with the classical fourth-order method (high-storage) and is considerably more efficient and accurate than existing third-order low-storage schemes.

Carpenter, Mark H.; Kennedy, Christopher A.

1994-01-01

94

The Intermediate Neutrino Program  

E-print Network

The US neutrino community gathered at the Workshop on the Intermediate Neutrino Program (WINP) at Brookhaven National Laboratory February 4-6, 2015 to explore opportunities in neutrino physics over the next five to ten years. Scientists from particle, astroparticle and nuclear physics participated in the workshop. The workshop examined promising opportunities for neutrino physics in the intermediate term, including possible new small to mid-scale experiments, US contributions to large experiments, upgrades to existing experiments, R&D plans and theory. The workshop was organized into two sets of parallel working group sessions, divided by physics topics and technology. Physics working groups covered topics on Sterile Neutrinos, Neutrino Mixing, Neutrino Interactions, Neutrino Properties and Astrophysical Neutrinos. Technology sessions were organized into Theory, Short-Baseline Accelerator Neutrinos, Reactor Neutrinos, Detector R&D and Source, Cyclotron and Meson Decay at Rest sessions.This report summarizes discussion and conclusions from the workshop.

C. Adams; J. R. Alonso; A. M. Ankowski; J. A. Asaadi; J. Ashenfelter; S. N. Axani; K. Babu; C. Backhouse; H. R. Band; P. S. Barbeau; N. Barros; A. Bernstein; M. Betancourt; M. Bishai; E. Blucher; J. Bouffard; N. Bowden; S. Brice; C. Bryan; L. Camilleri; J. Cao; J. Carlson; R. E. Carr; A. Chatterjee; M. Chen; S. Chen; M. Chiu; E. D. Church; J. I. Collar; G. Collin; J. M. Conrad; M. R. Convery; R. L. Cooper; D. Cowen; H. Davoudiasl; A. De Gouvea; D. J. Dean; G. Deichert; F. Descamps; T. DeYoung; M. V. Diwan; Z. Djurcic; M. J. Dolinski; J. Dolph; B. Donnelly; D. A. Dwyer; S. Dytman; Y. Efremenko; L. L. Everett; A. Fava; E. Figueroa-Feliciano; B. Fleming; A. Friedland; B. K. Fujikawa; T. K. Gaisser; M. Galeazzi; D. C. Galehouse; A. Galindo-Uribarri; G. T. Garvey; S. Gautam; K. E. Gilje; M. Gonzalez-Garcia; M. C. Goodman; H. Gordon; E. Gramellini; M. P. Green; A. Guglielmi; R. W. Hackenburg; A. Hackenburg; F. Halzen; K. Han; S. Hans; D. Harris; K. M. Heeger; M. Herman; R. Hill; A. Holin; P. Huber; D. E. Jaffe; R. A. Johnson; J. Joshi; G. Karagiorgi; L. J. Kaufman; B. Kayser; S. H. Kettell; B. J. Kirby; J. R. Klein; Yu. G. Kolomensky; R. M. Kriske; C. E. Lane; T. J. Langford; A. Lankford; K. Lau; J. G. Learned; J. Ling; J. M. Link; D. Lissauer; L. Littenberg; B. R. Littlejohn; S. Lockwitz; M. Lokajicek; W. C. Louis; K. Luk; J. Lykken; W. J. Marciano; J. Maricic; D. M. Markoff; D. A. Martinez Caicedo; C. Mauger; K. Mavrokoridis; E. McCluskey; D. McKeen; R. McKeown; G. Mills; I. Mocioiu; B. Monreal; M. R. Mooney; J. G. Morfin; P. Mumm; J. Napolitano; R. Neilson; J. K. Nelson; M. Nessi; D. Norcini; F. Nova; D. R. Nygren; G. D. Orebi Gann; O. Palamara; Z. Parsa; R. Patterson; P. Paul; A. Pocar; X. Qian; J. L. Raaf; R. Rameika; G. Ranucci; H. Ray; D. Reyna; G. C. Rich; P. Rodrigues; E. Romero Romero; R. Rosero; S. D. Rountree; B. Rybolt; M. C. Sanchez; G. Santucci; D. Schmitz; K. Scholberg; D. Seckel; M. Shaevitz; R. Shrock; M. B. Smy; M. Soderberg; A. Sonzogni; A. B. Sousa; J. Spitz; J. M. St. John; J. Stewart; J. B. Strait; G. Sullivan; R. Svoboda; A. M. Szelc; R. Tayloe; M. A. Thomson; M. Toups; A. Vacheret; M. Vagins; R. G. Van de Water; R. B. Vogelaar; M. Weber; W. Weng; M. Wetstein; C. White; B. R. White; L. Whitehead; D. W. Whittington; M. J. Wilking; R. J. Wilson; P. Wilson; D. Winklehner; D. R. Winn; E. Worcester; L. Yang; M. Yeh; Z. W. Yokley; J. Yoo; B. Yu; J. Yu; C. Zhang

2015-03-23

95

The Intermediate Neutrino Program  

E-print Network

The US neutrino community gathered at the Workshop on the Intermediate Neutrino Program (WINP) at Brookhaven National Laboratory February 4-6, 2015 to explore opportunities in neutrino physics over the next five to ten years. Scientists from particle, astroparticle and nuclear physics participated in the workshop. The workshop examined promising opportunities for neutrino physics in the intermediate term, including possible new small to mid-scale experiments, US contributions to large experiments, upgrades to existing experiments, R&D plans and theory. The workshop was organized into two sets of parallel working group sessions, divided by physics topics and technology. Physics working groups covered topics on Sterile Neutrinos, Neutrino Mixing, Neutrino Interactions, Neutrino Properties and Astrophysical Neutrinos. Technology sessions were organized into Theory, Short-Baseline Accelerator Neutrinos, Reactor Neutrinos, Detector R&D and Source, Cyclotron and Meson Decay at Rest sessions.This report summ...

Adams, C; Ankowski, A M; Asaadi, J A; Ashenfelter, J; Axani, S N; Babu, K; Backhouse, C; Band, H R; Barbeau, P S; Barros, N; Bernstein, A; Betancourt, M; Bishai, M; Blucher, E; Bouffard, J; Bowden, N; Brice, S; Bryan, C; Camilleri, L; Cao, J; Carlson, J; Carr, R E; Chatterjee, A; Chen, M; Chen, S; Chiu, M; Church, E D; Collar, J I; Collin, G; Conrad, J M; Convery, M R; Cooper, R L; Cowen, D; Davoudiasl, H; De Gouvea, A; Dean, D J; Deichert, G; Descamps, F; DeYoung, T; Diwan, M V; Djurcic, Z; Dolinski, M J; Dolph, J; Donnelly, B; Dwyer, D A; Dytman, S; Efremenko, Y; Everett, L L; Fava, A; Figueroa-Feliciano, E; Fleming, B; Friedland, A; Fujikawa, B K; Gaisser, T K; Galeazzi, M; Galehouse, D C; Galindo-Uribarri, A; Garvey, G T; Gautam, S; Gilje, K E; Gonzalez-Garcia, M; Goodman, M C; Gordon, H; Gramellini, E; Green, M P; Guglielmi, A; Hackenburg, R W; Hackenburg, A; Halzen, F; Han, K; Hans, S; Harris, D; Heeger, K M; Herman, M; Hill, R; Holin, A; Huber, P; Jaffe, D E; Johnson, R A; Joshi, J; Karagiorgi, G; Kaufman, L J; Kayser, B; Kettell, S H; Kirby, B J; Klein, J R; Kolomensky, Yu G; Kriske, R M; Lane, C E; Langford, T J; Lankford, A; Lau, K; Learned, J G; Ling, J; Link, J M; Lissauer, D; Littenberg, L; Littlejohn, B R; Lockwitz, S; Lokajicek, M; Louis, W C; Luk, K; Lykken, J; Marciano, W J; Maricic, J; Markoff, D M; Caicedo, D A Martinez; Mauger, C; Mavrokoridis, K; McCluskey, E; McKeen, D; McKeown, R; Mills, G; Mocioiu, I; Monreal, B; Mooney, M R; Morfin, J G; Mumm, P; Napolitano, J; Neilson, R; Nelson, J K; Nessi, M; Norcini, D; Nova, F; Nygren, D R; Gann, G D Orebi; Palamara, O; Parsa, Z; Patterson, R; Paul, P; Pocar, A; Qian, X; Raaf, J L; Rameika, R; Ranucci, G; Ray, H; Reyna, D; Rich, G C; Rodrigues, P; Romero, E Romero; Rosero, R; Rountree, S D; Rybolt, B; Sanchez, M C; Santucci, G; Schmitz, D; Scholberg, K; Seckel, D; Shaevitz, M; Shrock, R; Smy, M B; Soderberg, M; Sonzogni, A; Sousa, A B; Spitz, J; John, J M St; Stewart, J; Strait, J B; Sullivan, G; Svoboda, R; Szelc, A M; Tayloe, R; Thomson, M A; Toups, M; Vacheret, A; Vagins, M; Van de Water, R G; Vogelaar, R B; Weber, M; Weng, W; Wetstein, M; White, C; White, B R; Whitehead, L; Whittington, D W; Wilking, M J; Wilson, R J; Wilson, P; Winklehner, D; Winn, D R; Worcester, E; Yang, L; Yeh, M; Yokley, Z W; Yoo, J; Yu, B; Yu, J; Zhang, C

2015-01-01

96

The Intermediate Neutrino Program  

E-print Network

The US neutrino community gathered at the Workshop on the Intermediate Neutrino Program (WINP) at Brookhaven National Laboratory February 4-6, 2015 to explore opportunities in neutrino physics over the next five to ten years. Scientists from particle, astroparticle and nuclear physics participated in the workshop. The workshop examined promising opportunities for neutrino physics in the intermediate term, including possible new small to mid-scale experiments, US contributions to large experiments, upgrades to existing experiments, R&D plans and theory. The workshop was organized into two sets of parallel working group sessions, divided by physics topics and technology. Physics working groups covered topics on Sterile Neutrinos, Neutrino Mixing, Neutrino Interactions, Neutrino Properties and Astrophysical Neutrinos. Technology sessions were organized into Theory, Short-Baseline Accelerator Neutrinos, Reactor Neutrinos, Detector R&D and Source, Cyclotron and Meson Decay at Rest sessions.This report summarizes discussion and conclusions from the workshop.

C. Adams; J. R. Alonso; A. M. Ankowski; J. A. Asaadi; J. Ashenfelter; S. N. Axani; K. Babu; C. Backhouse; H. R. Band; P. S. Barbeau; N. Barros; A. Bernstein; M. Betancourt; M. Bishai; E. Blucher; J. Bouffard; N. Bowden; S. Brice; C. Bryan; L. Camilleri; J. Cao; J. Carlson; R. E. Carr; A. Chatterjee; M. Chen; S. Chen; M. Chiu; E. D. Church; J. I. Collar; G. Collin; J. M. Conrad; M. R. Convery; R. L. Cooper; D. Cowen; H. Davoudiasl; A. De Gouvea; D. J. Dean; G. Deichert; F. Descamps; T. DeYoung; M. V. Diwan; Z. Djurcic; M. J. Dolinski; J. Dolph; B. Donnelly; D. A. Dwyer; S. Dytman; Y. Efremenko; L. L. Everett; A. Fava; E. Figueroa-Feliciano; B. Fleming; A. Friedland; B. K. Fujikawa; T. K. Gaisser; M. Galeazzi; D. C. Galehouse; A. Galindo-Uribarri; G. T. Garvey; S. Gautam; K. E. Gilje; M. Gonzalez-Garcia; M. C. Goodman; H. Gordon; E. Gramellini; M. P. Green; A. Guglielmi; R. W. Hackenburg; A. Hackenburg; F. Halzen; K. Han; S. Hans; D. Harris; K. M. Heeger; M. Herman; R. Hill; A. Holin; P. Huber; D. E. Jaffe; R. A. Johnson; J. Joshi; G. Karagiorgi; L. J. Kaufman; B. Kayser; S. H. Kettell; B. J. Kirby; J. R. Klein; Yu. G. Kolomensky; R. M. Kriske; C. E. Lane; T. J. Langford; A. Lankford; K. Lau; J. G. Learned; J. Ling; J. M. Link; D. Lissauer; L. Littenberg; B. R. Littlejohn; S. Lockwitz; M. Lokajicek; W. C. Louis; K. Luk; J. Lykken; W. J. Marciano; J. Maricic; D. M. Markoff; D. A. Martinez Caicedo; C. Mauger; K. Mavrokoridis; E. McCluskey; D. McKeen; R. McKeown; G. Mills; I. Mocioiu; B. Monreal; M. R. Mooney; J. G. Morfin; P. Mumm; J. Napolitano; R. Neilson; J. K. Nelson; M. Nessi; D. Norcini; F. Nova; D. R. Nygren; G. D. Orebi Gann; O. Palamara; Z. Parsa; R. Patterson; P. Paul; A. Pocar; X. Qian; J. L. Raaf; R. Rameika; G. Ranucci; H. Ray; D. Reyna; G. C. Rich; P. Rodrigues; E. Romero Romero; R. Rosero; S. D. Rountree; B. Rybolt; M. C. Sanchez; G. Santucci; D. Schmitz; K. Scholberg; D. Seckel; M. Shaevitz; R. Shrock; M. B. Smy; M. Soderberg; A. Sonzogni; A. B. Sousa; J. Spitz; J. M. St. John; J. Stewart; J. B. Strait; G. Sullivan; R. Svoboda; A. M. Szelc; R. Tayloe; M. A. Thomson; M. Toups; A. Vacheret; M. Vagins; R. G. Van de Water; R. B. Vogelaar; M. Weber; W. Weng; M. Wetstein; C. White; B. R. White; L. Whitehead; D. W. Whittington; M. J. Wilking; R. J. Wilson; P. Wilson; D. Winklehner; D. R. Winn; E. Worcester; L. Yang; M. Yeh; Z. W. Yokley; J. Yoo; B. Yu; J. Yu; C. Zhang

2015-04-01

97

Ultra High Energy Neutrino Astronomy  

E-print Network

The short review of theoretical aspects of ultra high energy (UHE) neutrinos and superGZK neutrinos. The sources and diffuse fluxes of UHE neutrinos are discussed. Much attention is given to comparison of the cascade and cosmic ray upper bounds for diffuse neutrino fluxes. Cosmogenic neutrinos and neutrinos from the mirror mater are considered as superGZK neutrinos.

V. Berezinsky

2005-05-11

98

The Family Problem  

E-print Network

We all know that in our family of particle physics we have three generations but still don't know why - the so-called "family problem". On other hand, in view of the masses and oscillations, the neutrinos now present some basic difficulty in the Standard Model. In this note, I propose that on top of the SU_c(3) \\times SU(2) \\times U(1) standard model there is an SU_f (3) extension - a simple SU_c(3) \\times SU(2) \\times U(1) \\times SU_f (3) extended standard model. The family gauge bosons (familons) are massive through the so-called "colored" Higgs mechanism while the remaining Higgs particles are also massive. The three neutrinos, the electron-like, muon-like, and tao-like neutrinos, form the basic family triplets. Hopefully all the couplings to the "visible" matter are through the neutrinos, explaining why dark matter (25 %) is more than visible matter (5 %) in our Universe.

W-Y. Pauchy Hwang

2008-08-15

99

Muons and Neutrinos 2007  

E-print Network

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

Thomas K. Gaisser

2008-01-29

100

Neutrino oscillations in matter  

Microsoft Academic Search

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

L. Wolfenstein

1978-01-01

101

Underground neutrino astronomy  

SciTech Connect

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

Schramm, D.N.

1983-02-01

102

The history of neutrinos, 1930-1985. What have we learned about neutrinos? What have we learned using neutrinos?  

SciTech Connect

An attempt to remember some of the main events which highlight the evolution of our knowledge of the neutrinos and their properties, the 'families' of particles, a few of the very interesting persons who contributed to this progress, as well as the contribution of neutrino beam experiments to the validation of the electro-weak and quantum-chromo-dynamic theories, and the structure of the nucleon. - Highlights: Black-Right-Pointing-Pointer Early history: continuity of {beta}-spectrum, Pauli letter, universal Fermi interaction. Black-Right-Pointing-Pointer Neutrino beams and the discovery of the muon neutrino. Black-Right-Pointing-Pointer Gargamelle, the discovery of the neutral current and the verification of the quark-gluon nature of the parton. Black-Right-Pointing-Pointer Deep inelastic scattering at higher energies: scaling, quantitative verification of QCD, structure functions.

Steinberger, J., E-mail: jack.steinberger@cern.ch

2012-12-15

103

Neutrinos in Nuclear Physics  

E-print Network

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

R. D. McKeown

2014-12-03

104

Measuring Atmospheric Neutrino Oscillations with Neutrino Telescopes  

E-print Network

Neutrino telescopes with large detection volumes can demonstrate that the current indications of neutrino oscillation are correct or if a better description can be achieved with non-standard alternatives. Observations of contained muons produced by atmospheric neutrinos can better constrain the allowed region for oscillations or determine the relevant parameters of non-standard models. We analyze the possibility of neutrino telescopes measuring atmospheric neutrino oscillations. We suggest adjustments to improve this potential. An addition of four densely-instrumented strings to the AMANDA II detector makes observations feasible. Such a configuration is competitive with current and proposed experiments.

Ivone F. M. Albuquerque; George F. Smoot

2001-03-28

105

Measuring atmospheric neutrino oscillations with neutrino telescopes  

SciTech Connect

Neutrino telescopes with large detection volumes can demonstrate whether the current indications of neutrino oscillation are correct or if a better description can be achieved with nonstandard alternatives. Observations of contained muons produced by atmospheric neutrinos can better constrain the allowed region for oscillations or determine the relevant parameters of nonstandard models. We analyze the possibility of neutrino telescopes measuring atmospheric neutrino oscillations. We suggest adjustments to improve this potential. An addition of four densely instrumented strings to the AMANDA II detector makes oscillation observations feasible. Such a configuration is competitive with current and proposed experiments.

Albuquerque, Ivone F. M.; Smoot, George F.

2001-09-01

106

Supernova neutrinos  

SciTech Connect

Results are presented from a series of general relativistic stellar evolution calculations of the first 20 s in the lives of young neutron stars born in Type II supernovae. The study focuses on neutrino emissions from these protoneutron stars as they neutronize and cool. It is found that the central object in SN 1987A has a baryon mass between 1.2 and 1.7 solar mass and a best-fit gravitational mass between 1.3 and 1.5 solar masses. Also, simulations of stellar mass black hole formation by accretion onto protoneutron star intermediaries are presented. 61 references.

Burrows, A.

1988-11-01

107

Third ventriculostomy and fourth ventricle outlets obstruction.  

PubMed

A dilated fourth ventricle due to outlet obstruction is a clinical-radiologic entity with symptoms similar to those of a posterior fossa space-occupying lesion. Indeed, blockage of the foramina of Luschka and Magendie and of the aqueduct results in a "trapped" fourth ventricle. Continued cerebrospinal fluid (CSF) production within the fourth ventricle leads to cystic dilatation of the fourth ventricle. We could not, until now, understand the phenomenon, mainly on exploring endoscopically the permeability of the whole aqueduct. In adults, we call this condition the functional trapped fourth ventricle because in none of our cases have we found physical obstruction of CSF flow. Third ventricle-fourth ventriculostomy is by far the most frequently used technique for cannulation of the aqueduct in a trapped fourth ventricle. In our reported cases, we have introduced a silicone tube stent from below after accessing the fourth ventricle through a small suboccipital craniectomy, ascending it on the aqueduct in order to reach the third ventricle. Management of this infrequently isolated fourth ventricle, but communicated with the rest of ventricular system, remains a challenge for neurosurgeons. Lack of knowledge of the pathophysiology makes it difficult to treat a problem that we do not understand. PMID:22381846

Ferrer, Enrique; de Notaris, Matteo

2013-02-01

108

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

109

A spherical collapse solution with neutrino outflow  

SciTech Connect

A three-parameter family of solutions of Einstein's field equations is given that represents a collapsing perfect fluid with outgoing neutrino flux. Solutions with naked'' singularities are exhibited. They can be forbidden by requiring pressure less than or equal to the density as a condition of cosmic censorship.

Glass, E.N. (Physics Department, University of Windsor, Windsor, Ontario N9B 3P4 (Canada))

1990-08-01

110

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

111

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

112

Aging without agency: Theorizing the fourth age  

Microsoft Academic Search

This article looks at the “fourth age” as a manifestation of the fragmentation of “old age”. We argue that the fourth age emerges from the institutionalization of the infirmities of old age set against the appearance of a third-age culture that negates past representations of old age. We outline the historical marginalization of old age from early modern society to

Chris Gilleard; P. Higgs

2010-01-01

113

Informants and the Fourth Amendment: A Reconsideration  

Microsoft Academic Search

This Article argues that the Court's current interpretation of the Fourth Amendment, which sanctions the government's authority to insert secret spies and informants into our lives, is misguided. Part I highlights the historical background of the Fourth Amendment to show why its procedural safeguards are relevant when considering whether the government should be free of constitutional restraint when deploying informants

Tracey Maclin

1996-01-01

114

Academic Skills Problems. Fourth Edition Workbook  

ERIC Educational Resources Information Center

An ideal companion to "Academic Skills Problems, Fourth Edition", this indispensable workbook provides practice exercises and reproducible forms for use in direct assessment and intervention. Updated to reflect the changes in the fourth edition of the text, the workbook includes teacher and student interview forms, a complete guide to using the…

Shapiro, Edward S.

2010-01-01

115

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

116

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

117

Solar Neutrinos: History  

NSDL National Science Digital Library

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

Bahcall, John

118

Fourth order spatial derivative gravity  

SciTech Connect

In this work, we study a modified theory of gravity that contains up to fourth order spatial derivatives as a model for the Horava-Lifshitz gravity. The propagator is evaluated and, as a result, one extra pole is obtained, corresponding to a spin-2 nonrelativistic massless particle, an extra term which jeopardizes renormalizability, besides the unexpected general relativity unmodified propagator. Then unitarity is proved at the tree level, where the general relativity pole has been shown to have no dynamics, remaining only the 2 degrees of freedom of the new pole. Next, the nonrelativistic effective potential is determined from a scattering process of two identical massive gravitationally interacting bosons. In this limit, Newton's potential is obtained, together with a Darwin-like term that comes from the extra nonpole term in the propagator. Regarding renormalizability, this extra term may be harmful by power counting, but it can be eliminated by adjusting the free parameters of the model. This adjustment is in accord with the detailed balance condition suggested in the literature and shows that the way in which extra spatial derivative terms are added is of fundamental importance.

Bemfica, F. S.; Gomes, M. [Instituto de Fisica, Universidade de Sao Paulo Caixa Postal 66318, 05315-970, Sao Paulo, SP (Brazil)

2011-10-15

119

New development in radiative neutrino mass generation  

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 with a family-dependent Z4 symmetry acting on the leptons. 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 non-standard neutral Higgs bosons, if they are moderately heavy, decay significantly 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.

Julio

2014-10-01

120

Astroparticle physics with solar neutrinos  

PubMed Central

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

NAKAHATA, Masayuki

2011-01-01

121

Introduction to sterile neutrinos  

E-print Network

Model-building issues raised by the prospect of light sterile neutrinos are discussed in a pedagogical way. I first review the na\\"{\\i}ve proposal that sterile neutrinos be identified with ``right handed neutrinos''. A critical discussion of the simple expedient of adding three gauge singlet fermions to the usual minimal standard model matter content is followed by an examination of right handed neutrinos in extended theories. I introduce the terminology of ``fully sterile'' and ``weakly sterile'' to classify varieties usually conflated under the sterile neutrino banner. After introducing the concepts of ``technical naturalness'' and plain ``naturalness'', the unbearable lightness of being a sterile neutrino is confronted. This problem is used to motivate mirror neutrinos, whose connection with pairwise maximal mixing is emphasised. Some brief remarks about phenomenology are made throughout. The impossibility of identifying the sole sterile neutrino of the currently favoured $2 + 2$ and $3 + 1$ phenomenologic...

Volkas, R R

2002-01-01

122

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

123

Neutrino masses and mixings  

SciTech Connect

Theoretical prejudices, cosmology, and neutrino oscillation experiments all suggest neutrino mass are far below present direct experimental limits. Four interesting scenarios and their implications are discussed: (1) a 17 keV {nu}{sub {tau}}, (2) a 30 ev {nu}{sub {tau}} making up the dark matter, (3) a 10{sup {minus}3} ev {nu}{sub {mu}} to solve the solar neutrino problem, and (4) a three-neutrino MSW solution.

Wolfenstein, L.

1991-12-31

124

Solar neutrinos - Eclipse effect  

E-print Network

It is pointed out that the enhancement of the solar neutrino rate in a real time detector like Super-Kamioka, SNO or Borexino due to neutrino oscillations in the moon during a partial or total solar eclipse may be observable. The enhancement is calculated as a function of the neutrino parameters in the case of three flavor mixing. This enhancement if seen, can further help to determine the neutrino parameters.

Mohan Narayan; G. Rajasekaran; Rahul Sinha

1997-03-12

125

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

126

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

127

Youth at Risk: A Prevention Resource for Counselors, Teachers, and Parents. Fourth Edition.  

ERIC Educational Resources Information Center

The fourth revision of this text offers both tested prevention strategies for work with diverse at-risk populations and counseling techniques that address the complexities of destructive behavior from individual, family, school, and community perspectives. Drawing on the wisdom of 24 experts, this book provides concrete advice for creating and…

Capuzzi, David, Ed.; Gross, Douglas R., Ed.

128

Solar Neutrino Spectroscopy  

NASA Astrophysics Data System (ADS)

Since the pioneering experiment of R. Davis et al., which started neutrino astronomy by measuring the solar neutrinos via the inverse beta decay reaction on 37Cl, all solar neutrino experiments find a considerably lower flux than expected by standard solar models. This finding is generally called the solar neutrino problem. Many attempts have been made to explain this result by altering the solar models, or assuming different nuclear cross sections for fusion processes assumed to be the energy sources in the sun. There have been performed numerous experiments recently to investigate the different possibilities to explain the solar neutrino problem. These experiments covered solar physics with helioseismology, nuclear cross section measurements, and solar neutrino experiments. Up to now no convincing explanation based on "standard" physics was suggested. However, assuming nonstandard neutrino properties, i.e. neutrino masses and mixing as expected in most extensions of the standard theory of elementary particle physics, natural solutions for the solar neutrino problem can be found. It appears that with this newly invented neutrino astronomy fundamental information on astrophysics as well as elementary particle physics are tested uniquely. In this contribution an attempt is made to review the situation of the neutrino astronomy for solar neutrino spectroscopy and discuss the future prospects in this field.

Feilitzsch, F. v.

1999-01-01

129

B-L Neutrinos  

E-print Network

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

Kevin Cahill

2000-06-19

130

Neutrino Physics (theory)  

Microsoft Academic Search

Nonzero neutrino masses are the first definitive need to extend the standard model. After reviewing the basic framework, I describe the status of some of the major issues, including tests of the basic framework of neutrino masses and mixings; the question of Majorana vs. Dirac; the spectrum, mixings, and number of neutrinos; models, with special emphasis on constraints from typical

Paul Langacker

2005-01-01

131

Neutrino Magnetic Moment  

E-print Network

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

A. B. Balantekin

2006-01-13

132

Solar Neutrinos Kamioka Observatory  

E-print Network

Solar neutrinos are produced by nuclear reaction chains in the central core of the sun. The solar of the nuclear reactions, the opacity of the sun, and so on. The largest fraction of the solar neutrinos the CNO cycle. In the pp-chain, the following #12;ve nuclear reactions produce neutrinos: p + p ! d + e

Tokyo, University of

133

18. SECOND FLOOR, 202 EAST FOURTH STREET LOOKING NORTHWEST, BEARING ...  

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

18. SECOND FLOOR, 202 EAST FOURTH STREET LOOKING NORTHWEST, BEARING WALL BETWEEN 202 AND 204, INSIGNIA OF FOURTH WARD REPUBLICAN CLUB - Phillips-Thompson Building, 200-206 East Fourth Street, Wilmington, New Castle County, DE

134

Tachyonic neutrinos and the neutrino masses  

E-print Network

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_{\

Robert Ehrlich

2012-12-05

135

Neutrino Observations from the Sudbury Neutrino Observatory  

E-print Network

The Sudbury Neutrino Observatory (SNO) is a water imaging Cherenkov detector. Its usage of 1000 metric tons of D$_{2}$O as target allows the SNO detector to make a solar-model independent test of the neutrino oscillation hypothesis by simultaneously measuring the solar $\

A. W. P. Poon; for the SNO Collaboration

2001-10-07

136

Neutrino observations from the Sudbury Neutrino Observatory  

SciTech Connect

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

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

2001-09-24

137

Supernova Neutrino Detection  

E-print Network

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

Kate Scholberg

2012-05-27

138

Neutrinos and Mass  

NSDL National Science Digital Library

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

Harris, Kathryn Louise.

139

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

140

The Sudbury Neutrino Observatory  

NSDL National Science Digital Library

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

141

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

142

Democratic Neutrino Theory  

E-print Network

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

Dmitry Zhuridov

2014-05-21

143

Search for Majorana neutrinos in $B^- \\to \\pi^+\\mu^-\\mu^-$ decays  

E-print Network

A search for heavy Majorana neutrinos produced in the $B^- \\to \\pi^+\\mu^-\\mu^-$ 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 TeV and 8 TeV at the LHC. Neutrinos with masses in the range 250-5000 MeV and lifetimes from zero to 1000 ps are probed. In the absence of a signal, upper limits are set on the branching fraction ${\\cal{B}}(B^- \\to \\pi^+\\mu^-\\mu^-)$ 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, Roel; Adinolfi, Marco; Affolder, Anthony; Ajaltouni, Ziad; Albrecht, Johannes; Alessio, Federico; Alexander, Michael; Ali, Suvayu; Alkhazov, Georgy; Alvarez Cartelle, Paula; Alves Jr, Antonio; Amato, Sandra; Amerio, Silvia; Amhis, Yasmine; Anderlini, Lucio; Anderson, Jonathan; Andreassen, Rolf; Andreotti, Mirco; Andrews, Jason; Appleby, Robert; Aquines Gutierrez, Osvaldo; Archilli, Flavio; Artamonov, Alexander; Artuso, Marina; Aslanides, Elie; Auriemma, Giulio; Baalouch, Marouen; Bachmann, Sebastian; Back, John; Badalov, Alexey; Balagura, Vladislav; Baldini, Wander; Barlow, Roger; Barschel, Colin; Barsuk, Sergey; Barter, William; Batozskaya, Varvara; Bauer, Thomas; Bay, Aurelio; Beddow, John; Bedeschi, Franco; Bediaga, Ignacio; Belogurov, Sergey; Belous, Konstantin; Belyaev, Ivan; Ben-Haim, Eli; Bencivenni, Giovanni; Benson, Sean; Benton, Jack; Berezhnoy, Alexander; Bernet, Roland; Bettler, Marc-Olivier; van Beuzekom, Martinus; Bien, Alexander; Bifani, Simone; Bird, Thomas; Bizzeti, Andrea; Bjørnstad, Pål Marius; Blake, Thomas; Blanc, Frédéric; Blouw, Johan; Blusk, Steven; Bocci, Valerio; Bondar, Alexander; Bondar, Nikolay; Bonivento, Walter; Borghi, Silvia; Borgia, Alessandra; Borsato, Martino; Bowcock, Themistocles; Bowen, Espen Eie; Bozzi, Concezio; Brambach, Tobias; van den Brand, Johannes; Bressieux, Joël; Brett, David; Britsch, Markward; Britton, Thomas; Brook, Nicholas; Brown, Henry; Bursche, Albert; Busetto, Giovanni; Buytaert, Jan; Cadeddu, Sandro; Calabrese, Roberto; Callot, Olivier; Calvi, Marta; Calvo Gomez, Miriam; Camboni, Alessandro; Campana, Pierluigi; Campora Perez, Daniel; Carbone, Angelo; Carboni, Giovanni; Cardinale, Roberta; Cardini, Alessandro; Carranza-Mejia, Hector; Carson, Laurence; Carvalho Akiba, Kazuyoshi; Casse, Gianluigi; Castillo Garcia, Lucia; Cattaneo, Marco; Cauet, Christophe; Cenci, Riccardo; Charles, Matthew; Charpentier, Philippe; Cheung, Shu-Faye; Chiapolini, Nicola; Chrzaszcz, Marcin; Ciba, Krzystof; Cid Vidal, Xabier; Ciezarek, Gregory; Clarke, Peter; Clemencic, Marco; Cliff, Harry; Closier, Joel; Coca, Cornelia; Coco, Victor; Cogan, Julien; Cogneras, Eric; Collins, Paula; Comerma-Montells, Albert; Contu, Andrea; Cook, Andrew; Coombes, Matthew; Coquereau, Samuel; Corti, Gloria; Counts, Ian; Couturier, Benjamin; Cowan, Greig; Craik, Daniel Charles; Cruz Torres, Melissa Maria; Cunliffe, Samuel; Currie, Robert; D'Ambrosio, Carmelo; Dalseno, Jeremy; David, Pascal; David, Pieter; Davis, Adam; De Bonis, Isabelle; De Bruyn, Kristof; De Capua, Stefano; De Cian, Michel; De Miranda, Jussara; De Paula, Leandro; De Silva, Weeraddana; De Simone, Patrizia; Decamp, Daniel; Deckenhoff, Mirko; Del Buono, Luigi; Déléage, Nicolas; Derkach, Denis; Deschamps, Olivier; Dettori, Francesco; Di Canto, Angelo; Dijkstra, Hans; Donleavy, Stephanie; Dordei, Francesca; Dorigo, Mirco; Dorosz, Piotr; Dosil Suárez, Alvaro; Dossett, David; Dovbnya, Anatoliy; Dupertuis, Frederic; Durante, Paolo; Dzhelyadin, Rustem; Dziurda, Agnieszka; Dzyuba, Alexey; Easo, Sajan; Egede, Ulrik; Egorychev, Victor; Eidelman, Semen; Eisenhardt, Stephan; Eitschberger, Ulrich; Ekelhof, Robert; Eklund, Lars; El Rifai, Ibrahim; Elsasser, Christian; Falabella, Antonio; Färber, Christian; Farinelli, Chiara; Farry, Stephen; Ferguson, Dianne; Fernandez Albor, Victor; Ferreira Rodrigues, Fernando; Ferro-Luzzi, Massimiliano; Filippov, Sergey; Fiore, Marco; Fiorini, Massimiliano; Fitzpatrick, Conor; Fontana, Marianna; Fontanelli, Flavio; Forty, Roger; Francisco, Oscar; Frank, Markus; Frei, Christoph; Frosini, Maddalena; Furfaro, Emiliano; Gallas Torreira, Abraham; Galli, Domenico; Gandelman, Miriam; Gandini, Paolo; Gao, Yuanning; Garofoli, Justin; Garra Tico, Jordi; Garrido, Lluis; Gaspar, Clara; Gauld, Rhorry; Gersabeck, Evelina; Gersabeck, Marco; Gershon, Timothy; Ghez, Philippe; Gianelle, Alessio; Gibson, Valerie; Giubega, Lavinia-Helena; Gligorov, Vladimir; Göbel, Carla; Golubkov, Dmitry; Golutvin, Andrey; Gomes, Alvaro; Gordon, Hamish; Grabalosa Gándara, Marc; Graciani Diaz, Ricardo; Granado Cardoso, Luis Alberto; Graugés, Eugeni; Graziani, Giacomo; Grecu, Alexandru; Greening, Edward; Gregson, Sam; Griffith, Peter; Grillo, Lucia; Grünberg, Oliver; Gui, Bin; Gushchin, Evgeny; Guz, Yury; Gys, Thierry; Hadjivasiliou, Christos; Haefeli, Guido; Haen, Christophe; Hafkenscheid, Tom; Haines, Susan; Hall, Samuel; Hamilton, Brian; Hampson, Thomas; Hansmann-Menzemer, Stephanie; Harnew, Neville; Harnew, Samuel; Harrison, Jonathan; Hartmann, Thomas; He, Jibo; Head, Timothy; Heijne, Veerle; Hennessy, Karol; Henrard, Pierre

2014-01-01

144

Collective neutrino oscillations in supernovae  

SciTech Connect

In a dense neutrino medium neutrinos can experience collective flavor transformation through the neutrino-neutrino forward scattering. In this talk we present some basic features of collective neutrino flavor transformation in the context in core-collapse supernovae. We also give some qualitative arguments for why and when this interesting phenomenon may occur and how it may affect supernova nucleosynthesis.

Duan, Huaiyu [Department of Physics and Astronomy, University of New Mexico, Albuquerque, NM 87131 (United States)

2014-06-24

145

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

146

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

147

Atmospheric neutrino oscillations and tau neutrinos in ice  

E-print Network

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

Gerardo Giordano; Olga Mena; Irina Mocioiu

2010-04-20

148

Fundamental Neutrinos Properties  

NASA Astrophysics Data System (ADS)

After about six decades since the discovery of the neutrino, we have started to understand the role of neutrinos in our world. The discoveries of oscillations of atmospheric, solar, accelerator and reactor neutrinos have opened a new excited era in neutrino physics and represents a big step forward in our knowledge of neutrino properties. The observed small neutrino masses have profound implications for our understanding of the Universe and are now a major focus in astro, particle and nuclear physics and in cosmology. The physics community worldwide is embarking on the challenging problem, finding whether neutrinos are indeed Majorana particles (i.e., identical to its own antiparticle) as many particle models suggest or Dirac particles (i.e., is different from its antiparticle). The search for the 0? ? ?-decay represents the new frontiers of neutrino physics, allowing to determine the Majorana nature of neutrinos and to fix the neutrino mass scale and possible CP violation effects, which could explain the matter-antimatter asymmetry in the Universe.

Šimkovic, Fedor

149

SuperGZK neutrinos  

E-print Network

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

V. Berezinsky

2005-09-22

150

MINOS Sterile Neutrino Search  

SciTech Connect

The Main Injector Neutrino Oscillation Search (MINOS) is a long-baseline accelerator neutrino experiment designed to measure properties of neutrino oscillation. Using a high intensity muon neutrino beam, produced by the Neutrinos at Main Injector (NuMI) complex at Fermilab, MINOS makes two measurements of neutrino interactions. The first measurement is made using the Near Detector situated at Fermilab and the second is made using the Far Detector located in the Soudan Underground laboratory in northern Minnesota. The primary goal of MINOS is to verify, and measure the properties of, neutrino oscillation between the two detectors using the {nu}{sub {mu}} {yields} V{sub {tau}} transition. A complementary measurement can be made to search for the existence of sterile neutrinos; an oft theorized, but experimentally unvalidated particle. The following thesis will show the results of a sterile neutrino search using MINOS RunI and RunII data totaling {approx}2.5 x 10{sup 20} protons on target. Due to the theoretical nature of sterile neutrinos, complete formalism that covers transition probabilities for the three known active states with the addition of a sterile state is also presented.

Koskinen, David Jason; /University Coll. London

2009-09-01

151

Sudbury Neutrino Observatory  

SciTech Connect

This document is a technical progress report on work performed at the University of Pennsylvania during the current year on the Sudbury Neutrino Observatory project. The motivation for the experiment is the measurement of neutrinos emitted by the sun. The Sudbury Neutrino Observatory (SNO) is a second generation dedicated solar neutrino experiment which will extend the results of our work with the Kamiokande II detector by measuring three reactions of neutrinos rather than the single reaction measured by the Kamiokande experiment. The collaborative project includes physicists from Canada, the United Kingdom, and the United States. Full funding for the construction of this facility was obtained in January 1990, and its construction is estimated to take five years. The motivation for the SNO experiment is to study the fundamental properties of neutrinos, in particular the mass and mixing parameters, which remain undetermined after decades of experiments in neutrino physics utilizing accelerators and reactors as sources of neutrinos. To continue the study of neutrino properties it is necessary to use the sun as a neutrino source. The long distance to the sun makes the search for neutrino mass sensitive to much smaller mass than can be studied with terrestrial sources. Furthermore, the matter density in the sun is sufficiently large to enhance the effects of small mixing between electron neutrinos and mu or tau neutrinos. This experiment, when combined with the results of the radiochemical {sup 37}Cl and {sup 71}Ga experiments and the Kamiokande II experiment, should extend our knowledge of these fundamental particles, and as a byproduct, improve our understanding of energy generation in the sun.

Beier, E.W.

1992-03-01

152

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

SciTech Connect

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

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

2011-01-01

153

Neutrinos and Collider Physics  

E-print Network

We review the collider phenomenology of neutrino physics and the synergetic aspects at energy, intensity and cosmic frontiers to test the new physics behind the neutrino mass mechanism. In particular, we focus on seesaw models within the minimal setup as well as with extended gauge and/or Higgs sectors, and on supersymmetric neutrino mass models with seesaw mechanism and with $R$-parity violation. In the simplest Type-I seesaw scenario with sterile neutrinos, we summarize and update the current experimental constraints on the sterile neutrino mass and its mixing with the active neutrinos. We also discuss the future experimental prospects of testing the seesaw mechanism at colliders and in related low-energy searches for rare processes, such as lepton flavor violation and neutrinoless double beta decay. The implications of the discovery of lepton number violation at the LHC for leptogenesis are also studied.

Deppisch, Frank F; Pilaftsis, Apostolos

2015-01-01

154

Solar neutrino detection  

E-print Network

More than 40 years ago, neutrinos where conceived as a way to test the validity of the solar models which tell us that stars are powered by nuclear fusion reactions. The first measurement of the neutrino flux, in 1968 in the Homestake mine in South Dakota, detected only one third of the expected value, originating what has been known as the Solar Neutrino Problem. Different experiments were built in order to understand the origin of this discrepancy. Now we know that neutrinos undergo oscillation phenomenon changing their nature traveling from the core of the Sun to our detectors. In the work the 40 year long saga of the neutrino detection is presented; from the first proposals to test the solar models to last real time measurements of the low energy part of the neutrino spectrum.

Lino Miramonti

2009-01-22

155

Spectroscopy of Solar Neutrinos  

E-print Network

In the last years, liquid-scintillator detectors have opened a new window for the observation of low-energetic astrophysical neutrino sources. In 2007, the solar neutrino experiment Borexino began its data-taking in the Gran Sasso underground laboratory. High energy resolution and excellent radioactive background conditions in the detector allow the first-time spectroscopic measurement of solar neutrinos in the sub-MeV energy regime. The experimental results of the Beryllium-7 neutrino flux measurements as well as the prospects for the detection of solar Boron-8, pep and CNO neutrinos are presented in the context of the currently discussed ambiguities in solar metallicity. In addition, the potential of the future SNO+ and LENA experiments for high-precision solar neutrino spectroscopy will be outlined.

Wurm, Michael; Goeger-Neff, Marianne; Lachenmaier, Tobias; Lewke, Timo; Meindl, Quirin; Moellenberg, Randoplh; Oberauer, Lothar; Potzel, Walter; Tippmann, Marc; Traunsteiner, Christoph; Winter, Juergen

2010-01-01

156

Neutrinos from Gamma Ray Bursts  

E-print Network

We show that the detection of neutrinos from a typical gamma ray burst requires a kilometer-scale detector. We argue that large bursts should be visible with the neutrino telescopes under construction. We emphasize the 3 techniques by which neutrino telescopes can perform this search: by triggering on i) bursts of muons from muon neutrinos, ii) muons from air cascades initiated by high energy gamma rays and iii) showers made by relatively low energy ($\\simeq 100\\,\\mev$) electron neutrinos. Timing of neutrino-photon coincidences may yield a measurement of the neutrino mass to order $10^{-5}$~eV, an interesting range in light of the solar neutrino anomaly.

F. Halzen; G. Jaczko

1996-02-07

157

Neutrino Oscillation Studies with Reactors  

E-print Network

Nuclear reactors are one of the most intense, pure, controllable, cost-effective, and well-understood sources of neutrinos. Reactors have played a major role in the study of neutrino oscillations, a phenomenon that indicates that neutrinos have mass and that neutrino flavors are quantum mechanical mixtures. Over the past several decades reactors were used in the discovery of neutrinos, were crucial in solving the solar neutrino puzzle, and allowed the determination of the smallest mixing angle $\\theta_{13}$. In the near future, reactors will help to determine the neutrino mass hierarchy and to solve the puzzling issue of sterile neutrinos.

Vogel, Petr; Zhang, Chao

2015-01-01

158

Neutrino Oscillation Studies with Reactors  

E-print Network

Nuclear reactors are one of the most intense, pure, controllable, cost-effective, and well-understood sources of neutrinos. Reactors have played a major role in the study of neutrino oscillations, a phenomenon that indicates that neutrinos have mass and that neutrino flavors are quantum mechanical mixtures. Over the past several decades reactors were used in the discovery of neutrinos, were crucial in solving the solar neutrino puzzle, and allowed the determination of the smallest mixing angle $\\theta_{13}$. In the near future, reactors will help to determine the neutrino mass hierarchy and to solve the puzzling issue of sterile neutrinos.

Petr Vogel; Liangjian Wen; Chao Zhang

2015-03-03

159

The AMANDA Neutrino Detector  

Microsoft Academic Search

The first stage of the AMANDA High Energy Neutrino Detector at the South Pole, the 302 PMT array AMANDA-B with an expected effective area for TeV neutrinos of ~104m2, has been taking data since 1997. Progress with calibration, investigation of ice properties, as well as muon and neutrino data analysis are described. The next stage 20-string detector AMANDA-II with ~800PMTs

R. Wischnewski; E. Andrés; P. Askebjer; S. Barwick; R. Bay; L. Bergström; A. Biron; J. Booth; O. Botner; A. Bouchta; S. Carius; M. Carlson; W. Chinowsky; D. Chirkin; D. Cowen; C. Costa; E. Dalberg; T. De Young; J. Edsjo; P. Ekström; A. Goobar; L. Gray; A. Hallgren; F. Halzen; R. Hardtke; Y. He; G. Hill; P. Hulth; S. Hundertmark; J. Jacobsen; V. Kandhadai; A. Karle; J. Kim; H. Leich; M. Leuthold; P. Lindahl; T. Liss; I. Liubarsky; P. Loaiza; D. Lowder; P. Marciniewski; T. Miller; P. Miocinovic; P. Mock; R. Morse; M. Newcomer; P. Niessen; D. Nygren; C. Pérez de los Heros; R. Porrata; P. Price; G. Przybylski; W. Rhode; S. Richter; J. Rodriguez; P. Romenesko; D. Ross; H. Rubinstein; T. Schmidt; E. Schneider; R. Schwarz; U. Schwendicke; G. Smoot; M. Solarz; V. Sorin; C. Spiering; P. Steffen; R. Stokstad; O. Streicher; L. Thollander; T. Thon; S. Tilav; C. Walck; C. Wiebusch; K. Woschnagg; W. Wu; G. Yodh; S. Young

1999-01-01

160

The AMANDA Neutrino Detector  

SciTech Connect

The first stage of the AMANDA High Energy Neutrino Detectorat the South Pole, the 302 PMT array AMANDA-B with an expected effectivearea for TeV neutrinos of similar to 10(4) m(2), has been taking datasince 1997. Progress with calibration, investigation of ice properties,as well as muon and neutrino data analysis are described. The next stage20-string detector AMANDA-II with similar to 800 PMTs will be completedin spring 2000.

Wischnewski, R.; Andres, E.; Askebjer, P.; Barwick, S.; Bay, R.; Bergstrom, L.; Biron, A.; Booth, J.; Botner, O.; Bouchta, A.; Carius, S.; Carlson, M.; Chinowsky, W.; Chirkin, D.; Cowen, D.; Costa, C.; Dalberg,E.; Deyoung, T.; Edsjo, J.; Ekstrom, P.; Goobar, A.; Gray, L.; Hallgren,A.; Halzen, F.; Hardtke, R.; He, Y.; Hill, G.; Hulth, P.; Hundertmark,S.; Jacobsen, J.; Kandhadai, V.; Karle, A.; Kim, J.; Leich, H.; Leuthold,M.; Lindahl, P.; Liss, T.; Liubarsky, I.; Loaiza, P.; Lowder, D.; Marciniewski, P.; Miller, T.; Miocinovic, P.; Mock, P.; Morse, R.; Newcomer, M.; Niessen, P.; Nygren, D.; de, los, Heros, CP.; Porrata, R.; Price, P.; Przybylski, G.; Rhode, W.; Richter, S.; Rodriguez, J.; Romenesko, P.; Ross, D.; Rubinstein, H.; Schmidt, T.; Schneider, E.; Schwarz, R.; Schwendicke, U.; Smoot, G.; Solarz, M.; Sorin, V.; Spiering,C.; Steffen, P.; Stokstad, R.; Streicher, O.; Thollander, L.; Thon, T.; Tilav, S.; Walck, C.; Wiebusch, C.; Woschnagg, K.; Wu, W.; Yodh, G.; Young, S.

1999-08-23

161

Neutrinos: Nature's Ghosts?  

SciTech Connect

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

Lincoln, Don

2013-06-18

162

Neutrinos: Nature's Ghosts?  

ScienceCinema

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

Lincoln, Don

2014-08-12

163

Introduction to sterile neutrinos  

NASA Astrophysics Data System (ADS)

Model-building issues raised by the prospect of light sterile neutrinos are discussed in a pedagogical way. I first review the naive proposal that sterile neutrinos be identified with “right handed neutrinos”. A critical discussion of the simple expedient of adding three gauge singlet fermions to the usual minimal standard model matter content is followed by an examination of right handed neutrinos in extended theories. I introduce the terminology of “fully sterile” and “weakly sterile” to classify varieties usually conflated under the sterile neutrino banner. After introducing the concepts of “technical naturalness” and plain “naturalness”, the unbearable lightness of being a sterile neutrino is confronted. This problem is used to motivate mirror neutrinos, whose connection with pairwise maximal mixing is emphasised. Some brief remarks about phenomenology are made throughout. The impossibility of identifying the sole sterile neutrino of the currently favoured 2 + 2 and 3 + 1 phenomenological constructs as a lone gauge singlet fermion added to the minimal standard model is explained. Finally, I remark on the beauty and subtlety of light sterile neutrino cosmology.

Volkas, R. R.

2002-07-01

164

Introduction to sterile neutrinos  

E-print Network

Model-building issues raised by the prospect of light sterile neutrinos are discussed in a pedagogical way. I first review the na\\"{\\i}ve proposal that sterile neutrinos be identified with ``right handed neutrinos''. A critical discussion of the simple expedient of adding three gauge singlet fermions to the usual minimal standard model matter content is followed by an examination of right handed neutrinos in extended theories. I introduce the terminology of ``fully sterile'' and ``weakly sterile'' to classify varieties usually conflated under the sterile neutrino banner. After introducing the concepts of ``technical naturalness'' and plain ``naturalness'', the unbearable lightness of being a sterile neutrino is confronted. This problem is used to motivate mirror neutrinos, whose connection with pairwise maximal mixing is emphasised. Some brief remarks about phenomenology are made throughout. The impossibility of identifying the sole sterile neutrino of the currently favoured $2 + 2$ and $3 + 1$ phenomenological constructs as a lone gauge singlet fermion added to the minimal standard model is explained. Finally, I remark on the beauty and subtlety of light sterile neutrino cosmology.

Raymond R. Volkas

2001-11-26

165

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

166

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

167

Multimessenger Astronomy and Neutrinos  

NASA Astrophysics Data System (ADS)

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

Ando, Shin'ichiro

2013-04-01

168

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

169

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

170

Extremely high energy cosmic neutrinos and relic neutrinos  

SciTech Connect

I review the essentials of ultrahigh-energy neutrino interactions, show how neutral-current detection and flavor tagging can enhance the scientific potential of neutrino telescopes, and sketch new studies on neutrino encounters with dark matter relics and on gravitational lensing of neutrinos.

Quigg, Chris; /Fermilab /CERN

2006-03-01

171

High Energy Neutrinos with a Mediterranean Neutrino Telescope  

SciTech Connect

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

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

2007-09-01

172

Long range neutrino forces in the cosmic relic neutrino background  

E-print Network

Neutrinos mediate long range forces among macroscopic bodies in vacuum. When the bodies are placed in the neutrino cosmic background, these forces are modified. Indeed, at distances long compared to the scale $T^{-1}$, the relic neutrinos completely screen off the 2-neutrino exchange force, whereas for small distances the interaction remains unaffected.

Ferrer, F; Nowakowski, M

2000-01-01

173

Long range neutrino forces in the cosmic relic neutrino background  

E-print Network

Neutrinos mediate long range forces among macroscopic bodies in vacuum. When the bodies are placed in the neutrino cosmic background, these forces are modified. Indeed, at distances long compared to the scale $T^{-1}$, the relic neutrinos completely screen off the 2-neutrino exchange force, whereas for small distances the interaction remains unaffected.

F. Ferrer; J. A. Grifols; M. Nowakowski

1999-06-23

174

Effect of neutrino magnetic moment on solar neutrino observations  

Microsoft Academic Search

Neutrino spin precession effects in the magnetic field of the Sun are considered as an explanation of the outcome of Davis' solar neutrino experiments. Theoretically, it is possible to account for a neutrino magnetic moment only as the result of the interaction of the electromagnetic field with charged particles into which the neutrino can transform virtually. The currently accepted theory

Arturo Cisneros

1971-01-01

175

Solar Neutrinos: Where We Are, Where We Are Going  

E-print Network

There are four important facts about solar neutrinos. They are listed in order of importance in this abstract and discussed more in the text of the talk. First, solar neutrinos have been detected in four experiments with approximately the energies and fluxes predicted by the standard solar model, confirming the hypothesis that the energy source for the solar luminosity is the fusion of light elements. Second, the measured event rates are significantl less than the event rates predicted by the combined standard solar and electroweak models in all four experiments. Third, a comparison of the event rates measured in the chlorine experiment (threshold 0.8 Mev) and the neutrino-electron scattering experiment (Kamiokande II, threshold 7.5 MeV) indicates that the deficiency of electron-type neutrinos at the earth is energy dependent, if the rates and the uncertainties in both experiments have been correctly understood. The inference that the deficiency is energy-dependent conflicts with the simplest version of standard electroweak theory. Fourth, experiments are being constructed that have the capabilities to determine conclusively if new neutrino physics is required.

John N. Bahcall

1994-04-28

176

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

177

"Researching" with Third- and Fourth-Graders.  

ERIC Educational Resources Information Center

In order to instill in children the skills which will be basic to their school experience, words implying a process (such as "hemp,""parasite," and "vanilla") may be "researched" by third and fourth graders through the use of a dictionary, an encyclopedia, a supplementary book on the subject, and an interview with an adult. The child makes a…

Liston, Barbara

1970-01-01

178

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

179

THE FOURTH HEAD OF N ILIJAS FARAH  

E-print Network

THE FOURTH HEAD OF N ILIJAS FARAH Abstract. We start with a concrete problem about continuous maps. Start from N, the space of natural numbers with the discrete topology, and consider its Cech]), Jan van Mill called it a three-headed monster. The first head shows under the Continuum Hypothesis, CH

Farah, Ilijas

180

THE FOURTH HEAD OF #N ILIJAS FARAH  

E-print Network

THE FOURTH HEAD OF #N ILIJAS FARAH Abstract. We start with a concrete problem about continuous maps picture. Start from N, the space of natural numbers with the discrete topology, and consider its Ÿ Cech ([28]), Jan van Mill called it a three­headed monster. The first head shows under the Continuum

Farah, Ilijas

181

FOURTH GENERATION OF CLOSED POPULATION HONEYBEE BREEDING  

E-print Network

FOURTH GENERATION OF CLOSED POPULATION HONEYBEE BREEDING 2. Relationship between morphological that morphological characters can be used to improve honeybee stock. INTRODUCTION Honey production is a complex characteristic of a honeybee colony, and so an understanding of the various factors affecting it is important

Paris-Sud XI, Université de

182

Fourth & Fifth Graders Make Blueprints from Scratch.  

ERIC Educational Resources Information Center

Describes a project in which third and fourth graders in a special education writing skills class learned how to design a house and make blueprints. Discusses the project's beneficial effects on student writing and public speaking skills, vocabulary, telephone skills, and effective peer interaction. (SV)

Jones, Sandy

1988-01-01

183

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

184

Fourth Graders Invent Ways of Computing Averages.  

ERIC Educational Resources Information Center

Presents three methods invented by fourth graders for obtaining the arithmetic mean. This presentation is in support of the idea that encouraging children to invent their own mathematical processes is a good way for them to clarify the idea of representativeness and consequently the teacher can facilitate the students' construction of higher…

Kamii, Constance; And Others

1996-01-01

185

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

186

The Fourth Partial Derivative In Transport Dynamics  

E-print Network

A new fourth partial derivative is introduced for the study of transport dynamics. It is a Lagrangian partial derivative following the path of diffusion, not the path of convection. Use of this derivative decouples the effect of diffusion and convection and simplifies the analysis of transport processes.

Trinh Khanh Tuoc

2010-01-11

187

Literature for Today's Young Adults. Fourth Edition.  

ERIC Educational Resources Information Center

Designed to help teachers open young minds to literature, this book presents criteria for evaluating books in all genres and their suggested classroom uses, an examination of hotly debated topics, and an overview of the significance of young adult literature. The fourth edition of the book features 30 boxed inserts containing essays by some of the…

Nilsen, Alleen Pace; Donelson, Kenneth L.

188

Summary of neutrino presentations  

SciTech Connect

This summary is divided into two sections. First, we concentrate on conventional neutrino physics interpreted in the context of standard electroweak theory. Second, we discuss double beta decay where gross violations of the predictions of the theory might appear, and also we discuss specific searches for consequences of finite neutrino mass. 11 figs., 5 tabs.

White, D.H.

1988-01-01

189

Neutrino Physics (Rapporteur talk)  

NASA Astrophysics Data System (ADS)

Papers related to neutrino physics, submitted in the categories NU-EX (experimental results), NU-IN (methods, techniques, and instrumentation) and NU-TH (theory, model, and simulations) are reviewed with a brief introduction on the current understanding of neutrino masses and mixings.

Nakahata, Masayuki

2014-10-01

190

Reactor monitoring with Neutrinos  

NASA Astrophysics Data System (ADS)

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

Cribier, Michel

2011-12-01

191

Reactor Monitoring with Neutrinos  

E-print Network

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

M. Cribier

2007-04-06

192

Neutrino masses and oscillations  

Microsoft Academic Search

A report on neutrino masses, mixing and oscillations, made in Dubna at the symposium dedicated to 100 years of the Rutherford's discovery of atomic nucleus, is presented. We start with the hypothesis of neutrino which was proposed by W. Pauli in December 1930 in order to solve some problems of nuclei (the problem of spin of $^{7}N_{14}$ and other nuclei

S. M. Bilenky

2011-01-01

193

Monte Carlo Neutrino Oscillations  

E-print Network

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

James P. Kneller; Gail C. McLaughlin

2005-09-29

194

Measurements of neutrino mass  

SciTech Connect

Direct experimental information of neutrino mass as derived from the study of nuclear and elementary-particle weak decays is reviewed. Topics include tritium beta decay; the /sup 3/He-T mass difference; electron capture decay of /sup 163/Ho and /sup 158/Tb; and limits on massive neutrinos from cosmology. 38 references. (WHK)

Robertson, R.G.H.

1985-01-01

195

Neutrino Astronomy Scott Wilbur  

E-print Network

radiation as it travels through the ice Photomultipliers pick up the Cherenkov radiation and can infer the direction of travel To select only neutrino events, only tracks coming through the Earth are kept #12;TheV protons, which should be created with neutrinos, have been seen Can be used to observe possible dark

Golwala, Sunil

196

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

197

Physics and Astrophysics of Neutrinos  

Microsoft Academic Search

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

Masataka Fukugita; Atsuto Suzuki

1994-01-01

198

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

199

7 CFR 51.2296 - Three-fourths half kernel.  

Code of Federal Regulations, 2011 CFR

...FRUITS, VEGETABLES AND OTHER 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...

2011-01-01

200

7 CFR 51.2296 - Three-fourths half kernel.  

Code of Federal Regulations, 2014 CFR

...FRUITS, VEGETABLES AND OTHER 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...

2014-01-01

201

7 CFR 51.2296 - Three-fourths half kernel.  

Code of Federal Regulations, 2012 CFR

...FRUITS, VEGETABLES AND OTHER 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...

2012-01-01

202

7 CFR 51.2296 - Three-fourths half kernel.  

Code of Federal Regulations, 2013 CFR

...FRUITS, VEGETABLES AND OTHER 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...

2013-01-01

203

7 CFR 51.2296 - Three-fourths half kernel.  

Code of Federal Regulations, 2010 CFR

...FRUITS, VEGETABLES AND OTHER 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...

2010-01-01

204

Bäcklund transformations for new fourth Painlevé hierarchies  

NASA Astrophysics Data System (ADS)

We consider a system of equations defined using the Hamiltonian operator of the Boussinesq hierarchy, as well as two successive modifications thereof. We are able to reduce the order of these three systems and give Bäcklund transformations between the integrated equations. We also give auto-Bäcklund transformations for the two modified systems. Particular cases of two of the three equations considered correspond to generalized fourth Painlevé hierarchies and are new; these are particular cases of the two modified systems. Thus we obtain auto-Bäcklund transformations for these new fourth Painlevé hierarchies, as well as Bäcklund transformations between our hierarchies. Our results on reduction of order are also applicable in this special case, and include as a particular example a reduction of order for the scaling similarity reduction of the Boussinesq equation, a result which, remarkably, seems not to have been given previously.

Conde, J. M.; Gordoa, P. R.; Pickering, A.

2014-03-01

205

Fourth-generation photovoltaic concentrator system development  

SciTech Connect

In 1991, under a contract with Sandia for the Concentrator Initiative, the ENTECH team initiated the design and development of a fourth-generation concentrator module. In 1992, Sandia also contracted with ENTECH to develop a new control and drive system for the ENTECH array. This report documents the design and development work performed under both contracts. Manufacturing processes for the new module were developed at the same time under a complementary PVMaT contract with the National Renewable Energy Laboratory. Two 100-kW power plants were deployed in 1995 in Texas using the newly developed fourth-generation concentrator technology, one at the CSW Solar Park near Ft. Davis and one at TUE Energy Park in Dallas. Technology developed under the Sandia contracts has made a successful transition from the laboratory to the production line to the field.

O`Neill, M.J.; McDanal, A.J. [ENTECH, Inc., Dallas-Fort Worth Airport, TX (United States)

1995-10-01

206

Is fourth generation mobile nirvana or … nothing?  

Microsoft Academic Search

So far fourth generation (4G) has not been well defined technically, functionally or commercially despite conceptual research having been quietly under way since 1998. But as we have not fully rolled out and digested 2.5G, let alone 3G, why on earth should we be interested in a still further mobile technology? And how will WiFi, WiMAX and existing networks figure

Simon Forge

2004-01-01

207

Fourth High Alpha Conference, volume 2  

NASA Technical Reports Server (NTRS)

The goal of the Fourth High Alpha Conference, held at the NASA Dryden Flight Research Center on July 12-14, 1994, was to focus on the flight validation of high angle of attack technologies and provide an in-depth review of the latest high angle of attack activities. Areas that were covered include high angle of attack aerodynamics, propulsion and inlet dynamics, thrust vectoring, control laws and handling qualities, and tactical utility.

1994-01-01

208

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

209

Fourth High Alpha Conference, volume 1  

NASA Technical Reports Server (NTRS)

The goal of the Fourth High Alpha Conference was to focus on the flight validation of high angle-of-attack technologies and provide an in-depth review of the latest high angle-of-attack activities. Areas that were covered include: high angle-of-attack aerodynamics, propulsion and inlet dynamics, thrust vectoring, control laws and handling qualities, tactical utility, and forebody controls.

1994-01-01

210

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

211

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

212

Neutrinos: Nature's Identity Thieves?  

SciTech Connect

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

Lincoln, Don

2013-07-11

213

Neutrino time travel  

E-print Network

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

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

2007-12-09

214

Neutrino mass experiments  

SciTech Connect

The current status of the experimental search for neutrino mass is reviewed, with emphasis on direct kinematic methods. Simpson and Hime report finding new evidence for a 17-keV neutrino in the ..beta.. decay of /sup 3/H and /sup 35/S. The situation concerning the electron neutrino mass as measured in tritium beta decay has not changed significantly in the last two years. We discuss the ''model independent'' lower limit of 17 eV obtained by the ITEP group in light of existing data on the /sup 3/H--/sup 3/He mass difference. 42 refs., 1 fig., 1 tab.

Robertson, R.G.H.

1989-01-01

215

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

216

Neutrinos: Nature's Identity Thieves?  

ScienceCinema

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

Lincoln, Don

2014-08-07

217

Submarine neutrino communication  

E-print Network

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

Patrick Huber

2010-08-20

218

Submarine neutrino communication  

E-print Network

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

Huber, Patrick

2009-01-01

219

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

220

SNO+ Multipurpose Neutrino Detector  

NASA Astrophysics Data System (ADS)

SNO+ proposes to fill the existing SNO detector with liquid scintillator. The unique location in SNOLAB, currently the worlds deepest international underground facility, will enable a variety of physics measurements from further studies of solar neutrinos (pep and CNO), to geo- and reactor neutrinos, to supernova neutrinos to the possibility of studying neutrinoless double beta decay. With the addition of ^150Nd to the liquid scintillator SNO+ is capable of a competitive next-generation search for this rare process. The physics potential and experimental sensitivities will be discussed.

Kraus, Christine

2008-10-01

221

Fourth order difference methods for hyperbolic IBVP's  

NASA Technical Reports Server (NTRS)

Fourth order difference approximations of initial-boundary value problems for hyperbolic partial differential equations are considered. We use the method of lines approach with both explicit and compact implicit difference operators in space. The explicit operator satisfies an energy estimate leading to strict stability. For the implicit operator we develop boundary conditions and give a complete proof of strong stability using the Laplace transform technique. We also present numerical experiments for the linear advection equation and Burgers' equation with discontinuities in the solution or in its derivative. The first equation is used for modeling contact discontinuities in fluid dynamics, the second one for modeling shocks and rarefaction waves. The time discretization is done with a third order Runge-Kutta TVD method. For solutions with discontinuities in the solution itself we add a filter based on second order viscosity. In case of the non-linear Burger's equation we use a flux splitting technique that results in an energy estimate for certain different approximations, in which case also an entropy condition is fulfilled. In particular we shall demonstrate that the unsplit conservative form produces a non-physical shock instead of the physically correct rarefaction wave. In the numerical experiments we compare our fourth order methods with a standard second order one and with a third order TVD-method. The results show that the fourth order methods are the only ones that give good results for all the considered test problems.

Gustafsson, Bertil; Olsson, Pelle

1994-01-01

222

HOST FAMILY PROGRAM Host family: ____________________________________ Family No. _________  

E-print Network

HOST FAMILY PROGRAM Host family: ____________________________________ Family No. _________ Student: 13 January ­ 28 May 2003 THE FAMILY PROVIDES THE STUDENT WITH: 1. Three meals daily all week long. (If a student should arrive home too late for a meal, the family should leave the prepared meal

223

Atmospheric neutrino oscillations and tau neutrinos in ice  

SciTech Connect

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

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

2010-06-01

224

Leptogenesis in a Hybrid Texture Neutrino Mass Model  

E-print Network

We investigate the CP asymmetry for a hybrid texture of the neutrino mass matrix predicted by $Q_8$ family symmetry in the context of the type-I seesaw mechanism and examine its consequences for leptogenesis. We, also, calculate the resulting Baryon Asymmetry of the Universe (BAU) for this texture.

S. Dev; Surender Verma

2010-05-25

225

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

226

Neutrino astrophysics : recent advances and open issues  

E-print Network

We highlight recent advances in neutrino astrophysics, the open issues and the interplay with neutrino properties. We emphasize the important progress in our understanding of neutrino flavor conversion in media. We discuss the case of solar neutrinos, of core-collapse supernova neutrinos and of SN1987A, and of the recently discovered ultra-high energy neutrinos whose origin is to be determined.

Volpe, Cristina

2015-01-01

227

The Science of NOA Neutrinos are everywhere!  

E-print Network

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

Quigg, Chris

228

Neutrino mass: Recent results  

SciTech Connect

Some recent developments in the experimental search for neutrino mass are discussed. Simpson and Hime report finding new evidence for a 17-keV neutrino in the {beta} decay of {sup 3}H and {sup 35}S. New data from Los Alamos on the electron neutrino mass as measured in tritium beta decay give an upper limit of 13.5 eV at the 95% confidence level. This result is not consistent with the long-standing ITEP result of 26(5) eV within a model-independent'' range of 17 to 40 eV. It now appears that the electron neutrino is not sufficiently massive to close the universe by itself. 38 refs., 1 figs., 2 tabs.

Robertson, R.G.H.

1989-01-01

229

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

230

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

231

Cosmological and supernova neutrinos  

NASA Astrophysics Data System (ADS)

The Big Bang nucleosynthesis (BBN) and the cosmic microwave background (CMB) anisotropies are the pillars of modern cosmology. It has recently been suggested that axion which is a dark matter candidate in the framework of the standard model could condensate in the early universe and induce photon cooling before the epoch of the photon last scattering. Although this may render a solution to the overproduction problem of primordial 7Li abundance, there arises another serious difficulty of overproducing D abundance. We propose a hybrid dark matter model with both axions and relic supersymmetric (SUSY) particles to solve both overproduction problems of the primordial D and 7Li abundances simultaneously. The BBN also serves to constrain the nature of neutrinos. Considering non-thermal photons produced in the decay of the heavy sterile neutrinos due to the magnetic moment, we explore the cosmological constraint on the strength of neutrino magnetic moment consistent with the observed light element abundances. Core-collapse supernovae eject huge flux of energetic neutrinos which affect explosive nucleosynthesis of rare isotopes like 7Li, 11B, 92Nb, 138La and 180Ta and r-process elements. Several isotopes depend strongly on the neutrino flavor oscillation due to the Mikheyev-Smirnov-Wolfenstein (MSW) effect. Combining the recent experimental constraints on ?13 with predicted and observed supernova-produced abundance ratio 11B/7Li encapsulated in the presolar grains from the Murchison meteorite, we show a marginal preference for an inverted neutrino mass hierarchy. We also discuss supernova relic neutrinos (SRN) that may indicate the softness of the equation of state (EoS) of nuclear matter and adiabatic conditions of the neutrino oscillation.

Kajino, T.; Aoki, W.; Balantekin, A. B.; Cheoun, M.-K.; Hayakawa, T.; Hidaka, J.; Hirai, Y.; Kusakabe, M.; Mathews, G. J.; Nakamura, K.; Pehlivan, Y.; Shibagaki, S.; Suzuki, T.

2014-06-01

232

Supernova neutrino detection  

E-print Network

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

K. Scholberg

2007-01-04

233

The AMANDA neutrino telescope  

Microsoft Academic Search

With an effective telescope area of order 104 m2 for TeV neutrinos, a threshold near ?50 GeV and a pointing accuracy of 2.5 degrees per muon track, the AMANDA detector represents the first of a new generation of high energy neutrino telescopes, reaching a scale envisaged over 25 years ago. We describe early results on the calibration of natural deep

E. C. Andrés; P. Askebjer; S. W. Barwick; R. C. Bay; L. Bergström; A. Biron; J. Booth; O. Botner; A. Bouchta; S. Carius; M. Carlson; W. Chinowsky; D. Chirkin; J. Conrad; C. G. S. Costa; D. Cowen; E. Dalberg; T. De Young; J. Edsjö; P. Ekström; A. Goobar; L. Gray; A. Hallgren; F. Halzen; R. Hardtke; S. Hart; Y. He; C. P. de los Heros; G. Hill; P. O. Hulth; S. Hundertmark; J. Jacobsen; A. Jones; V. Kandhadai; A. Karle; J. Kim; H. Leich; M. Leuthold; P. Lindahl; I. Liubarsky; D. Lowder; P. Marciniewski; T. C. Miller; P. C. Mock; R. Morse; M. Newcomer; P. Niessen; D. Nygren; R. Porrata; D. Potter; P. B. Price; G. Przybylski; W. Rhode; S. Richter; J. Rodriguez; P. Romenesko; D. Ross; H. Rubinstein; T. Schmidt; E. Schneider; R. Schwarz; U. Schwendicke; G. Smoot; M. Solarz; V. Sorin; C. Spiering; P. Steffen; R. Stokstad; O. Streicher; I. Taboada; T. Thon; S. Tilav; C. Walck; C. H. Wiebusch; R. Wischnewski; K. Woschnagg; W. Wu; G. Yodh; S. Young

1999-01-01

234

The AMANDA neutrino telescope  

SciTech Connect

With an effective telescope area of order 10(4) m(2) for TeVneutrinos, a threshold near similar to 50 GeV and a pointing accuracy of2.5 degrees per muon track, the AMANDA detector represents the first of anew generation of high energy neutrino telescopes, reaching a scaleenvisaged over 25 years ago. We describe early results on the calibrationof natural deep ice as a particle detector as well as on AMANDA'sperformance as a neutrino telescope.

Andres, E.C.; Askebjer, P.; Barwick, S.W.; Bay, R.C.; Bergstrom,L.; Biron, A.; Booth, J.; Botner, O.; Bouchta, A.; Carius, S.; Carlson,M.; Chinowsky, W.; Chirkin, D.; Conrad,J.; Costa, C.G.S.; Cowen, D.; Dalberg, E.; DeYoung, T.; Edsjo, J.; Ekstrom, P.; Goobar, A.; Gray, L.; Hallgren, A.; Halzen, F.; Hardtke, R.; Hart, S.; He, Y.; de, los, Heros,C.P.; Hill, G.; Hulth, PO.; Hundertmark, S.; Jacobsen, J.; Jones, A.; Kandhadai, V.; Karle, A.; Kim, J.; Leich, H.; Leuthold, M.; Lindahl, P.; Liubarsky, I.; Loaiza, P.; Lowder, D.; Marciniewski, P.; Miller, T.C.; Miocinovic, P.; Mock, P.C.; Morse, R.; Newcomer, M.; Niessen, P.; Nygren,D.; Porrata, R.; Potter, D.; Price, P.B.; Przybylski, G.; Rhode, W.; Richter, S.; Rodriguez, J.; Romenesko, P.; Ross, D.; Rubinstein, H.; Schmidt, T.; Schneider, E.; Schwarz, R.; Schwendicke, U.; Smoot, G.; Solarz, M.; Sorin, V.; Spiering, C.; Steffen, P.; Stokstad, R.; Streicher, O.; Taboada, I.; Thon, T.; Tilav, S.; Walck, C.; Wiebusch,C.H.; Wischnewski, R.; Woschnagg, K.; Wu, W.; Yodh, G.; Young, S.; AMANDACollaboration

1999-04-01

235

Cosmological and supernova neutrinos  

SciTech Connect

The Big Bang nucleosynthesis (BBN) and the cosmic microwave background (CMB) anisotropies are the pillars of modern cosmology. It has recently been suggested that axion which is a dark matter candidate in the framework of the standard model could condensate in the early universe and induce photon cooling before the epoch of the photon last scattering. Although this may render a solution to the overproduction problem of primordial {sup 7}Li abundance, there arises another serious difficulty of overproducing D abundance. We propose a hybrid dark matter model with both axions and relic supersymmetric (SUSY) particles to solve both overproduction problems of the primordial D and {sup 7}Li abundances simultaneously. The BBN also serves to constrain the nature of neutrinos. Considering non-thermal photons produced in the decay of the heavy sterile neutrinos due to the magnetic moment, we explore the cosmological constraint on the strength of neutrino magnetic moment consistent with the observed light element abundances. Core-collapse supernovae eject huge flux of energetic neutrinos which affect explosive nucleosynthesis of rare isotopes like {sup 7}Li, {sup 11}B, {sup 92}Nb, {sup 138}La and {sup 180}Ta and r-process elements. Several isotopes depend strongly on the neutrino flavor oscillation due to the Mikheyev-Smirnov-Wolfenstein (MSW) effect. Combining the recent experimental constraints on ?{sub 13} with predicted and observed supernova-produced abundance ratio {sup 11}B/{sup 7}Li encapsulated in the presolar grains from the Murchison meteorite, we show a marginal preference for an inverted neutrino mass hierarchy. We also discuss supernova relic neutrinos (SRN) that may indicate the softness of the equation of state (EoS) of nuclear matter and adiabatic conditions of the neutrino oscillation.

Kajino, T. [National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan Department of Astronomy, University of Tokyo, Hongo 7-3-1, Bunkyo-ku, Tokyo 113-0033 (Japan); Aoki, W. [National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan); Balantekin, A. B. [Department of Physics, University of Wisconsin - Madison, Wisconsin 53706 (United States); Cheoun, M.-K. [Department of Physics, Soongsil University, Seoul 156-743 (Korea, Republic of); Hayakawa, T. [Japan Atomic Energy Agency, Shirakara-Shirane 2-4, Tokai-mura, Ibaraki 319-1195 (Japan); Hidaka, J. [National Astronomical Observatory, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan); Hirai, Y.; Shibagaki, S. [National Astronomical Observatory, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan and Department of Astronomy, University of Tokyo, Hongo 7-3-1, Bunkyo-ku, Tokyo 113-0033 (Japan); Kusakabe, M. [School of Liberal Arts and Science, Korea Aerospace University, Goyang 412-791 (Korea, Republic of); Mathews, G. J. [Department of Physics, University of Notre Dame, IN 46556 (United States); Nakamura, K. [Waseda University, Ohkubo 3-4-1, Shinjuku, Tokyo 169-8555 (Japan); Pehlivan, Y. [Mimar Sinan GSÜ, Department of Physics, ?i?li, ?stanbul 34380 (Turkey); Suzuki, T. [Nihon University, Sakurajosui 3-25-40, Setagaya-ku, Tokyo 156-8550 (Japan)

2014-06-24

236

Helicity of Neutrinos  

Microsoft Academic Search

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

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

1958-01-01

237

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

238

The Sudbury Neutrino Observatory  

SciTech Connect

Two experiments now in progress have reported measurements of the flux of high energy neutrinos from the Sun. Since about 1970, Davis and his co-workers have been using a [sup 37]Cl-based detector to measure the [sup 7]Be and [sup 8]B solar neutrino flux and have found it to be at least a factor of three lower than that predicted by the Standard Solar Model (SSM). The Kamiokande collaborations has been taking data since 1986 using a large light-water Cerenkov detector and have confirmed that the flux is about two times lower than predicted. Recent results from the SAGE and GALLEX gallium-based detectors show that there is also a deficit of the low energy pp solar neutrinos. These discrepancies between experiment and theory could arise because of inadequacies in the theoretical models of solar energy generation or because of previously unobserved properties of neutrinos. The Sudbury Neutrino Observatory (SNO) will provide the information necessary to decide which of these solutions to the solar neutrino problem'' is correct.

Norman, E.B.; Chan, Y.D.; Garcia, A.; Lesko, K.T.; Smith, A.R.; Stokstad, R.G.; Zlimen, I. (Lawrence Berkeley Lab., CA (United States)); Evans, H.C.; Ewan, G.T.; Hallin, A.; Lee, H.W.; Leslie, J.R.; MacArthur, J.D.; Mak, H.B.; McDonald, A.B.; McLatchie, W.; Robertson, B.C.; Skensved, P.; Sur, B. (Queen's Univ., Kingston, ON (Canada). Dept. of Physics); Bonvin, E.; Earle, E.D.; Hepburn, D.; Milton, G.M. (Atomic Energ

1992-11-01

239

Search for a Light Sterile Neutrino at Daya Bay  

E-print Network

A search for light sterile neutrino mixing was performed with the first 217 days of data from the Daya Bay Reactor Antineutrino Experiment. The experiment's unique configuration of multiple baselines from six 2.9~GW$_{\\rm th}$ nuclear reactors to six antineutrino detectors deployed in two near (effective baselines 512~m and 561~m) and one far (1579~m) underground experimental halls makes it possible to test for oscillations to a fourth (sterile) neutrino in the $10^{\\rm -3}~{\\rm eV}^{2} < |\\Delta m_{41}^{2}| < 0.3~{\\rm eV}^{2}$ range. The relative spectral distortion due to electron antineutrino disappearance was found to be consistent with that of the three-flavor oscillation model. The derived limits on $\\sin^22\\theta_{14}$ cover the $10^{-3}~{\\rm eV}^{2} \\lesssim |\\Delta m^{2}_{41}| \\lesssim 0.1~{\\rm eV}^{2}$ region, which was largely unexplored.

F. P. An; A. B. Balantekin; H. R. Band; W. Beriguete; M. Bishai; S. Blyth; I. Butorov; G. F. Cao; J. Cao; Y. L. Chan; J. F. Chang; L. C. Chang; Y. Chang; C. Chasman; H. Chen; Q. Y. Chen; S. M. Chen; X. Chen; X. Chen; Y. X. Chen; Y. Chen; Y. P. Cheng; J. J. Cherwinka; M. C. Chu; J. P. Cummings; J. de Arcos; Z. Y. Deng; Y. Y. Ding; M. V. Diwan; E. Draeger; X. F. Du; D. A. Dwyer; W. R. Edwards; S. R. Ely; J. Y. Fu; L. Q. Ge; R. Gill; M. Gonchar; G. H. Gong; H. Gong; M. Grassi; W. Q. Gu; M. Y. Guan; X. H. Guo; R. W. Hackenburg; G. H. Han; S. Hans; M. He; K. M. Heeger; Y. K. Heng; P. Hinrichs; Y. K. Hor; Y. B. Hsiung; B. Z. Hu; L. M. Hu; L. J. Hu; T. Hu; W. Hu; E. C. Huang; H. Huang; X. T. Huang; P. Huber; G. Hussain; Z. Isvan; D. E. Jaffe; P. Jaffke; K. L. Jen; S. Jetter; X. P. Ji; X. L. Ji; H. J. Jiang; J. B. Jiao; R. A. Johnson; L. Kang; S. H. Kettell; M. Kramer; K. K. Kwan; M. W. Kwok; T. Kwok; W. C. Lai; K. Lau; L. Lebanowski; J. Lee; R. T. Lei; R. Leitner; A. Leung; J. K. C. Leung; C. A. Lewis; D. J. Li; F. Li; G. S. Li; Q. J. Li; W. D. Li; X. N. Li; X. Q. Li; Y. F. Li; Z. B. Li; H. Liang; C. J. Lin; G. L. Lin; P. Y. Lin; S. K. Lin; Y. C. Lin; J. J. Ling; J. M. Link; L. Littenberg; B. R. Littlejohn; D. W. Liu; H. Liu; J. L. Liu; J. C. Liu; S. S. Liu; Y. B. Liu; C. Lu; H. Q. Lu; K. B. Luk; Q. M. Ma; X. Y. Ma; X. B. Ma; Y. Q. Ma; K. T. McDonald; M. C. McFarlane; R. D. McKeown; Y. Meng; I. Mitchell; J. Monari Kebwaro; Y. Nakajima; J. Napolitano; D. Naumov; E. Naumova; I. Nemchenok; H. Y. Ngai; Z. Ning; J. P. Ochoa-Ricoux; A. Olshevski; S. Patton; V. Pec; J. C. Peng; L. E. Piilonen; L. Pinsky; C. S. J. Pun; F. Z. Qi; M. Qi; X. Qian; N. Raper; B. Ren; J. Ren; R. Rosero; B. Roskovec; X. C. Ruan; B. B. Shao; H. Steiner; G. X. Sun; J. L. Sun; Y. H. Tam; X. Tang; H. Themann; K. V. Tsang; R. H. M. Tsang; C. E. Tull; Y. C. Tung; B. Viren; V. Vorobel; C. H. Wang; L. S. Wang; L. Y. Wang; M. Wang; N. Y. Wang; R. G. Wang; W. Wang; W. W. Wang; X. Wang; Y. F. Wang; Z. Wang; Z. Wang; Z. M. Wang; D. M. Webber; H. Y. Wei; Y. D. Wei; L. J. Wen; K. Whisnant; C. G. White; L. Whitehead; T. Wise; H. L. H. Wong; S. C. F. Wong; E. Worcester; Q. Wu; D. M. Xia; J. K. Xia; X. Xia; Z. Z. Xing; J. Y. Xu; J. L. Xu; J. Xu; Y. Xu; T. Xue; J. Yan; C. C. Yang; L. Yang; M. S. Yang; M. T. Yang; M. Ye; M. Yeh; Y. S. Yeh; B. L. Young; G. Y. Yu; J. Y. Yu; Z. Y. Yu; S. L. Zang; B. Zeng; L. Zhan; C. Zhang; F. H. Zhang; J. W. Zhang; Q. M. Zhang; Q. Zhang; S. H. Zhang; Y. C. Zhang; Y. M. Zhang; Y. H. Zhang; Y. X. Zhang; Z. J. Zhang; Z. Y. Zhang; Z. P. Zhang; J. Zhao; Q. W. Zhao; Y. Zhao; Y. B. Zhao; L. Zheng; W. L. Zhong; L. Zhou; Z. Y. Zhou; H. L. Zhuang; J. H. Zou

2014-10-08

240

Search for a light sterile neutrino at Daya Bay.  

PubMed

A search for light sterile neutrino mixing was performed with the first 217 days of data from the Daya Bay Reactor Antineutrino Experiment. The experiment's unique configuration of multiple baselines from six 2.9 GW(th) nuclear reactors to six antineutrino detectors deployed in two near (effective baselines 512 m and 561 m) and one far (1579 m) underground experimental halls makes it possible to test for oscillations to a fourth (sterile) neutrino in the 10(-3) eV(2)<|?m(41)(2) |< 0.3 eV(2) range. The relative spectral distortion due to the disappearance of electron antineutrinos was found to be consistent with that of the three-flavor oscillation model. The derived limits on sin(2) 2?(14) cover the 10(-3) eV(2) ? |?m(41)(2)| ? 0.1 eV(2) region, which was largely unexplored. PMID:25325631

An, F P; Balantekin, A B; Band, H R; Beriguete, W; Bishai, M; Blyth, S; Butorov, I; Cao, G F; Cao, J; Chan, Y L; Chang, J F; Chang, L C; Chang, Y; Chasman, C; Chen, H; Chen, Q Y; Chen, S M; Chen, X; Chen, X; Chen, Y X; Chen, Y; Cheng, Y P; Cherwinka, J J; Chu, M C; Cummings, J P; de Arcos, J; Deng, Z Y; Ding, Y Y; Diwan, M V; Draeger, E; Du, X F; Dwyer, D A; Edwards, W R; Ely, S R; Fu, J Y; Ge, L Q; Gill, R; Gonchar, M; Gong, G H; Gong, H; Grassi, M; Gu, W Q; Guan, M Y; Guo, X H; Hackenburg, R W; Han, G H; Hans, S; He, M; Heeger, K M; Heng, Y K; Hinrichs, P; Hor, Y K; Hsiung, Y B; Hu, B Z; Hu, L M; Hu, L J; Hu, T; Hu, W; Huang, E C; Huang, H; Huang, X T; Huber, P; Hussain, G; Isvan, Z; Jaffe, D E; Jaffke, P; Jen, K L; Jetter, S; Ji, X P; Ji, X L; Jiang, H J; Jiao, J B; Johnson, R A; Kang, L; Kettell, S H; Kramer, M; Kwan, K K; Kwok, M W; Kwok, T; Lai, W C; Lau, K; Lebanowski, L; Lee, J; Lei, R T; Leitner, R; Leung, A; Leung, J K C; Lewis, C A; Li, D J; Li, F; Li, G S; Li, Q J; Li, W D; Li, X N; Li, X Q; Li, Y F; Li, Z B; Liang, H; Lin, C J; Lin, G L; Lin, P Y; Lin, S K; Lin, Y C; Ling, J J; Link, J M; Littenberg, L; Littlejohn, B R; Liu, D W; Liu, H; Liu, J L; Liu, J C; Liu, S S; Liu, Y B; Lu, C; Lu, H Q; Luk, K B; Ma, Q M; Ma, X Y; Ma, X B; Ma, Y Q; McDonald, K T; McFarlane, M C; McKeown, R D; Meng, Y; Mitchell, I; Monari Kebwaro, J; Nakajima, Y; Napolitano, J; Naumov, D; Naumova, E; Nemchenok, I; Ngai, H Y; Ning, Z; Ochoa-Ricoux, J P; Olshevski, A; Patton, S; Pec, V; Peng, J C; Piilonen, L E; Pinsky, L; Pun, C S J; Qi, F Z; Qi, M; Qian, X; Raper, N; Ren, B; Ren, J; Rosero, R; Roskovec, B; Ruan, X C; Shao, B B; Steiner, H; Sun, G X; Sun, J L; Tam, Y H; Tang, X; Themann, H; Tsang, K V; Tsang, R H M; Tull, C E; Tung, Y C; Viren, B; Vorobel, V; Wang, C H; Wang, L S; Wang, L Y; Wang, M; Wang, N Y; Wang, R G; Wang, W; Wang, W W; Wang, X; Wang, Y F; Wang, Z; Wang, Z; Wang, Z M; Webber, D M; Wei, H Y; Wei, Y D; Wen, L J; Whisnant, K; White, C G; Whitehead, L; Wise, T; Wong, H L H; Wong, S C F; Worcester, E; Wu, Q; Xia, D M; Xia, J K; Xia, X; Xing, Z Z; Xu, J Y; Xu, J L; Xu, J; Xu, Y; Xue, T; Yan, J; Yang, C C; Yang, L; Yang, M S; Yang, M T; Ye, M; Yeh, M; Yeh, Y S; Young, B L; Yu, G Y; Yu, J Y; Yu, Z Y; Zang, S L; Zeng, B; Zhan, L; Zhang, C; Zhang, F H; Zhang, J W; Zhang, Q M; Zhang, Q; Zhang, S H; Zhang, Y C; Zhang, Y M; Zhang, Y H; Zhang, Y X; Zhang, Z J; Zhang, Z Y; Zhang, Z P; Zhao, J; Zhao, Q W; Zhao, Y; Zhao, Y B; Zheng, L; Zhong, W L; Zhou, L; Zhou, Z Y; Zhuang, H L; Zou, J H

2014-10-01

241

GENIUS project, neutrino oscillations and Cosmology neutrinos reveal their nature?  

E-print Network

The neutrinoless double beta decay as well as any other laboratory experiment has not been able to answer the question of the neutrino's nature. Hints on the answer are available when neutrino oscillations and $(\\beta\\beta)_{0 \

Czakon, M; Zralek, M; Gluza, J

2000-01-01

242

GENIUS project, neutrino oscillations and Cosmology: neutrinos reveal their nature?  

E-print Network

The neutrinoless double beta decay as well as any other laboratory experiment has not been able to answer the question of the neutrino's nature. Hints on the answer are available when neutrino oscillations and $(\\beta\\beta)_{0 \

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

2000-05-17

243

Core-collapse supernova neutrinos and neutrino properties  

E-print Network

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

J. Gava; C. Volpe

2008-05-18

244

Measurement of Atmospheric Neutrinos at the Sudbury Neutrino Observatory  

E-print Network

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

Formaggio, Joseph A.

245

Sterile Neutrino Fits to Short-Baseline Neutrino Oscillation Measurements  

E-print Network

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

Conrad, J. M.

2013-01-01

246

No-neutrino double beta decay: more than one neutrino  

SciTech Connect

Interference effects between light and heavy Majorana neutrinos in the amplitude for no-neutrino double beta decay are discussed. The effects include an upper bound on the heavy neutrino mass, and an A dependence for the effective mass extracted from double beta decay. Thus the search for the no-neutrino decay mode should be pursued in several nuclei, and particularly in Ca/sup 48/, where the effective mass may be quite large.

Rosen, S.P.

1983-01-01

247

Envelope instability and the fourth order resonance  

NASA Astrophysics Data System (ADS)

The well-known envelope instability or the second order even collective mode [I. Hofmann, Phys. Rev. E 57, 4 (1998)] and the fourth order resonance 4 ? =360 ° due to the nonlinear space charge effect in high intensity beams have been studied previously. A wide stop band around 15° is found in a pure periodic focusing channel. In addition, it is illustrated that the fourth order resonance dominates over the envelope instability and practically replaces it in the stop band [D. Jeon et al., Phys. Rev. ST Accel. Beams 12, 054204 (2009)]. In this paper, for a continuous beam with remarkable space charge, our 2D self-consistent particle-in-cell simulation work with the code topopic shows these two kinds of effects respectively in a periodic focusing defocusing (FD) channel. For a fixed tune depression ? =0.8 , a stop band with a width of almost 15° is also demonstrated. Moreover, it is confirmed that analytical results of the rms envelope instability diagram are a valid tool to interpret the width of the stop band. Emittance growth rates in stop band are also well explained. It is found that, for a nearly rms matched beam, the emittance growth in the stop band is almost proportional to the saturation time of the nonlinear instability of the envelope, which happens in a quick manner and takes only a few FD cells. In contrast, the fourth order resonance is independent of rms matching and will be accompanied by beam evolution as "a long term effect" once the related mechanism is excited.

Li, Chao; Zhao, Ya Liang

2014-12-01

248

Fourth International Symposium on Magnetic Suspension Technology  

NASA Technical Reports Server (NTRS)

In order to examine the state of technology of all areas of magnetic suspension and to review recent developments in sensors, controls, superconducting magnet technology, and design/implementation practices, the Fourth International Symposium on Magnetic Suspension Technology was held at The Nagaragawa Convention Center in Gifu, Japan, on October 30 - November 1, 1997. The symposium included 13 sessions in which a total of 35 papers were presented. The technical sessions covered the areas of maglev, controls, high critical temperature (T(sub c)) superconductivity, bearings, magnetic suspension and balance systems (MSBS), levitation, modeling, and applications. A list of attendees is included in the document.

Groom, Nelson J. (Editor); Britcher, Colin P. (Editor)

1998-01-01

249

Atmospheric neutrinos in ice and measurement of neutrino oscillation parameters  

SciTech Connect

The main goal of the IceCube Deep Core array is to search for neutrinos of astrophysical origins. Atmospheric neutrinos are commonly considered as a background for these searches. We show that the very high statistics atmospheric neutrino data can be used to obtain precise measurements of the main oscillation parameters.

Fernandez-Martinez, Enrique [Max-Planck-Institut fuer Physik (Werner-Heisenberg-Institut), Foehringer Ring 6, 80805 Muenchen (Germany); Giordano, Gerardo; Mocioiu, Irina [Department of Physics, Pennsylvania State University, University Park, Pennsylvania 16802 (United States); Mena, Olga [Instituto de Fisica Corpuscular, IFIC, CSIC, and Universidad de Valencia (Spain)

2010-11-01

250

The Neutrino Eye: A Megaton Low Energy Neutrino  

E-print Network

from WIMPS and gamma ray bursts, and upon real time counting of solar neutrinos, are all from sensi­ tivity, and conduct a watch for for neutrino correlates to sporadic phenomenon such as gamma ray bursts. The main thrust would be to detect actual muon neutrino appearance as well as disappearance

Learned, John

251

Vetoing atmospheric neutrinos in a high energy neutrino telescope  

E-print Network

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

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

2008-12-22

252

Formation of Neutrino Stars from Cosmological Background Neutrinos  

E-print Network

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

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

2006-09-20

253

Neutrino oscillometry at the next generation neutrino observatory  

Microsoft Academic Search

The large next generation liquid-scintillator detector LENA (Low Energy Neutrino Astronomy) offers an excellent opportunity for neutrino oscillometry. The characteristic spatial pattern of very low monoenergetic neutrino disappearance from artificial radioactive sources can be detected within the long length of detector. Sufficiently strong sources of more than 1 MCi activity can be produced at nuclear reactors. Oscillometry will provide a

Yu. N. Novikov; T. Enqvist; A. N. Erykalov; F. v. Feilitzsch; J. Hissa; K. Loo; D. A. Nesterenko; L. Oberauer; F. Thorne; W. Trzaska; J. D. Vergados; M. Wurm

2011-01-01

254

Secondary atmospheric tau neutrino production  

SciTech Connect

We evaluate the flux of tau neutrinos produced from the decay of pair produced taus from incident muons using a cascade equation analysis. To solve the cascade equations, our numerical result for the tau production Z moment is given. Our results for the flux of tau neutrinos produced from incident muons are compared to the flux of tau neutrinos produced via oscillations and the direct prompt atmospheric tau neutrino flux. Results are given for both downward and upward going neutrinos fluxes and higher zenith angles are discussed. We conclude that the direct prompt atmospheric tau neutrino flux dominates these other atmospheric sources of tau neutrinos for neutrino energies larger than a few TeV for upward fluxes, and over a wider range of energy for downward fluxes.

Bulmahn, Alexander; Hall Reno, Mary [Department of Physics and Astronomy, University of Iowa, Iowa City, Iowa 52242 (United States)

2010-09-01

255

Simulating nonlinear neutrino flavor evolution  

E-print Network

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

Huaiyu Duan; George M. Fuller; J. Carlson

2008-03-26

256

Local demands on sterile neutrinos  

E-print Network

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

David C. Latimer; David J. Ernst

2005-12-13

257

Steps towards the Neutrino Factory  

NASA Astrophysics Data System (ADS)

The properties of the neutrino provide a unique window on physics beyond that described by the Standard Model. The study of sub-leading effects in neutrino oscillations has begun with the race to measure ?13. A consensus is emerging within the international community that a novel neutrino source is required to allow sensitive searches for leptonic CP violation to be carried out and the neutrino mass-hierarchy to be determined. The Neutrino Factory, in which intense neutrino beams are produced from the decay of muons, has been shown to out-perform the other proposed facilities. The physics case for the Neutrino Factory will be reviewed and the baseline design of the facility being developed by the International Design Study for the Neutrino Factory (the IDS-NF) collaboration will be described.

Long, K.

2012-08-01

258

Neutrino Factory: status and prospects  

NASA Astrophysics Data System (ADS)

The properties of the neutrino provide a unique window on physics beyond that described by the Standard Model. The study of sub-leading effects in neutrino oscillations has begun with the race to measure ? consensus is emerging within the international community that a novel neutrino source is required to allow sensitive searches for leptonic CP violation to be carried out and the neutrino mass-hierarchy to be determined. The Neutrino Factory, in which intense neutrino beams are produced from the decay of muons, has been shown to out-perform the other proposed facilities. The physics case for the Neutrino Factory will be reviewed and the baseline design of the facility being developed by the International Design Study for the Neutrino Factory (the IDS-NF) collaboration will be described.

Long, K.

2011-08-01

259

Neutrino dispersion in magnetized plasma  

E-print Network

The neutrino dispersion in the charge symmetric magnetized plasma is investigated. We have studied the plasma contribution into the additional energy of neutrino and obtained the simple expression for it. We consider in detail the neutrino self-energy under physical conditions of weak field, moderate field and strong field limits. It is shown that our result for neutrino dispersion in moderate magnetic field differ substantially from the previous one in the literature.

N. V. Mikheev; E. N. Narynskaya

2008-12-02

260

Electromagnetic neutrino: a short review  

E-print Network

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

Alexander I. Studenikin

2014-11-09

261

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

262

Are there atmospheric neutrino oscillations?  

SciTech Connect

The neutrino oscillation explanation ({nu}{sub {mu}} {yields} {nu}{sub {tau}}) of the atmospheric neutrino deficit is often discussed but is far from widely accepted. This paper discusses several experimental observations, and how a consistent picture pointing towards neutrino oscillations might develop.

Goodman, M.C.

1993-06-01

263

Supernova Neutrinos Detection On Earth  

E-print Network

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

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

2009-05-12

264

Solar Neutrino Matter Effects Redux  

E-print Network

Following recent low-threshold analysis of the Sudbury Neutrino Observatory and asymmetry measurements of the BOREXINO Collaboration of the solar neutrino flux, we revisit the analysis of the matter effects in the Sun. We show that solar neutrino data constrains the mixing angle $\\theta_{13}$ poorly and that subdominant Standard Model effects can mimic the effects of the physics beyond the Standard Model.

A. B. Balantekin; A. Malkus

2011-12-19

265

Neutrino Factory: status and prospects  

Microsoft Academic Search

The properties of the neutrino provide a unique window on physics beyond that described by the Standard Model. The study of sub-leading effects in neutrino oscillations has begun with the race to measure theta consensus is emerging within the international community that a novel neutrino source is required to allow sensitive searches for leptonic CP violation to be carried out

K. Long

2011-01-01

266

Neutrino oscillations: brief history and present status  

E-print Network

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

S. M. Bilenky

2014-08-12

267

Relating quark mixing neutrino mixing and {delta}{sub lep}  

SciTech Connect

It is proposed that all flavor mixing is caused by the mixing of the three quark and lepton families with vectorlike fermions in 5+5-bar multiplets of SU(5). The entire 3 Multiplication-Sign 3 complex mass matrix of the neutrinos M{sub {nu}} is then found to have a simple expression in terms of two complex parameters and an overall scale. Thus, all the presently unknown neutrino parameters are predicted. The best fits are for {theta}{sub atm} Less-Than-Or-Equivalent-To 40 Degree-Sign The leptonic Dirac CP phase is found to be somewhat greater than {pi}.

Barr, S. M.; Chen Hengyu [Department of Physics and Astronomy, University of Delaware (United States)

2013-05-23

268

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

269

Child Care and Child Welfare. Joint Hearing before the Subcommittee on Human Resources of the Committee on Ways and Means and the Subcommittee on Early Childhood, Youth, and Families of the Committee on Economic and Educational Opportunities. House of Representatives, One Hundred Fourth Congress, First Session.  

ERIC Educational Resources Information Center

This document outlines the joint hearing before the House of Representatives, between the Committee on Ways and Means, Subcommittee on Human Resources and the Committee on Economic and Educational Opportunities, Subcommittee on Early Childhood, Youth and Families. The hearing was scheduled out of concern by Congress members over the proliferation…

Congress of the U.S., Washington, DC. House Committee on Ways and Means.

270

Limits on neutrino-neutrino scattering in the early Universe  

NASA Astrophysics Data System (ADS)

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

Cyr-Racine, Francis-Yan; Sigurdson, Kris

2014-12-01

271

Family Secrets  

Microsoft Academic Search

The purpose of this article is to provide an overview of the literature that reveals extensive classifications of the family secrets. The review includes definitions, comparisons of family secrecy to family privacy, types of family secrets, reasons why families avoid exposing certain activities, and factors contributing to the maintenance of a secret. The disclosing of hidden information is discussed with

NAIMA BROWN-SMITH

1998-01-01

272

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

SciTech Connect

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

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

2011-10-01

273

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

274

Black rings with fourth dipole cause less hair loss  

E-print Network

An example of entropy enigma with a controlled CFT dual was recently studied in arXiv:1108.0411. 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 arXiv:1201.2585. 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.

Borun D. Chowdhury

2012-11-05

275

Implications of Neutrino Oscillations on the Dark-Matter World  

NASA Astrophysics Data System (ADS)

According to my own belief that "The God wouldn't create a world that is so boring that a particle knows only the very feeble weak interaction.", maybe we underestimate the roles of neutrinos. We note that right-handed neutrinos play no roles, or don't exist, in the minimal Standard Model. We discuss the language to write down an extended Standard Model - using renormalizable quantum field theory as the language; to start with a certain set of basic units under a certain gauge group; in fact, to use the three right-handed neutrinos to initiate the family gauge group SUf(3). Specifically we use the left-handed and right-handed spinors to form the basic units together with SUc(3)×SUL(2)×U(1)×SUf(3) as the gauge group. The dark-matter SUf(3) world couples with the lepton world, but not with the quark world. Amazingly enough, the space of the Standard-Model Higgs ?(1,2), the family Higgs triplet ?(3, 1), and the neutral part of the mixed family Higgs ?0(3,2) undergoes the spontaneous symmetry breaking, i.e. the Standard-Model Higgs mechanism and the "project-out" family Higgs mechanism, to give rise to the weak bosons W± and Z0, one Standard-Model Higgs, the eight massive family gauge bosons, and the remaining four massive neutral family Higgs particles, and nothing more. Thus, the roles of neutrinos in this extended Standard Model are extremely interesting in connection with the dark-matter world.

Hwang, W.-Y. Pauchy

2014-01-01

276

Entanglement in neutrino oscillations  

E-print Network

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

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

2009-04-17

277

Popcorn Neutrino Lab  

NSDL National Science Digital Library

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

Jason Petula

278

Are neutrinos their own antiparticles?  

SciTech Connect

We explain the relationship between Majorana neutrinos, which are their own antiparticles, and Majorana neutrino masses. We point out that Majorana masses would make the neutrinos very distinctive particles, and explain why many theorists strongly suspect that neutrinos do have Majorana masses. The promising approach to confirming this suspicion is to seek neutrinoless double beta decay. We introduce a toy model that illustrates why this decay requires nonzero neutrino masses, even when there are both right-handed and left-handed weak currents.

Kayser, Boris; /Fermilab

2009-03-01

279

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

280

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

281

Neutrino Physics: A Selective Overview  

E-print Network

Neutrinos in the Standard Model of particle physics are massless, neutral fermions that seemingly do little more than conserve 4-momentum, angular momentum, lepton number, and lepton flavour in weak interactions. In the last decade conclusive evidence has demonstrated that the Standard Model's description of neutrinos does not match reality. We now know that neutrinos undergo flavour oscillations, violating lepton flavour conservation and implying that neutrinos have non-zero mass. A rich oscillation phenomenology then becomes possible, including matter-enhanced oscillation and possibly CP violation in the neutrino sector. Extending the Standard Model to include neutrino masses requires the addition of new fields and mass terms, and possibly new methods of mass generation. In this review article I will discuss the evidence that has established the existence of neutrino oscillation, and then highlight unresolved issues in neutrino physics, such as the nature of three-generational mixing (including CP-violating effects), the origins of neutrino mass, the possible existence of light sterile neutrinos, and the difficult question of measuring the absolute mass scale of neutrinos.

Scott M. Oser

2006-04-11

282

Family History  

MedlinePLUS

Your family history includes health information about you and your close relatives. Families have many factors in common, including their genes, ... as heart disease, stroke, and cancer. Having a family member with a disease raises your risk, but ...

283

Solar neutrino experiments  

Microsoft Academic Search

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

John Bahcall

1978-01-01

284

Fourth International Symposium Computational Methods in Toxicology and Pharmacology  

E-print Network

Fourth International Symposium Computational Methods in Toxicology and Pharmacology Integrating-Chemical Pharmacology of RAS, Russia) A. Lagunin (Institute of Biomedical Chemistry of RAMS, Russia ) A. Lisitsa

Ferreira, Márcia M. C.

285

95. ROOM 402 (LAW LIBRARY), EAST WING, FOURTH FLOOR, LOOKING ...  

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

95. ROOM 402 (LAW LIBRARY), EAST WING, FOURTH FLOOR, LOOKING SOUTHEAST - Smithsonian Institution Building, 1000 Jefferson Drive, between Ninth & Twelfth Streets, Southwest, Washington, District of Columbia, DC

286

Symmetries in collective neutrino oscillations  

E-print Network

We discuss the relationship between a symmetry in the neutrino flavour evolution equations and neutrino flavour oscillations in the collective precession mode. This collective precession mode can give rise to spectral swaps (splits) when conditions can be approximated as homogeneous and isotropic. Multi-angle numerical simulations of supernova neutrino flavour transformation show that when this approximation breaks down, non-collective neutrino oscillation modes decohere kinematically, but the collective precession mode still is expected to stand out. We provide a criterion for significant flavour transformation to occur if neutrinos participate in a collective precession mode. This criterion can be used to understand the suppression of collective neutrino oscillations in anisotropic environments in the presence of a high matter density. This criterion is also useful in understanding the breakdown of the collective precession mode when neutrino densities are small.

Huaiyu Duan; George M. Fuller; Yong-Zhong Qian

2009-07-31

287

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

E-print Network

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

Boyer, Edmond

288

Nonstandard neutrino interactions and transition magnetic moments  

DOE PAGESBeta

We constrain generic nonstandard neutrino interactions with existing experimental data on neutrino transition magnetic moments and derive strong bounds on tensorial couplings of neutrinos to charged fermions. We also discuss how some of these tensorial couplings can be constrained by other experiments, e.g., on neutrino-electron and neutrino-nucleus scattering.

Healey, Kristopher J.; Petrov, Alexey A.; Zhuridov, Dmitry

2013-06-01

289

Neutrinoless double beta decay and neutrino physics  

E-print Network

The connection of neutrino physics with neutrinoless double beta decay is reviewed. After presenting the current status of the PMNS matrix and the theoretical background of neutrino mass and lepton mixing, we will summarize the various implications of neutrino physics for double beta decay. The influence of light sterile neutrinos and other exotic modifications of the three neutrino picture is also discussed.

Werner Rodejohann

2012-08-20

290

Neutrinos from a core collapse supernova  

E-print Network

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

Amol Dighe

2007-12-28

291

The JHF-Kamioka neutrino project  

Microsoft Academic Search

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

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

2001-01-01

292

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

293

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

E-print Network

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

Debasish Majumdar

2006-07-31

294

Neutrino Event Generators  

SciTech Connect

A brief description of recent progress in NEUGEN improvements is given. Comparison of various neutrino event generators based on a previous study is also made. Existing event generator models differ most strongly in the treatment of nuclear fsi, the focus of the paper.

Dytman, Steven [Dept. of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260 (United States)

2007-03-19

295

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

296

Neutrino and it's lepton  

E-print Network

In this paper I cite p.p. 100-117 of book G. Quznetsov, Probabilistic Treatment of Gauge Theories, in series Contemporary Fundamental Physics,ed. V. Dvoeglazov, Nova Sci. Publ., NY (2007). There I research a bound between neutrino and it's lepton.

G. Quznetsov

2008-11-10

297

Neutrino Factory Downstream Systems  

SciTech Connect

We describe the Neutrino Factory accelerator systems downstream from the target and capture area. These include the bunching and phase rotation, cooling, acceleration, and decay ring systems. We also briefly discuss the R&D program under way to develop these systems, and indicate areas where help from CERN would be invaluable.

Zisman, Michael S.

2009-12-23

298

Solar neutrinos at Super-Kamiokande: Solving the solar neutrino puzzle via neutrino flavor oscillations  

NASA Astrophysics Data System (ADS)

The Super-Kamiokande neutrino detector was built with the intent to explain the long-standing apparent solar neutrino flux deficit through signatures of neutrino flavor oscillations, such as a distortion in the energy spectrum and an asymmetry in the day and night fluxes. With the absence of any such "smoking-gun" evidence, an oscillation analysis of solar neutrinos was performed using the data sample from Super-Kamiokande I (SK), Sudbury Neutrino Observatory (SNO), and all other neutrino detectors. A model-independent analysis of SK's total solar neutrino rate and SNO's solar electron-neutrino rate showed at 3.7 sigma level that the apparent deficit is due to the effects of neutrino flavor oscillations. This analysis was possible because for a careful choice of energy thresholds, SK and SNO have virtually the same response to 8B solar neutrinos, whose energy spectrum is undistorted, as demonstrated by the data. By utilizing the full data sets of SK and SNO, however, the oscillation scenario is favored at 6.0 sigma level, with the best-fit oscillation parameters of Deltam2 = 6.3 x 10-5 eV2 and tan 2theta = 0.44 (in the LMA region). The measured 8B neutrino flux is phinu = 5.45+0.64-0.69 x 106 cm-2s-1 , which confirms its theoretical prediction from the Standard Solar Model. With the addition of the neutrino rates from the radiochemical experiments (gallium and chlorine), and the anti-neutrino oscillation result from KamLAND, the LMA solution is further constricted, the 8B neutrino flux is again confirmed (phinu = 5.66+0.62-0.59 x 106 cm-2s -1), and the no-oscillation scenario is ruled out at more than 10 sigma level.

Turcan, Dusan

299

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

2007-12-01

300

Pseudo-dirac neutrinos: a challenge for neutrino telescopes.  

PubMed

Neutrinos may be pseudo-Dirac states, such that each generation is actually composed of two maximally mixed Majorana neutrinos separated by a tiny mass difference. The usual active neutrino oscillation phenomenology would be unaltered if the pseudo-Dirac splittings are deltam(2) less, similar 10(-12) eV(2); in addition, neutrinoless double beta decay would be highly suppressed. However, it may be possible to distinguish pseudo-Dirac from Dirac neutrinos using high-energy astrophysical neutrinos. By measuring flavor ratios as a function of L/E, mass-squared differences down to deltam(2) approximately 10(-18) eV(2) can be reached. We comment on the possibility of probing cosmological parameters with neutrinos. PMID:14753977

Beacom, John F; Bell, Nicole F; Hooper, Dan; Learned, John G; Pakvasa, Sandip; Weiler, Thomas J

2004-01-01

301

Measurement of Atmospheric Neutrino Oscillations with the ANTARES Neutrino Telescope  

E-print Network

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

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

2012-07-02

302

Family Privilege  

ERIC Educational Resources Information Center

Family privilege is defined as "strengths and supports gained through primary caring relationships." A generation ago, the typical family included two parents and a bevy of kids living under one roof. Now, every variation of blended caregiving qualifies as family. But over the long arc of human history, a real family was a…

Seita, John R.

2014-01-01

303

Human Resources Administration: A School-Based Perspective. Fourth Edition  

ERIC Educational Resources Information Center

Enhanced and updated, this Fourth Edition of Richard E. Smith's highly successful text examines the growing role of the principal in planning, hiring, staff development, supervision, and other human resource functions. The Fourth Edition includes new sections on ethics, induction, and the role of the mentor teacher. This edition also introduces…

Smith, Richard

2009-01-01

304

Department of Obstetrics and Gynecology Fourth Year Student Evaluation Form  

E-print Network

Department of Obstetrics and Gynecology Fourth Year Student Evaluation Form Student: _____________________________ , M.D. Please complete the following form with your assessment of the fourth year medical student" Patient Education Response to Organization/Time constructive feedback management Ability to get things

305

Reading To Learn: Lessons from Exemplary Fourth-Grade Classrooms.  

ERIC Educational Resources Information Center

Fourth graders around the country face new, high-stakes standardized tests, drawing increased attention to the need for effective literacy instruction in the upper elementary grades. This book goes beyond "political catch phrases" to examine what actually works in the fourth-grade classroom. The book offers a view of the techniques and strategies…

Allington, Richard L.; Johnston, Peter H.

306

Pizza Anyone? Exploring Halves and Fourths/Quarters  

NSDL National Science Digital Library

This activity practices the decomposing of a whole to equal shares for halves, fourths, and quarters through pizza and candy bar manipulatives. Students are then challenge to demonstrate how many different ways they can fold a square sticky not into fourths!

Brandi Harris

2012-07-31

307

Toward a systematic analysis of the fourth-root trick  

E-print Network

In this note I briefly discuss ideas related to the so-called fourth-root trick. A decomposition of the ``rooted'' fermion effective action into Wilson fermions and a nonlocal, lattice spacing suppressed functional is presented, complete with link interactions. Some proposals are given for analytical, nonperturbative studies of the fourth-root trick.

Joel Giedt

2005-12-30

308

THE Fourth SHANGHAI INTERNATIONAL SYMPOSIUM ON NONLINEAR SCIENCES AND APPLICATIONS  

E-print Network

THE Fourth SHANGHAI INTERNATIONAL SYMPOSIUM ON NONLINEAR SCIENCES AND APPLICATIONS Shanghai NSA'10 for Papers The Fourth Shanghai International Symposium on Nonlinear Sciences and Applications (Shanghai NSA'10) will be held in Xuzhou and Shanghai on June 29-July 4, 2010. Shanghai NSA'10 is sponsored

Yang, Jianke

309

GENDER EQUALITY SCHEME: Fourth Annual Progress Report (2010-2011)  

E-print Network

1 GENDER EQUALITY SCHEME: Fourth Annual Progress Report (2010-2011) For copies of this report and development of the GES 14 2011 membership 15 #12;2 1. Introduction This fourth annual report on the Gender's ongoing gender equality work, and provides data on key aspects of the staff and student population

Henderson, Gideon

310

Fourth frame forums: interactive comics for collaborative learning  

Microsoft Academic Search

In this paper, we describe Fourth Frame Forums, an application that combines traditional four-frame comic strips with online web- based discussion forums. In this application, users are presented with a four-frame comic strip where the last dialogue balloon of the fourth frame is left blank. By typing a statement into this dialogue balloon, the user creates a new discussion thread

Andrew S. Gordon

2006-01-01

311

Using Inquiry to Learn about Soil: A Fourth Grade Experience  

ERIC Educational Resources Information Center

In this article, we describe a fourth-grade inquiry unit on soil. The unit was designed and taught by preservice elementary teachers as part of a university science methods course. Using a student-driven inquiry approach to designing curriculum, the unit engaged fourth graders in learning about the physical properties soil, erosion, worms, and…

Magee, Paula A.; Wingate, Elisha

2014-01-01

312

High Energy Neutrinos: Sources and Fluxes  

E-print Network

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

Todor Stanev

2005-11-28

313

Review on new Neutrino Oscillation Experiments  

E-print Network

Driven by new experimental results, in the latest period several new neutrino oscillation experiments have been proposed. I will outline the main ideas behind the different proposals, in particular concerning atmospheric neutrinos and neutrinos from accelerated beams.

Mario Campanelli

1999-05-19

314

91THE FOURTH PARADIGM HEALTH AND WELLBEING  

E-print Network

. Furthermore, the social ben- efits of EHRs may be greater from such population-level uses than from individual/citizens/consumers) and communi- ties (families/local populations etc.) than with healthcare organizations. In sum- mary, the use in molecular medical research. Some tech- niques, such as genome-wide analysis, produce large volumes of data

Winn, John

315

Neutrino magnetic moment effects in neutrino nucleus reactions  

SciTech Connect

Some low energy neutrino nucleus reactions induced by neutrinos (antineutrinos) having a magnetic moment of the order of 10{sup {minus}9}{minus}10{sup {minus}10} Bohr magneton are studied. It is found that in the case of {sup 4}He, {sup 12}C, and {sup 16}O, the detection of very low energy scalar and isoscalar elastic and inelastic reactions induced by the isoscalar vector currents can provide a better limit on the neutrino magnetic moment.

Singh, S.K.; Athar, M.S. [Department of Physics, Aligarh Muslim University, Aligarh-202002 (India)] [Department of Physics, Aligarh Muslim University, Aligarh-202002 (India)

1995-10-01

316

Neutrino Physics and Astrophysics with the Antares Neutrino Telescope  

NASA Astrophysics Data System (ADS)

The ANTARES detector is currently the largest operating neutrino telescope in the Northern Hemisphere. Its scientific target is the detection of ultra-high energy cosmic neutrinos through measurement of Cherenkov radiation from neutrino-induced charged leptons. Here, an overview of the results of various analyses will be given, in particular for the searches of point-like sources and the opportunities for multi-messenger astronomy.

Spurio, M.

2015-01-01

317

Collective flavour transitions of supernova neutrinos  

E-print Network

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

Irene Tamborra

2009-05-15

318

Heavy sterile neutrinos and supernova explosions  

E-print Network

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

George M. Fuller; Alexander Kusenko; Kalliopi Petraki

2008-10-01

319

Status of global fits to neutrino oscillations  

Microsoft Academic Search

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

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

2004-01-01

320

Searching for hep Neutrinos using the Sudbury Neutrino Observatory  

E-print Network

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

Chris Howard; for the SNO Collaboration

2009-05-29

321

Non-unitary neutrino propagation from neutrino decay  

NASA Astrophysics Data System (ADS)

Neutrino propagation in space-time is not constrained to be unitary if very light states - lighter than the active neutrinos - exist into which neutrinos may decay. If this is the case, neutrino flavor-change is governed by a handful of extra mixing and "oscillation" parameters, including new sources of CP-invariance violation. We compute the transition probabilities in the two- and three-flavor scenarios and discuss the different phenomenological consequences of the new physics. These are qualitatively different from other sources of unitarity violation discussed in the literature.

Berryman, Jeffrey M.; de Gouvêa, André; Hernández, Daniel; Oliveira, Roberto L. N.

2015-03-01

322

Genetic concepts in Greek literature from the eighth to the fourth century B.C.  

PubMed

A review of the concepts of genetics found in epic, historical and dramatic ancient Greek writings from the eighth to the fourth centuries B.C., is presented. The derived data suggest that the development of genetical concepts and ideas started with the praise of the heroes' divine or noble origin in Homer's epic poems (eighth century B.C.). It continued in the tracing of the descent and vicissitudes of the families of the Greek gods and the common ancestry of the Greek tribes as described in Hesiod's genealogical poems (around 700 B.C.), in the statement of descent and dual parenthood of leaders and kings in the books of Herodotus and Xenophon (fifth and fourth centuries B.C.), and in the concern about the lineage of the tragic figures in Greek drama (fifth century B.C.). The genetical concepts expressed in these writings most probably reflected popular notions of that time. They must, therefore, have been the basis of the perceptions and theories on heredity and procreation expressed by the ancient physicians and philosophers in the fifth and fourth centuries B.C., which in turn influenced the development of genetics for many centuries. PMID:1551655

Bazopoulou-Kyrkanidou, E

1992-03-01

323

Fourth generation electron cyclotron resonance ion sources.  

PubMed

The concepts and technical challenges related to developing a fourth generation electron cyclotron resonance (ECR) ion source with a rf frequency greater than 40 GHz and magnetic confinement fields greater than twice B(ECR) will be explored in this article. Based on the semiempirical frequency scaling of ECR plasma density with the square of operating frequency, there should be significant gains in performance over current third generation ECR ion sources, which operate at rf frequencies between 20 and 30 GHz. While the third generation ECR ion sources use NbTi superconducting solenoid and sextupole coils, the new sources will need to use different superconducting materials, such as Nb(3)Sn, to reach the required magnetic confinement, which scales linearly with rf frequency. Additional technical challenges include increased bremsstrahlung production, which may increase faster than the plasma density, bremsstrahlung heating of the cold mass, and the availability of high power continuous wave microwave sources at these frequencies. With each generation of ECR ion sources, there are new challenges to be mastered, but the potential for higher performance and reduced cost of the associated accelerator continues to make this a promising avenue for development. PMID:18315111

Lyneis, Claude M; Leitner, D; Todd, D S; Sabbi, G; Prestemon, S; Caspi, S; Ferracin, P

2008-02-01

324

Burst Neutrinos from Nitrogen Flash  

E-print Network

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

A. M. Serenelli; M. Fukugita

2005-09-07

325

Gauge Trimming of Neutrino Masses  

SciTech Connect

We show that under a new U(1) gauge symmetry, which is non-anomalous in the presence of one ''right-handed neutrino'' per generation and consistent with the standard model Yukawa couplings, the most general fermion charges are determined in terms of four rational parameters. This generalization of the B-L symmetry with generation-dependent lepton charges leads to neutrino masses induced by operators of high dimensionality. Neutrino masses are thus naturally small without invoking physics at energies above the TeV scale, whether neutrinos are Majorana or Dirac fermions. This ''Leptocratic'' Model predicts the existence of light quasi-sterile neutrinos with consequences for cosmology, and implies that collider experiments may reveal the origin of neutrino masses.

Chen, Mu-Chun; /Fermilab /UC, Irvine; de Gouvea, Andre; /Northwestern U. /Fermilab; Dobrescu, Bogdan A.; /Fermilab

2006-12-01

326

Neutrino Magnetic Moments and Electromagnetic Leptogenesis  

SciTech Connect

We analyze the connection between neutrino magnetic moments and neutrino masses. Electroweak radiative corrections to the neutrino mass are used to derive naturalness upper bounds on neutrino magnetic moments, generated by physics above the electroweak scale. For Dirac (Majorana) neutrinos the bound is several orders of magnitude stronger (weaker) than present experimental limits. The discovery of a neutrino magnetic moment near the present experimental sensitivity would thus suggest that neutrinos are Majorana particles. We also outline a new baryogenesis-via-leptogenesis scenario where the lepton asymmetry is generated by CP violating decays of heavy right handed neutrinos via electromagnetic dipole moment couplings.

Bell, Nicole F. [School of Physics, University of Melbourne, Victoria 3010 (Australia)

2009-12-17

327

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

328

Family Secrets and Family Environment  

Microsoft Academic Search

This study explored whether family secrecy might be a potential mediator of later adult psychological functioning in the offspring of the family. Results revealed that family secrecy was related to psychological well-being in adulthood. The number of potentially secretive events, as well as the negativity of the family environment were strongly associated with poorer psychological functioning.

Marianne F. Jahn

1995-01-01

329

Neutrino Masses and Flavor Mixing  

E-print Network

We discuss the neutrino oscillations, using texture zero mass matrices for the leptons. The reactor mixing angle $\\theta^{}_{l}$ is calculated. The ratio of the masses of two neutrinos is determined by the solar mixing angle. We can calculate the masses of the three neutrinos: $m_1$ $\\approx$ 0.003 eV - $m_2$ $\\approx$ 0.012 eV - $m_3$ $\\approx$ 0.048 eV.

Fritzsch, Harald

2015-01-01

330

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

331

Neutrino Masses and Flavor Oscillations  

E-print Network

This essay is intended to provide a brief description of the peculiar properties of neutrinos within and beyond the standard theory of weak interactions. The focus is on the flavor oscillations of massive neutrinos, from which one has achieved some striking knowledge about their mass spectrum and flavor mixing pattern. The experimental prospects towards probing the absolute neutrino mass scale, possible Majorana nature and CP-violating effects will also be addressed.

Wang, Yifang

2015-01-01

332

Geo-neutrinos and Borexino  

NASA Astrophysics Data System (ADS)

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. After a brief introduction about the Earth, the geo-neutrinos' properties and the main aims of their study are discussed. An overview of the latest experimental results obtained by the Borexino collaboration is provided, followed by a short overview of future perspectives of this new inter-disciplinary field.

Ludhova, L.; Bellini, G.; Benziger, J.; Bick, D.; Bonfini, G.; Bravo, D.; Caccianiga, B.; Calaprice, F.; Caminata, A.; Cavalcante, P.; Chavarria, A.; Chepurnov, A.; D'Angelo, D.; Davini, S.; Derbin, A.; Empl, A.; Etenko, A.; Fomenko, K.; Franco, D.; Fiorentini, G.; Galbiati, C.; Gazzana, S.; Ghiano, C.; Giammarchi, M.; Göger-Neff, M.; Goretti, A.; Hagner, C.; Hungerford, E.; Ianni, Aldo; Ianni, Andrea; Kobychev, V.; Korablev, D.; Korga, G.; Kryn, D.; Laubenstein, M.; Lehnert, B.; Lewke, T.; Litvinovich, E.; Lombardi, F.; Lombardi, P.; Lukyanchenko, G.; Machulin, I.; Manecki, S.; Maneschg, W.; Mantovani, F.; Marcocci, S.; Meindl, Q.; Meroni, E.; Meyer, M.; Miramonti, L.; Misiaszek, M.; Mosteiro, P.; Muratova, V.; Oberauer, L.; Obolensky, M.; Ortica, F.; Otis, K.; Pallavicini, M.; Papp, L.; Perasso, L.; Pocar, A.; Ranucci, G.; Razeto, A.; Re, A.; Ricci, B.; 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.; Wang, H.; Winter, J.; Wojcik, M.; Wright, A.; Wurm, M.; Zaimidoroga, O.; Zavatarelli, S.; Zuber, K.; Zuzel, G.

2015-03-01

333

Can relic neutrinos be observed  

SciTech Connect

Within the framework of big-bang cosmology and the standard electroweak model, it appears that the only possibly detectable interaction of relic neutrinos is their annihilation with cosmic ray neutrinos on the Z resonance. However, measurement will require the existence of a large density of z approx. > 5 red-shifted sources with intense neutrino emission in the energy region 10/sup 21/eV/sup 2//m/sub nu/.

Weiler, T.

1983-01-01

334

Supernova neutrino three-flavor evolution with dominant collective effects  

SciTech Connect

Neutrino and antineutrino fluxes from a core-collapse galactic supernova are studied, within a representative three-flavor scenario with inverted mass hierarchy and tiny 1-3 mixing. The initial flavor evolution is dominated by collective self-interaction effects, which are computed in a full three-family framework along an averaged radial trajectory. During the whole time span considered (t = 1-20 s), neutrino and antineutrino spectral splits emerge as dominant features in the energy domain for the final, observable fluxes. The main results can be useful for SN event rate simulations in specific detectors. Some minor or unobservable three-family features (e.g., related to the muonic-tauonic flavor sector), as well as observable effects due to variations in the spectral input, are also discussed for completeness.

Fogli, Gianluigi; Marrone, Antonio; Tamborra, Irene [Dipartimento Interateneo di Fisica ''Michelangelo Merlin'', Via Amendola 173, 70126 Bari (Italy)] [Dipartimento Interateneo di Fisica ''Michelangelo Merlin'', Via Amendola 173, 70126 Bari (Italy); Lisi, Eligio, E-mail: gianluigi.fogli@ba.infn.it, E-mail: eligio.lisi@ba.infn.it, E-mail: antonio.marrone@ba.infn.it, E-mail: irene.tamborra@ba.infn.it [Istituto Nazionale di Fisica Nucleare, Sezione di Bari, Via Orabona 4, 70126 Bari (Italy)] [Istituto Nazionale di Fisica Nucleare, Sezione di Bari, Via Orabona 4, 70126 Bari (Italy)

2009-04-15

335

MINOS Search for Sterile Neutrinos  

E-print Network

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

Alexandre Sousa; on behalf of the MINOS Collaboration

2011-10-16

336

Supernova neutrinos and explosive nucleosynthesis  

SciTech Connect

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

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

2014-05-09

337

Proton and Neutrino Extragalactic Astronomy  

E-print Network

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

Paolo Lipari

2008-08-04

338

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

339

Combined search for the quarks of a sequential fourth generation  

DOE PAGESBeta

Results are presented from a search for a fourth generation of quarks produced singly or in pairs in a data set corresponding to an integrated luminosity of 5??fb?1 recorded by the CMS experiment at the LHC in 2011. A novel strategy has been developed for a combined search for quarks of the up and down type in decay channels with at least one isolated muon or electron. Limits on the mass of the fourth-generation quarks and the relevant Cabibbo-Kobayashi-Maskawa matrix elements are derived in the context of a simple extension of the standard model with a sequential fourth generation of fermions. The existence of mass-degenerate fourth-generation quarks with masses below 685 GeV is excluded at 95% confidence level for minimal off-diagonal mixing between the third- and the fourth-generation quarks. With a mass difference of 25 GeV between the quark masses, the obtained limit on the masses of the fourth-generation quarks shifts by about ±20??GeV . These results significantly reduce the allowed parameter space for a fourth generation of fermions.

Chatrchyan, S.; Khachatryan, V.; Sirunyan, A. M.; Tumasyan, A.; Adam, W.; Aguilo, E.; Bergauer, T.; Dragicevic, M.; Erö, J.; Fabjan, C.; Friedl, M.; Frühwirth, R.; Ghete, V. M.; Hammer, J.; Hörmann, N.; Hrubec, J.; Jeitler, M.; Kiesenhofer, W.; Knünz, V.; Krammer, M.; Krätschmer, I.; Liko, D.; Mikulec, I.; Pernicka, M.; Rahbaran, B.; Rohringer, C.; Rohringer, H.; Schöfbeck, R.; Strauss, J.; Taurok, A.; Waltenberger, W.; Walzel, G.; Widl, E.; Wulz, C.-E.; Mossolov, V.; Shumeiko, N.; Suarez Gonzalez, J.; Bansal, M.; Bansal, S.; Cornelis, T.; De Wolf, E. A.; Janssen, X.; Luyckx, S.; Mucibello, L.; Ochesanu, S.; Roland, B.; Rougny, R.; Selvaggi, M.; Staykova, Z.; Van Haevermaet, H.; Van Mechelen, P.; Van Remortel, N.; Van Spilbeeck, A.; Blekman, F.; Blyweert, S.; D’Hondt, J.; Gonzalez Suarez, R.; Kalogeropoulos, A.; Maes, M.; Olbrechts, A.; Van Doninck, W.; Van Mulders, P.; Van Onsem, G. P.; Villella, I.; Clerbaux, B.; De Lentdecker, G.; Dero, V.; Gay, A. P. R.; Hreus, T.; Léonard, A.; Marage, P. E.; Mohammadi, A.; Reis, T.; Thomas, L.; Vander Marcken, G.; Vander Velde, C.; Vanlaer, P.; Wang, J.; Adler, V.; Beernaert, K.; Cimmino, A.; Costantini, S.; Garcia, G.; Grunewald, M.; Klein, B.; Lellouch, J.; Marinov, A.; Mccartin, J.; Ocampo Rios, A. A.; Ryckbosch, D.; Strobbe, N.; Thyssen, F.; Tytgat, M.; Verwilligen, P.; Walsh, S.; Yazgan, E.; Zaganidis, N.; Basegmez, S.; Bruno, G.; Castello, R.; Ceard, L.; Delaere, C.; du Pree, T.; Favart, D.; Forthomme, L.; Giammanco, A.; Hollar, J.; Lemaitre, V.; Liao, J.; Militaru, O.; Nuttens, C.; Pagano, D.; Pin, A.; Piotrzkowski, K.; Schul, N.; Vizan Garcia, J. M.; Beliy, N.; Caebergs, T.; Daubie, E.; Hammad, G. H.; Alves, G. A.; Correa Martins Junior, M.; De Jesus Damiao, D.; Martins, T.; Pol, M. E.; Souza, M. H. G.; Aldá Júnior, W. L.; Carvalho, W.; Custódio, A.; Da Costa, E. M.; De Oliveira Martins, C.; Fonseca De Souza, S.; Matos Figueiredo, D.; Mundim, L.; Nogima, H.; Oguri, V.; Prado Da Silva, W. L.; Santoro, A.; Soares Jorge, L.; Sznajder, A.; Anjos, T. S.; Bernardes, C. A.; Dias, F. A.; Tomei, T.R. Fernandez Perez; Gregores, E. M.; Lagana, C.; Marinho, F.; Mercadante, P. G.; Novaes, S. F.; Padula, Sandra S.; Genchev, V.; Iaydjiev, P.; Piperov, S.; Rodozov, M.; Stoykova, S.; Sultanov, G.; Tcholakov, V.; Trayanov, R.; Vutova, M.; Dimitrov, A.; Hadjiiska, R.; Kozhuharov, V.; Litov, L.; Pavlov, B.; Petkov, P.; Bian, J. G.; Chen, G. M.; Chen, H. S.; Jiang, C. H.; Liang, D.; Liang, S.; Meng, X.; Tao, J.; Wang, J.; Wang, X.; Wang, Z.; Xiao, H.; Xu, M.; Zang, J.; Zhang, Z.; Asawatangtrakuldee, C.; Ban, Y.; Guo, S.; Guo, Y.; Li, W.; Liu, S.; Mao, Y.; Qian, S. J.; Teng, H.; Wang, D.; Zhang, L.; Zhu, B.; Zou, W.; Avila, C.; Gomez, J. P.; Gomez Moreno, B.; Osorio Oliveros, A. F.; Sanabria, J. C.; Godinovic, N.; Lelas, D.; Plestina, R.; Polic, D.; Puljak, I.; Antunovic, Z.; Kovac, M.; Brigljevic, V.; Duric, S.; Kadija, K.; Luetic, J.; Morovic, S.; Attikis, A.; Galanti, M.; Mavromanolakis, G.; Mousa, J.; Nicolaou, C.; Ptochos, F.; Razis, P. A.; Finger, M.; Finger, M.; Assran, Y.; Elgammal, S.; Ellithi Kamel, A.; Khalil, S.; Mahmoud, M. A.; Radi, A.; Kadastik, M.; Müntel, M.; Raidal, M.; Rebane, L.; Tiko, A.; Eerola, P.; Fedi, G.; Voutilainen, M.; Härkönen, J.; Heikkinen, A.; Karimäki, V.; Kinnunen, R.; Kortelainen, M. J.; Lampén, T.; Lassila-Perini, K.; Lehti, S.; Lindén, T.; Luukka, P.; Mäenpää, T.; Peltola, T.; Tuominen, E.; Tuominiemi, J.; Tuovinen, E.; Ungaro, D.; Wendland, L.; Banzuzi, K.; Karjalainen, A.; Korpela, A.; Tuuva, T.; Besancon, M.; Choudhury, S.; Dejardin, M.; Denegri, D.; Fabbro, B.; Faure, J. L.; Ferri, F.; Ganjour, S.; Givernaud, A.; Gras, P.; Hamel de Monchenault, G.; Jarry, P.; Locci, E.; Malcles, J.; Millischer, L.; Nayak, A.; Rander, J.; Rosowsky, A.; Shreyber, I.; Titov, M.; Baffioni, S.; Beaudette, F.; Benhabib, L.; Bianchini, L.; Bluj, M.; Broutin, C.; Busson, P.; Charlot, C.; Daci, N.; Dahms, T.; Dobrzynski, L.; Granier de Cassagnac, R.; Haguenauer, M.; Miné, P.; Mironov, C.; Naranjo, I. N.; Nguyen, M.; Ochando, C.; Paganini, P.; Sabes, D.; Salerno, R.; Sirois, Y.; Veelken, C.; Zabi, A.; Agram, J.-L.; Andrea, J.; Bloch, D.; Bodin, D.; Brom, J.-M.; Cardaci, M.; Chabert, E. C.; Collard, C.; Conte, E.; Drouhin, F.; Ferro, C.; Fontaine, J.-C.; Gelé, D.; Goerlach, U.; Juillot, P.; Le Bihan, A.-C.; Van Hove, P.; Fassi, F.; Mercier, D.; Beauceron, S.; Beaupere, N.; Bondu, O.; Boudoul, G.; Chasserat, J.; Chierici, R.; Contardo, D.; Depasse, P.; El Mamouni, H.; Fay, J.; Gascon, S.; Gouzevitch, M.; Ille, B.; Kurca, T.; Lethuillier, M.; Mirabito, L.; Perries, S.; Sordini, V.; Tschudi, Y.; Verdier, P.; Viret, S.; Tsamalaidze, Z.; Anagnostou, G.; Beranek, S.; Edelhoff, M.; Feld, L.; Heracleous, N.; Hindrichs, O.; Jussen, R.; Klein, K.

2012-12-01

340

Neutrino detection primer  

NASA Astrophysics Data System (ADS)

This report is intended to provide for non-expert readers a survey of natural and manmade neutrino sources and a critical review of various methods proposed for their detection. Detection methods may be divided into two classes, those which have very modest performance and might actually work, and those which promise spectacular performance but violate the laws of physics. Emphasis in this report is on the second. The purpose is not to describe in detail what is possible, but to establish firm limits beyond which all schemes for detection capability are impossible. The last two sections of the report are for advanced students only and should be skipped by the non-expert. They provide precise mathematical statements and proofs of the limits which the laws of physics impose on neutrino cross sections. The limits are neither simple nor obvious. Consequently, it may be useful to have their technical justification here put on record.

Callan, C.; Dyson, F.; Treiman, S.

1988-03-01

341

Gravity triggered neutrino condensates  

SciTech Connect

In this work we use the Schwinger-Dyson equations to study the possibility that an enhanced gravitational attraction triggers the formation of a right-handed neutrino condensate, inducing dynamical symmetry breaking and generating a Majorana mass for the right-handed neutrino at a scale appropriate for the seesaw mechanism. The composite field formed by the condensate phase could drive an early epoch of inflation. We find that to the lowest order, the theory does not allow dynamical symmetry breaking. Nevertheless, thanks to the large number of matter fields in the model, the suppression by additional powers in G of higher order terms can be compensated, boosting them up to their lowest order counterparts. This way chiral symmetry can be broken dynamically and the infrared mass generated turns out to be in the expected range for a successful seesaw scenario.

Barenboim, Gabriela [Departament de Fisica Teorica and IFIC, Universitat de Valencia-CSIC, E-46100, Burjassot (Spain)

2010-11-01

342

Observables in Neutrino Mass Spectroscopy Using Atoms  

E-print Network

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

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

2013-01-17

343

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

344

Neutrinos in the Electron  

E-print Network

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

E. L. Koschmieder

2006-09-26

345

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

346

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

347

The Superior Transvelar Approach to the Fourth Ventricle and Brainstem  

PubMed Central

Objective?The superior transvelar approach is used to access pathologies located in the fourth ventricle and brainstem. The surgical path is below the venous structures, through the superior medullary velum. Following splitting the tentorial edge, near the tentorial apex, the superior medullary velum is split in the cerebello-mesencephalic fissure. Using the supracerebellar infratentorial, transtentorial or parietal interhemispheric routes, the superior medullary velum is approached. Splitting this velum provides a detailed view of the fourth ventricle and its floor. Materials and Methods?A total of 10 formalin-fixed specimens were dissected in a stepwise manner to simulate the superior transvelar approach to the fourth ventricle. The exposure gained the distance from the craniotomy site and the ease of access was assessed for each of the routes. We also present an illustrative case, operated by the senior author (AN). Results?The superior transvelar approach provides access to the entire length of the fourth ventricle floor, from the aqueduct to the obex, when using the parietal interhemispheric route. In addition, this approach provides access to the entire width of the floor of the fourth ventricle; however, this requires retracting the superior cerebellar peduncle. Using the supracerebellar infratentorial route gives a limited exposure of the superior part of the fourth ventricle. The occipital interhemispheric route is a compromise between these two. Conclusion?The superior transvelar approach to the fourth ventricle provides a route for approaching the fourth ventricle from above. This approach does not require opening the posterior fossa in the traditional way, and provides a reasonable alternative for accessing the superior fourth ventricle. PMID:23730546

Ezer, Haim; Banerjee, Anirban Deep; Bollam, Papireddy; Guthikonda, Bharat; Nanda, Anil

2012-01-01

348

Proceedings: Fourth Workshop on Mining Scientific Datasets  

SciTech Connect

Commercial applications of data mining in areas such as e-commerce, market-basket analysis, text-mining, and web-mining have taken on a central focus in the JCDD community. However, there is a significant amount of innovative data mining work taking place in the context of scientific and engineering applications that is not well represented in the mainstream KDD conferences. For example, scientific data mining techniques are being developed and applied to diverse fields such as remote sensing, physics, chemistry, biology, astronomy, structural mechanics, computational fluid dynamics etc. In these areas, data mining frequently complements and enhances existing analysis methods based on statistics, exploratory data analysis, and domain-specific approaches. On the surface, it may appear that data from one scientific field, say genomics, is very different from another field, such as physics. However, despite their diversity, there is much that is common across the mining of scientific and engineering data. For example, techniques used to identify objects in images are very similar, regardless of whether the images came from a remote sensing application, a physics experiment, an astronomy observation, or a medical study. Further, with data mining being applied to new types of data, such as mesh data from scientific simulations, there is the opportunity to apply and extend data mining to new scientific domains. This one-day workshop brings together data miners analyzing science data and scientists from diverse fields to share their experiences, learn how techniques developed in one field can be applied in another, and better understand some of the newer techniques being developed in the KDD community. This is the fourth workshop on the topic of Mining Scientific Data sets; for information on earlier workshops, see http://www.ahpcrc.org/conferences/. This workshop continues the tradition of addressing challenging problems in a field where the diversity of applications is matched only by the opportunities that await a practitioner.

Kamath, C

2001-07-24

349

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

350

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

351

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

E-print Network

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

Shao-Hsuan Chiu; T. K. Kuo

2006-02-27

352

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

353

ON SOLAR NEUTRINO PROBLEM TIAN MA AND SHOUHONG WANG  

E-print Network

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

354

Family History  

MedlinePLUS

... Home CDC 24/7: Saving Lives. Protecting People.™ Genomics All CDC Topics Search The CDC Note: Javascript ... visit this page: About CDC.gov . Public Health Genomics Genomics Family Health History Share Compartir Family History ...

355

Family Arguments  

MedlinePLUS

... Pediatric First Aid for Caregivers and Teachers (PedFACTs) Teaching Package HealthyChildren.org Post-it Notes Family Life Health Management - Medical Home Family Dynamics Adoption & Foster Care Communication & Discipline Types ...

356

Family Meals  

MedlinePLUS

... Sports: Keeping Kids Safe Concussions: What to Know Family Meals KidsHealth > Parents > Nutrition & Fitness Center > Healthy Eating & ... even more important as kids get older. Making Family Meals Happen It can be a big challenge ...

357

Foster Families  

MedlinePLUS

... child in another home. Continue Why Do Kids Live With Foster Families? Most often, a kid goes ... this stressful and emotional time. Why Do Kids Live With Foster Families? Most often, a kid goes ...

358

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

359

Supernova Neutrinos and the Tau-Neutrino Mass  

E-print Network

We perform an extensive investigation of the sensitivity to non-vanishing tau-neutrino mass in a large water Cherenkov detector, developing an analysis method for neutrino events originated by a supernova explosion. This approach, based on directional considerations, provides informations almost undepending on the supernova model. We analyze several theoretical models from numerical simulations and phenomenological models based on SN1987A data, and determine optimal values of the analysis parameters so as to reach the highest sensitivity to a non-vanishing tau-neutrino mass. The minimal detectable mass is generally just above the cosmologically interesting range, m ~ 100 eV, in the case of a supernova explosion near the galactic center. For the case that no positive signal is obtained, observation of a neutrino burst with Super-Kamiokande will anyhow lower the present upper bound on tau-neutrino mass to few hundred eV.

Gianni Fiorentini; Camillo Acerbi

1997-01-30

360

45. Neutrino Cross Section Measurements 1 45. Neutrino Cross Section Measurements  

E-print Network

comprehensive discussion of neutrino interaction cross sections, including neutrino-electron scattering.1. Inclusive Scattering Over the years, many experiments have measured the total cross section for neutrino (µ45. Neutrino Cross Section Measurements 1 45. Neutrino Cross Section Measurements Written in April

361

Family Support.  

ERIC Educational Resources Information Center

This "Feature Issue" of the quarterly journal "Impact" presents 19 brief articles on family support systems in the United States for persons with developmental disabilities and their families. Emphasis is on provisions of Public Law 99-457. Articles include: "Family Support in the United States: Setting a Course for the 1990s" (James Knoll);…

Wieck, Colleen, Ed.; McBride, Marijo, Ed.

1990-01-01

362

Family therapy.  

PubMed

Another major force not letting us succeed in the treatment of diabetes remains right inside the patients home, their family members. Hence, it is important to know the perception of the close family members about this simple and strong tool in diabetes, 'insulin'. The drug is nearing its century, it has not fully being accepted gracefully even in todays electronic savvy society. So, we need to strongly discover the reason for its non-acceptance, while trials are out inventing new drugs. One vital thing that can change this attitude is increasing the understanding of this drug, insulin in depth to close people around the patient, the 'family'. Underestimating family's perception about disease and treatment for diabetes is detrimental to both diseased and the doctor. This consists of a biopsychosocial model; biological, psychological and social factors. Family forms the most important part of it. The strategies in family therapy include psychodynamic, structural, strategic, and cognitive-behavioral component. Diabetes has and will continue to rise, so will be the treatment options. From the clinicians side its to fix fasting first but from patients its fix family first. Family therapy demonstrates the importance of insulin initiation and maintenance in insulin naive patients, and continuation for others. The specific needs of such patients and their impact on family life are met with family therapy. Who needs family therapy? Benefits of family therapy and a case based approach is covered. PMID:24251191

Altamash, Shaikh

2013-10-01

363

Family grief  

Microsoft Academic Search

Grief traditionally has been described from the individual perspective. In contrast, this article presents a family systems perspective on death and grieving. A group of interconnected individuals forming a system, defined as a “family,” reciprocally affect one another in response to internal or external events. Minuchin's structural theory emphasizes the importance of subsystems within a family; boundaries between subsystems are

Carol Michler Detmer; Joseph W. Lamberti

1991-01-01

364

Limits on Neutrino-Neutrino Scattering in the Early Universe  

E-print Network

In the standard model neutrinos are assumed to have streamed across the Universe since they last scattered at the weak decoupling epoch when the temperature of the standard-model plasma was ~MeV. The shear stress of free-streaming neutrinos imprints itself gravitationally on the Cosmic Microwave Background (CMB) and makes the CMB a sensitive probe of neutrino scattering. Yet, the presence of nonstandard physics in the neutrino sector may alter this standard chronology and delay neutrino free-streaming until a much later epoch. We use observations of the CMB to constrain the strength of neutrino self-interactions G_eff and put limits on new physics in the neutrino sector from the early Universe. Recent measurements of the CMB at large multipoles made by the Planck satellite and high-l experiments are critical for probing this physics. Within the context of conventional LambdaCDM parameters cosmological data are compatible with G_eff strength in a narrow region around $G_{\\rm eff} \\simeq 1/({\\rm 10 \\, MeV})^{2} \\simeq 8.6\\times10^8 G_{\\rm F}$, where $G_{\\rm F}$ is the Fermi constant. This distinct self-interacting neutrino cosmology is characterized by somewhat lower values of both the scalar spectral index and the amplitude of primordial fluctuations. While we phrase our discussion here in terms of a specific scenario in which a late onset of neutrino free-streaming could occur, our constraints on the neutrino visibility function are very general.

Francis-Yan Cyr-Racine; Kris Sigurdson

2014-12-06

365

Lepton textures and neutrino oscillations  

NASA Astrophysics Data System (ADS)

A systematic analysis of the textures arising in lepton mass matrices have been carried out using unitary transformations and condition of naturalness for the Dirac and Majorana neutrino possibilities. It is observed that the recent three neutrino oscillation data together with the effective mass in neutrinoless double beta decay provide vital clues in predicting the general structures of these lepton mass matrices.

Verma, Rohit

2014-08-01

366

High energy neutrino spin light  

E-print Network

The quantum theory of spin light (electromagnetic radiation emitted by a Dirac massive neutrino propagating in dense matter due to the weak interaction of a neutrino with background fermions) is developed. In contrast to the Cherenkov radiation, this effect does not disappear even if the medium refractive index is assumed to be equal to unity. The formulas for the transition rate and the total radiation power are obtained. It is found out that radiation of photons is possible only when the sign of the particle helicity is opposite to that of the effective potential describing the interaction of a neutrino (antineutrino) with the background medium. Due to the radiative self-polarization the radiating particle can change its helicity. As a result, the active left-handed polarized neutrino (right-handed polarized antineutrino) converting to the state with inverse helicity can become practically ``sterile''. Since the sign of the effective potential depends on the neutrino flavor and the matter structure, the spin light can change a ratio of active neutrinos of different flavors. In the ultra relativistic approach, the radiated photons averaged energy is equal to one third of the initial neutrino energy, and two thirds of the energy are carried out by the final ``sterile'' neutrinos.

A. E. Lobanov

2005-06-01

367

Lepton textures and neutrino oscillations  

E-print Network

Systematic analyses of the textures arising in lepton mass matrices have been carried out using unitary transformations and condition of naturalness for the Dirac and Majorana neutrino possibilities. It is observed that the recent three neutrino oscillation data together with the effective mass in neutrinoless double beta decay provide vital clues in predicting the general structures of these lepton mass matrices.

Rohit Verma

2014-06-03

368

Neutrino Physics and Astrophysics : Highlights  

E-print Network

This article presents an overview of neutrino physics research, with highlights on the physics goals, results and interpretations of the current neutrino experiments and future directions and program. It is not meant to be a comprehensive account or detailed review article. Interested readers can pursue the details via the listed references.

Henry Tsz-King Wong

2007-02-28

369

Observation of Geo-Neutrinos  

E-print Network

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

Borexino Collaboration

2010-03-20

370

The Mass of the Neutrinos  

E-print Network

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

Burra G. Sidharth

2009-04-30

371

Solar Models and Solar Neutrinos  

E-print Network

I summarize 40 years of development of the standard solar model that is used to predict solar neutrino fluxes and then describe the current uncertainties in the predictions. I will also attempt to explain why it took so long, about three and a half decades, to reach a consensus view that new physics is being learned from solar neutrino experiments.

John N. Bahcall

2003-10-01

372

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

373

Neutrino Theory of Stellar Collapse  

Microsoft Academic Search

At the very high temperatures and densities which must exist in the interior of contracting stars during the later stages of their evolution, one must expect a special type of nuclear processes accompanied by the emission of a large number of neutrinos. These neutrinos penetrating almost without difficulty the body of the star, must carry away very large amounts of

G. Gamow; M. Schoenberg

1941-01-01

374

Neutrino astronomy and lepton charge  

Microsoft Academic Search

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

V. Gribov; B. Pontecorvo

1969-01-01

375

31. Fourth floor, looking south at former milkstorage tank room, ...  

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

31. Fourth floor, looking south at former milk-storage tank room, spiral stair in right hand corner - Sheffield Farms Milk Plant, 1075 Webster Avenue (southwest corner of 166th Street), Bronx, Bronx County, NY

376

21. Fourth floor, second level of milk room looking southeast ...  

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

21. Fourth floor, second level of milk room looking southeast (original location of heaters) - Sheffield Farms Milk Plant, 1075 Webster Avenue (southwest corner of 166th Street), Bronx, Bronx County, NY

377

Man and Energy, Module C. Fourth Grade. Pilot Form.  

ERIC Educational Resources Information Center

This booklet is one of a set of learning modules on energy for use by students and teachers in the fourth grade. This module investigates solar energy, ecology, and fossil fuels. Included are laboratory activities and values exercises. (BT)

Pasco County Schools, Dade City, FL.

378

11. SANDSORTING BUILDING, FOURTH FLOOR; ELEVATOR No. 2 AT LEFT ...  

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

11. SAND-SORTING BUILDING, FOURTH FLOOR; ELEVATOR No. 2 AT LEFT CENTER, VIEW LOOKING NORTHEAST - Mill "C" Complex, Sand-Sorting Building, South of Dee Bennet Road, near Illinois River, Ottawa, La Salle County, IL

379

Proceedings of the Fourth PHANTOM Users Group Workshop  

E-print Network

This Report contains the proceedings of the Fourth Phantom Users Group Workshop contains 17 papers presented October 9-12, 1999 at MIT Endicott House in Dedham Massachusetts. The workshop included sessions on, Tools ...

Salisbury, J. Kenneth

1999-11-04

380

View of fourth level platform from north. Note the outline ...  

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

View of fourth level platform from north. Note the outline of the Shuttle cargo bay and wing formed by the edge of the platforms. - Marshall Space Flight Center, Saturn V Dynamic Test Facility, East Test Area, Huntsville, Madison County, AL

381

3. FOURTH FLOOR OF LARD REFINERY (NOTICE ORIGINAL WOODEN BEAMS ...  

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

3. FOURTH FLOOR OF LARD REFINERY (NOTICE ORIGINAL WOODEN BEAMS AND UNDATED LARD PRESS AND VATS ON RIGHT SIDE) - Wilson's Oil House, Lard Refinery, & Edible Fats Factory, Lard Refinery, 2801 Southwest Fifteenth Street, Oklahoma City, Oklahoma County, OK

382

7. FOURTH FLOOR, DETAIL OF HOTEL SOAP LINE TO WEST: ...  

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

7. FOURTH FLOOR, DETAIL OF HOTEL SOAP LINE TO WEST: FERGUSON & HAAS AUTOMATIC WRAPPING MACHINE INSTALLED BY 1929 - Colgate & Company Jersey City Plant, Building No. B-15, 90-96 Greene Street, Jersey City, Hudson County, NJ

383

5. FOURTH FLOOR, HOTEL SOAP LINES TO NORTHWEST: PRESS (LEFT ...  

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

5. FOURTH FLOOR, HOTEL SOAP LINES TO NORTHWEST: PRESS (LEFT CENTER), MANUAL CUTTERS (CENTER, RIGHT CENTER) - Colgate & Company Jersey City Plant, Building No. B-15, 90-96 Greene Street, Jersey City, Hudson County, NJ

384

39. FOURTH FLOOR: DETAIL OF STEAM HEATING PIPES ON NORTHEAST ...  

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

39. FOURTH FLOOR: DETAIL OF STEAM HEATING PIPES ON NORTHEAST WALL OF DINING AND SOCIAL HALL ON NORTHWEST END OF BUILDING LOOKING NORTHEAST - Masonic Temple, 1111-1119 Eleventh Street, Altoona, Blair County, PA

385

97. DETAIL OF FOURTH CATWALK LEVEL SHOWING WEST SIDE, LOOKING ...  

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

97. DETAIL OF FOURTH CATWALK LEVEL SHOWING WEST SIDE, LOOKING NORTH, INNER DOME ON RIGHT WITH KNEE BRACE FROM INNER COLUMN TO CROSS BEAM - Maryland State House, State Circle, Annapolis, Anne Arundel County, MD

386

Trace formulas for fourth order operators on unit interval, II  

E-print Network

We consider self-adjoint fourth order operators on the unit interval with the Dirichlet type boundary conditions. For such operators we determine few trace formulas, similar to the case of Gelfand--Levitan formulas for second order operators.

Andrey Badanin; Evgeny Korotyaev

2014-12-16

387

Combined search for the quarks of a sequential fourth generation  

E-print Network

Results are presented from a search for a fourth generation of quarks produced singly or in pairs in a data set corresponding to an integrated luminosity of 5??fb[superscript -1] recorded by the CMS experiment at the LHC ...

Apyan, Aram

388

Thermodynamic Laws of Neutrino and Photon Emission.  

ERIC Educational Resources Information Center

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

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

1980-01-01

389

Double Beta Decay and Majorana Neutrino  

Microsoft Academic Search

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

Masaru Doi; Tsuneyuki Kotani; Eiichi Takasugi

1985-01-01

390

Theory of neutrinos: a white paper  

Microsoft Academic Search

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

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

2007-01-01

391

Reactor Monitoring with Neutrino Detectors  

NASA Astrophysics Data System (ADS)

The study of the use of neutrino detectors to monitor nuclear reactors is currently a very active field of research. While neutrino detectors located close to reactors have been used to provide information about the global performance of the reactors, a general improvement of the technique is needed in order to use it in a practical way to monitor the fissile contents of the fuel of the nuclear reactors or the thermal power delivered. I describe the current status of the Angra Neutrino Project, aimed to building a low-mass neutrino detector to monitor the Angra II reactor of the Brazilian nuclear power plant Almirante Alvaro Ramos in order to explore new approaches to reactor monitoring with neutrino detectors.

Casimiro Linares, Edgar

2011-09-01

392

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

393

Neutrino Mixing from SUSY breaking  

E-print Network

We propose a mechanism to generate the neutrino mixing matrix from supersymmetric threshold corrections. Flavor violating soft breaking terms induce flavor changing self-energies that give a finite renormalization to the mixing matrix. The described threshold corrections get enhanced in case of quasi-degenerate neutrino masses. In this scenario, we adjust potentially arbitrary soft breaking parameters in a way to reproduce the observed neutrino mixing at one loop working with non-minimal flavor violating soft parameters. To incorporate small neutrino masses already at tree-level via a type I seesaw mechanism, we extend the Minimal Supersymmetric Standard Model with singlet Majorana neutrinos. The radiative corrections do not decouple with the scale of Supersymmetry and persist when the spectrum is shifted to higher values. Moreover, the mixing matrix renormalization with flavor-changing self-energies is not restricted to supersymmetric theories and give similar results in any theory with new flavor structures...

Hollik, Wolfgang G

2015-01-01

394

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

395

ANTARES deep sea neutrino telescope results  

SciTech Connect

The ANTARES experiment is currently the largest underwater neutrino telescope in the Northern Hemisphere. It is taking high quality data since 2007. Its main scientific goal is to search for high energy neutrinos that are expected from the acceleration of cosmic rays from astrophysical sources. This contribution reviews the status of the detector and presents several analyses carried out on atmospheric muons and neutrinos. For example it shows the results from the measurement of atmospheric muon neutrino spectrum and of atmospheric neutrino oscillation parameters as well as searches for neutrinos from steady cosmic point-like sources, for neutrinos from gamma ray bursts and for relativistic magnetic monopoles.

Mangano, Salvatore [IFIC - Instituto de Física Corpuscular, Edificio Institutos de Investigatión, 46071 Valencia (Spain); Collaboration: ANTARES Collaboration

2014-06-24

396

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

397

On the origin of families of quarks and leptons - predictions for four families  

E-print Network

The approach unifying all the internal degrees of freedom--proposed by one of us--is offering a new way of understanding families of quarks and leptons: A part of the starting Lagrange density in d(=1+13), which includes two kinds of spin connection fields--the gauge fields of two types of Clifford algebra objects--transforms the right handed quarks and leptons into the left handed ones manifesting in d=1+3 the Yukawa couplings of the Standard model. We study the influence of the way of breaking symmetries on the Yukawa couplings and estimate properties of the fourth family--the quark masses and the mixing matrix, investigating the possibility that the fourth family of quarks and leptons appears at low enough energies to be observable with the new generation of accelerators.

G. Bregar; M. Breskvar; D. Lukman; N. S. Mankoc Borstnik

2007-08-21

398

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

E-print Network

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

Joao Pulido; Ana M. Mourao

1998-03-02

399

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

E-print Network

the atmosphere produce a neutrino flux of about 1/cm2/s at sea level. Neutrinos produced in the Big Bang later in 1933, Enrico Fermi devised a theory for beta decays which 1 #12;Chapter 1: Neutrino Physics 2

400

Generic lepton mass matrices and neutrino oscillations  

E-print Network

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 seesaw mechanism suffices to determine the texture structure of fermion Yukawa couplings and discuss the significance of the effective mass in 0{\

Rohit Verma

2014-02-10

401

Neutrino electromagnetic properties and new physics  

E-print Network

New effects of nontrivial neutrino electromagnetic properties are investigated on the basis of exact solutions of the modified Dirac equations for neutrinos in dense magnetized rotating matter. The effect of spatial separation of different types of neutrinos and antineutrinos (different in flavors and energies) moving inside dense magnetized rotating matter is predicted. We also describe a new mechanism of a star rotation frequency shift by neutrinos escaping the star (termed "Neutrino Star Turning" mechanism, $\

Alexander Studenikin; Ilya Tokarev

2014-06-10

402

An angle to tackle the neutrinos  

E-print Network

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

G. Rajasekaran

2012-06-01

403

Neutrino magnetic moment in a magnetized plasma  

SciTech Connect

The magnetized-plasma contribution to the neutrino anomalous magnetic moment is calculated. It is shown that, in a magnetized plasma, only part of the neutrino additional energy associated with the neutrino spin and with the magnetic-field strength contributes to the neutrino magnetic moment. It is found that, in contrast to results presented previously in the literature, the presence of a magnetized plasma does not lead to a substantial enhancement of the neutrino magnetic moment.

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

2010-12-15

404

Novel photosensors for neutrino detectors and telescopes  

Microsoft Academic Search

The volume and the photosensitive area of next generation detectors of the numerous rarely occurring phenomena will greatly\\u000a exceed the sizes of the current experiments. These phenomena include cosmic neutrinos, atmospheric neutrinos, long-baseline\\u000a neutrino beams from accelerators, geo-neutrinos, geo-reactor neutrinos, and hypothetic proton decays. Similar requirements\\u000a hold for a new type of a large scanning device for homeland security and

Daniel Ferenc; Eckart Lorenz

2007-01-01

405

Superluminal Neutrinos without Revolution  

E-print Network

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

Susan Gardner

2011-12-06

406

Strongly Interacting Astrophysical Neutrinos  

E-print Network

The origin and chemical composition of ultra high energy cosmic rays is still an open question in astroparticle physics. The observed large-scale isotropy and also direct composition measurements can be interpreted as an extragalactic proton dominance above the ankle at about 10^10 GeV. Photopion production of extragalactic protons in the cosmic microwave background predicts a cutoff at about 5x10^10 GeV in conflict with excesses reported by some experiments. In this report we will outline a recent statistical analysis (astro-ph/0506698) of cosmic ray data using strongly interacting neutrinos as primaries for these excesses.

Markus Ahlers

2005-11-16

407

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

408

Neutrino and Anti-neutrino Cross Sections at MiniBooNE  

NASA Astrophysics Data System (ADS)

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 (CH2). 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

2011-10-01

409

Masses and Mixings from Neutrino Beams pointing to Neutrino Telescopes  

E-print Network

We discuss the potential to determine leading oscillation parameters, the value and the sign of \\Delta m^2_{31}, as well as the magnitude of \\sin^2 2\\theta_{13} using a conventional wide band neutrino beam pointing to water or ice Cherenkov neutrino detectors known as ``Neutrino Telescopes''. We find that precision measurements of \\Delta m^2_{31} and \\theta_{23} are possible and that, even though it is not possible to discriminate between charges in the detector, there is a remarkably good sensitivity to the mixing angle \\theta_{13} and the sign of \\Delta m^2_{31}.

K. Dick; M. Freund; P. Huber; M. Lindner

2000-06-09

410

A search for heavy neutrino decays in a neutrino beam  

SciTech Connect

Decay of heavy neutrinos ..nu../sub H/ ..-->.. ..nu..l..mu..e(l = e, ..mu..) has been searched for in the Brookhaven Alternting Gradient Synchrotron wide-band neutrino beam. Since no significant excess of such events was found, upper limits on the neutrino mixing matrix elements, absolute value of U/sub eH//sup 2/ and absolute value of U/sub ..mu..H//sup 2/ were obtained for the mass range of 180 to 500 MeV.

Ahrens, L.A.; Aronson, S.H.; Gibbard, B.G.; Murtagh, M.J.; White, D.H.; Callas, J.L.; Cutts, D.; Diwan, M.; Hoftun, J.S.; Lanau, R.E.

1987-01-01

411

Geometry of Majorana neutrino and new symmetries  

E-print Network

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

G. G. Volkov

2006-07-30

412

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

413

Solar monopoles and terrestrial neutrinos  

SciTech Connect

Magnetic monopoles captured in the core of the sun may give rise to a substantial flux of energetic neutrinos by catalyzing the decay of solar hydrogen. We discuss the expected neutrino flux in underground detectors under different assumptions about solar interior conditions. Although a monopole flux as low as F/sub M/ /approximately/ 10/sup /minus/24/ cm/sup /minus/2/ sec/sup /minus/1/ sr/sup /minus/1/ could give rise to a neutrino flux above atmospheric background, due to M/bar M/ annihilation, this does not translate into a reliable monopole flux bound stronger than the Parker limit. 8 refs., 1 fig.

Frieman, J.

1988-04-01

414

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, and some proposals for direct counting 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.

1984-01-01

415

Solar (and other) Neutrinos 4.1 Solar neutrino detectors  

E-print Network

, they form a path in the lower right quadrant. However the experimental data is in the upper left quadrant neutrino flux can be produced by lowering the central temperature of the sun somewhat. However

Washington at Seattle, University of - Department of Physics, Electroweak Interaction Research Group

416

Implementing a Fourth Order Runge-Kutta Method for Orbit Simulation  

E-print Network

Implementing a Fourth Order Runge-Kutta Method for Orbit Simulation C.J. Voesenek June 14, 2008 1 and to reduce calculation time. A fourth order Runge-Kutta method (RK4) is very well suited for this purpose, as it is stable at large time steps, accurate and relatively fast. 2 Fourth order Runge-Kutta method The fourth

Richmond, Michael W.

417

Supernova II Neutrino Bursts and Neutrino Massive Mixing  

E-print Network

We describe the Neutrino Spectrum and detection for SN II sources. We discuss the effects of neutrino mixing in the SN II. A new analysis of SN1987A is described. We discuss the possible detection of the diffuse relic SN II flux. Finally we discuss a new detection concept, OMNIS, for Nu sub mu and Nu sub tau and detection and compare with other present and future SN detectors.

David B. Cline

2001-03-08

418

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

419

The Liquid Scintillator Neutrino Detector and LAMPF Neutrino Source  

E-print Network

A search for neutrino oscillations of the type nu_bar_mu to nu_bar_e has been conducted at the Los Alamos Meson Physics Facility using nu_bar_mu from muon decay at rest. Evidence for this transition has been reported previously. This paper discusses in detail the experimental setup, detector operation and neutrino source, including aspects relevant to oscillation searches in the muon decay-at-rest and pion decay in flight channels.

C. Athanassopoulos; L. B. Auerbach; D. Bauer; R. D. Bolton; R. L. Burman; I. Cohen; D. O. Caldwell; B. D. Dieterle; J. B. Donahue; A. M. Eisner; A. Fazely; F. J. Federspiel; G. T. Garvey; M. Gray; R. M. Gunasingha; V. Highland; R. Imlay; K. Johnston; H. J. Kim; W. C. Louis; A. Lu; J. Margulies; G. B. Mills; K. McIlhany; W. Metcalf; R. A. Reeder; V. Sandberg; M. Schillaci; D. Smith; I. Stancu; W. Strossman; R. Tayloe; G. J. VanDalen; W. Vernon; Y-X. Wang; D. H. White; D. Whitehouse; D. Works; Y. Xiao; S. Yellin

1996-05-07

420

Neutrino mass hierarchy extraction using atmospheric neutrinos in ice  

E-print Network

We show that the measurements of 10 GeV atmospheric neutrinos by an upcoming array of densely packed phototubes buried deep inside the IceCube detector at the South Pole can be used to determine the neutrino mass hierarchy for values of sin^2(2theta13) close to the present bound, if the hierarchy is normal. These results are obtained for an exposure of 100 Mton years and systematic uncertainties up to 10%.

Olga Mena; Irina Mocioiu; Soebur Razzaque

2008-10-21

421

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

422

Rotation Curves of Galaxies by Fourth Order Gravity  

E-print Network

We investigate the radial behavior of galactic rotation curves by a Fourth Order Gravity adding also the Dark Matter component. The Fourth Order Gravity is a Lagrangian containing the Ricci scalar, the Ricci and Riemann tensor, but the rotation curves are depending only on two free parameters. A systematic analysis of rotation curves, in the Newtonian Limit of theory, induced by all galactic sub-structures of ordinary matter is shown. This analysis is presented for Fourth Order Gravity with and without Dark Matter. The outcomes are compared with respect to classical outcomes of General Relativity. The gravitational potential of point-like mass is the usual potential corrected by two Yukawa terms. The rotation curve is higher or also lower than curve of General Relativity if in the Lagrangian the Ricci scalar square is dominant or not with respect to the contribution of the Ricci tensor square. The curves are compared with the experimental data for the Milky Way and the galaxy NGC 3198. Although the Fourth Order Gravity gives more rotational contributions, in the limit of large distances the Keplerian behavior is present, and it is missing if we add a Dark Matter component. By modifying the theory of Gravitation consequently also the spatial description of Dark Matter could undergo a modification. At last we compare the gravitational potential by Fourth Order Gravity with respect to more used potential induced by power law of Ricci scalar.

A. Stabile; G. Scelza

2011-12-21

423

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

NASA Astrophysics Data System (ADS)

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

Wittich, Peter

2000-12-01

424

Radiative Emission of Neutrino Pairs in Atoms and Light Sterile Neutrinos  

E-print Network

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

D. N. Dinh; S. T. Petcov

2015-01-22

425

Radiative emission of neutrino pairs in atoms and light sterile neutrinos  

NASA Astrophysics Data System (ADS)

The process of Radiative Emission of Neutrino Pair (RENP) in atoms is sensitive to the absolute neutrino mass scale, the type of spectrum neutrino masses obey and the nature - Dirac or Majorana - of massive neutrinos. We analyse the possibility to test the hypothesis of existence of neutrinos with masses at the eV scale coupled to the electron in the weak charged lepton current in an RENP experiment. The presence of eV scale neutrinos in the neutrino mixing is associated with the existence of sterile neutrinos which mix with the active flavour neutrinos. At present there are a number of hints for active-sterile neutrino oscillations driven by ?m2 ? 1 eV2. We perform a detailed analysis of the RENP phenomenology within the " 3 + 1" scheme with one sterile neutrino.

Dinh, D. N.; Petcov, S. T.

2015-03-01

426

Astrophysical Neutrino Event Rates and Sensitivity for Neutrino Telescopes  

E-print Network

Spectacular processes in astrophysical sites produce high-energy cosmic rays which are further accelerated by Fermi-shocks into a power-law spectrum. These, in passing through radiation fields and matter, produce neutrinos. Neutrino telescopes are designed with large detection volumes to observe such astrophysical sources. A large volume is necessary because the fluxes and cross-sections are small. We estimate various telescopes' sensitivities and expected event rates from astrophysical sources of high-energy neutrinos. We find that an ideal detector of km^2 incident area can be sensitive to a flux of neutrinos integrated over energy from 10^5 and 10^{7} GeV as low as 1.3 * 10^(-8) * E^(-2) (GeV/cm^2 s sr) which is three times smaller than the Waxman-Bachall conservative upper limit on potential neutrino flux. A real detector will have degraded performance. Detection from known point sources is possible but unlikely unless there is prior knowledge of the source location and neutrino arrival time.

Ivone F. M. Albuquerque; Jodi Lamoureux; George F. Smoot

2002-02-22

427

FAMILY POTYVIRIDAE  

Technology Transfer Automated Retrieval System (TEKTRAN)

The International Committee on the Taxonomy of Viruses potyvirus study group has revised the description of the family Geminiviridae for inclusion in the ICTV 8th report. Characteristic features of each genus within the family is presented. Revised criteria for demarcation and nomenclature of vira...

428

FAMILY GEMINIVIRIDAE  

Technology Transfer Automated Retrieval System (TEKTRAN)

The International Committee on the Taxonomy of Viruses geminivirus study group has revised the description of the family Geminiviridae for inclusion in the ICTV 8th report. Characteristic features of each genus within the family is presented. Revised criteria for demarcation and nomenclature of vi...

429

Family, Extended  

ERIC Educational Resources Information Center

Parents are a child's first and most influential teacher. People hear this truism often, yet nowhere has the author seen it more taken to heart than at Tower Street Elementary School. The school's efforts to form a true partnership with students' families--from involving families in the first day of school, to the principal making home visits, to…

Patton, Jessica Rae

2006-01-01

430

Family Theory and Family Health Research  

PubMed Central

Different family theories can be applied to different aspects of how families experience health and illness. The family health and illness cycle describes the phases of a family's experience, beginning with health promotion and risk reduction, then family vulnerability and disease onset or relapse, family illness appraisal, family acute response, and finally family adaptation to illness and recovery. For each phase, specific family theories that are most appropriate for guiding family and health research are discussed. PMID:21229056

Doherty, William J.

1991-01-01

431

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

432

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

433

Neutrinos from the sun and from radioactive sources  

NASA Astrophysics Data System (ADS)

A brief review of the solar neutrino observations is given. Future solar neutrino measurements are discussed. The use of an artificial neutrino source to be used with low threshold solar neutrino detectors is presented. At present the neutrino source is mainly planned for short baseline neutrino studies.

Ianni, A.; Bellini, G.; Benziger, J.; Bick, D.; Bonfini, G.; Bravo, D.; Buizza Avanzini, M.; Caccianiga, B.; Cadonati, L.; Calaprice, F.; Carraro, C.; Cavalcante, P.; Chavarria, A.; D'Angelo, D.; Davini, S.; Derbin, A.; Etenko, A.; Franco, D.; Fomenko, K.; Galbiati, C.; Gazzana, S.; Ghiano, C.; Giammarchi, M.; Göger-Neff, M.; Goretti, A.; Grandi, L.; Guardincerri, E.; Hardy, S.; Ianni, Andrea; Kayunov, A.; Kobychev, V.; Korablev, D.; Korga, G.; Koshio, Y.; Kryn, D.; Laubenstein, M.; Lewke, T.; Litvinovich, E.; Ludhova, L.; Loer, B.; Lombardi, F.; Lombardi, P.; Machulin, I.; Manecki, S.; Maneschg, W.; Manuzio, G.; Meindl, Q.; Meroni, E.; Miramonti, L.; Misiaszek, M.; Montanari, D.; 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, P. A.; Sabelnikov, A.; 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.

2013-04-01

434

Neutrinos and Nucleosynthesis in Supernova  

E-print Network

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

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

2005-11-12

435

Direct measurements of neutrino mass  

SciTech Connect

Some recent developments in the experimental search for neutrino mass are discussed. New data from Los Alamos on the electron neutrino mass as measured in tritium beta decay give an upper limit of 9.3 eV at the 95% confidence level. This result is not consistent with the long-standing ITEP result of 26(5) eV within a model-independent'' range of 17 to 40 eV. It now appears that the electron neutrino is not sufficiently massive to close the universe by itself. Hime and Jelley report finding new evidence for a 17-keV neutrino in the {Beta} decay of {sup 35}S and {sup 63}Ni. Many other experiments are being reported and the situation is still unresolved. 56 refs., 1 fig., 3 tabs.

Robertson, R.G.H.

1991-01-01

436

The Fermilab neutrino beam program  

SciTech Connect

This talk presents an overview of the Fermilab Neutrino Beam Program. Results from completed experiments as well as the status and outlook for current experiments is given. Emphasis is given to current activities towards planning for a future program.

Rameika, Regina A.; /Fermilab

2007-01-01

437

Solar Neutrino Experiments: New Physics?  

E-print Network

Physics beyond the simplest version of the standard electroweak model is required to reconcile the results of the chlorine and the Kamiokande solar neutrino experiments. None of the 1000 solar models in a full Monte Carlo simulation is consistent with the results of the chlorine or the Kamiokande experiments. Even if the solar models are forced articficially to have a ${}^8 B$ neutrino flux in agreement with the Kamiokande experiment, none of the fudged models agrees with the chlorine observations. This comparison shows that consistency of the chlorine and Kamiokande experiments requires some physical process that changes the shape of the ${}^8 B$ neutrino energy spectrum. The GALLEX and SAGE experiments, which currently have large statistical uncertainties, differ from the predictions of the standard solar model by $2 \\sigma$ and $3 \\sigma$, respectively. The possibility that the neutrino experiments are incorrect is briefly discussed.

John N. Bahcall

1993-07-07

438

Neutrino capital of the world  

E-print Network

Neutrinos are ubiquitous particles, but they don't like to mingle. Each second, billions of them pass through our bodies, slicing imperceptibly through our delicate internal organs. They can barrel through the sun, stars, ...

Johnson, Carolyn Y., 1980-

2004-01-01

439

Neutrino oscillation experiments at CERN  

SciTech Connect

A review is given of the three neutrino oscillation experiments which will be started next spring at CERN-PS. Their main characteristics are presented. Possible analyses with three oscillation parameters are also discussed.

Baldo-Ceolin, M.

1983-01-01

440

Research in Neutrino Physics  

SciTech Connect

Research in Neutrino Physics We describe here the recent activities of our two groups over the first year of this award (effectively November 2010 through January 2012) and our proposed activities and associated budgets for the coming grant year. Both of our groups are collaborating on the Double Chooz reactor neutrino experiment and are playing major roles in calibration and analysis. A major milestone was reached recently: the collaboration obtained the first result on the search for 13 based on 100 days of data from the far detector. Our data indicates that 13 is not zero; specifically the best fit of the neutrino oscillation hypothesis to our data gives sin2 (2 13) = 0.086 ± 0.041 (stat) ± 0.030 (syst) The null oscillation hypothesis is excluded at the 94.6% C.L. This result1 has been submitted to Physical Review Letters. As we continue to take data with the far detector in the coming year, in parallel with completing the construction of the near lab and installing the near detector, we expect the precision of our measurement to improve as we gather significantly more statistics, gain better control of backgrounds through use of partial power data and improved event selection, and better understand the detector energy scale and detection efficiency from calibration data. With both detectors taking data starting in the second half of 2013, we expect to further drive down the uncertainty on our measurement of sin2 (2 13) to less than 0.02. Stancu’s group is also collaborating on the MiniBooNE experiment. Data taking is scheduled to continue through April, by which time 1.18 × 1021 POT is projected. The UA group is playing a leading role in the measurement of antineutrino cross sections, which should be the subject of a publication later this year as well as of Ranjan Dharmapalan’s Ph.D. thesis, which he is expected to defend by the end of this year. It is time to begin working on projects which will eventually succeed Double Chooz and MiniBooNE as the main foci of our efforts. The Stancu group plans to become re–involved in LBNE and possibly also to join NO A, and the Busenitz group has begun to explore joining a direct dark matter search.

Busenitz, Jerome [The University of Alabama

2014-09-30

441

Fourth order evolution equations which describe pseudospherical surfaces  

NASA Astrophysics Data System (ADS)

Differential equations that describe pseudospherical surfaces are considered. These equations are equivalent to the structure equations of a metric with Gaussian curvature K=-1. They can also be described as the compatibility condition of an associated linear problem also referred to as a zero curvature representation. A complete and explicit classification of a class of fourth order evolution equations is given. The classification provides four huge classes (referred to as Types I-IV) of fourth order evolution equations that describe pseudospherical surfaces, together with the associated one (or more) parameter linear problems. The differential equations of each type are determined by choosing certain arbitrary differentiable functions. Fourth-order member of the Burgers hierarchy and a modified Kuramoto-Sivashinsky equation are examples of equations described by Types I and IV, respectively. Many other explicit examples are presented.

Catalano Ferraioli, Diego; Tenenblat, Keti

2014-11-01

442

Standard and non-standard primordial neutrinos  

E-print Network

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

P. D. Serpico

2006-08-14

443

Neutrino scattering and flavor transformation in supernovae.  

PubMed

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

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

2012-06-29

444

Status of non-standard neutrino interactions.  

PubMed

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

Ohlsson, Tommy

2013-04-01

445

Atmospheric neutrinos in Soudan 2.  

SciTech Connect

Soudan 2 has measured the atmospheric neutrino flavor ratio with 4.2 fiducial kiloton-years of exposure. It measures a flavor ratio of 0.66 {+-} 0.11(stat), inconsistent with the expected ratio but consistent with the hypothesis of neutrino oscillations and the Super-Kamiokande data. In a sample of events with good angular resolution, fits to the L/E distribution suggest that {Delta}m{sup 2} > 10{sup {minus}3} eV{sup 2}.

Goodman, M. C.; Soudan 2 Collaboration

1999-03-30

446

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

447

Neutrino Factory Near Detector Simulation  

NASA Astrophysics Data System (ADS)

We present a simulation with GENIE MC generator of the Neutrino Factory baseline near detector interaction rates for the purely leptonic process ??+e-??e+?- and for ??+N??-+X scattering in view of measuring the first one and suppressing the second one for neutrino flux estimation. A set of most sensitive measurable quantities are discussed and their selective power against experimental uncertainties is examined.

Karadzhov, Yordan

2010-03-01

448

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

449

New mixing pattern for neutrinos  

NASA Astrophysics Data System (ADS)

We propose a new mixing pattern for neutrinos with a nonzero mixing angle ?13. Under a simple form, it agrees well with current neutrino oscillation data and displays a number of intriguing features including the ?-? interchange symmetry |U?i|=|U?i|, (i=1, 2, 3), the trimaximal mixing |Ue2|=|U?2|=|U?2|=1/3, the self-complementarity relation ?1+?3=45°, together with the maximal Dirac CP violation as a prediction.

Qu, Huilin; Ma, Bo-Qiang

2013-08-01

450

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

451

Neutrinos And Big Bang Nucleosynthesis  

E-print Network

According to the standard models of particle physics and cosmology, there should be a background of cosmic neutrinos in the present Universe, similar to the cosmic microwave photon background. The weakness of the weak interactions renders this neutrino background undetectable with current technology. The cosmic neutrino background can, however, be probed indirectly through its cosmological effects on big bang nucleosynthesis (BBN) and the cosmic microwave background (CMB) radiation. In this BBN review, focused on neutrinos and, more generally on dark radiation, the BBN constraints on the number of "equivalent neutrinos" (dark radiation), on the baryon asymmetry (baryon density), and on a possible lepton asymmetry (neutrino degeneracy) are reviewed and updated. The BBN constraints on dark radiation and on the baryon density following from considerations of the primordial abundances of deuterium and helium-4 are in excellent agreement with the complementary results from the CMB, providing a suggestive, but currently inconclusive, hint of the presence of dark radiation and, they constrain any lepton asymmetry. For all the cases considered here there is a "lithium problem": the BBN-predicted lithium abundance exceeds the observationally inferred primordial value by a factor of ~3.

Gary Steigman

2012-07-31

452

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

453

Search for Cosmic Background Neutrino Decay  

NASA Astrophysics Data System (ADS)

We present a proposal of an experiment for search for cosmic background neutrino decay. Due to the mass difference between neutrino generations, a heavier neutrino can decay into a lighter neutrino with a photon. Standard model predicts the neutrino lifetime is 1043 year, while the current experimental lower limit of neutrino lifetime is 3 × 1012 year. However, left-right symmetric model suggests much shorter neutrino lifetime down to 1017 year in the shortest. If we assume a mass of the heaviest neutrino is 50 meV, the expected photon energy at the neutrino rest frame is 25 meV. The energy spectrum of the photon from the cosmic background neutrino decay has a cutoff at this energy and a low energy tail due to a red shift effect. Thus we propose an experiment to search for the photon emission from the decay of cosmic background neutrino by measuring the continuous photon energy spectrum in the far infrared wavelength region. We plan to perform a rocket experiment with a superconducting tunnel junction (STJ) detector in 2016 in the earliest, aiming at improving the neutrino lifetime limit by two orders of magnitude. We aim at a 10-hour satellite experiment with 5? sensitivity for the neutrino lifetime of 1017 year.

Kim, Shin-Hong; Takeuchi, Yuji; Nagata, Kazuki; Kasahara, Kota; Okudaira, Takuya; Ikeda, Hirokazu; Matsuura, Shuji; Wada, Takehiko; Ishino, Hirokazu; Itsuki, Atsuko; Mima, Satoshi; Yoshida, Takuo; Kato, Yukihiro; Hazumi, Masashi; Arai, Yasuo; Ramberg, Erik; Yoo, Jong-Hee; Kim, Soo-Bong

454

Neutrino masses: from fantasy to facts  

NASA Astrophysics Data System (ADS)

Theory suggests the existence of neutrino masses, but little more. Facts are coming close to revealing our fantasy: solar- and atmospheric-neutrino data strongly indicate the need for neutrino conversions, while LSND provides an intriguing hint. The simplest ways to reconcile these data in terms of neutrino oscillations invoke a light sterile neutrino in addition to the three active ones. Out of the four neutrinos, two are maximally mixed and lie at the LSND scale, while the others are at the solar-mass scale. These schemes can be distinguished at neutral-current-sensitive solar- and atmospheric-neutrino experiments. I discuss the simplest theoretical scenarios, where the lightness of the sterile neutrino, the nearly maximal atmospheric-neutrino mixing and the generation of ?m {?/2} and ?m {atm/2} all follow naturally from the assumed lepton-number symmetry and its breaking. Although the most likely interpretation of the present data is in terms of neutrino-mass-induced oscillations, one still has room for alternative explanations, such as flavor-changing neutrino interactions, with no need for neutrino mass or mixing. Such flavor-violating transitions arise in theories with strictly massless neutrinos and may lead to other sizeable flavor non-conservation effects, such as ? ? e + ?, ? - e conversion in nuclei, unaccompanied by neutrinoless double-beta decay.

Valle, J. W. F.

455

Neutrino factories: realization and physics potential  

SciTech Connect

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

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

2006-12-01

456

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

457

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

E-print Network

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

Learned, John

458

Survey of atmospheric neutrino data and implications for neutrino mass and mixing  

Microsoft Academic Search

A detailed comparison is made of the atmospheric neutrino results obtained by the Fréjus, IMB-3, and Kamiokande detectors. The implications of these results for vacuum neutrino oscillations are presented, and juxtaposed with the results for matter neutrino oscillations from the solar neutrino data.

E. W. Beier; E. D. Frank; W. Frati; S. B. Kim; A. K. Mann; F. M. Newcomer; R. van Berg; W. Zhang; K. S. Hirata; K. Inoue; T. Ishida; T. Kajita; K. Kihara; M. Nakahata; K. Nakamura; S. Ohara; A. Sakai; N. Sato; Y. Suzuki; Y. Totsuka; Y. Yaginuma; M. Mori; Y. Oyama; A. Suzuki; K. Takahashi; M. Yamada; M. Koshiba; K. Nishijima; T. Kajimura; T. Suda; T. Tajima; K. Miyano; H. Miyata; H. Takei; Y. Fukuda; E. Kodera; Y. Nagashima; M. Takita; H. Yokoyama; K. Kaneyuki; Y. Takeuchi; T. Tanimori

1992-01-01

459

Type II familial synpolydactyly: report on two families with an emphasis on variations of expression.  

PubMed

Type II familial synpolydactyly is rare and is known to have variable expression. However, no previous papers have attempted to review these variations. The aim of this paper was to review these variations and show several of these variable expressions in two families. The classic features of type II familial synpolydactyly are bilateral synpolydactyly of the third web spaces of the hands and bilateral synpolydactyly of the fourth web spaces of the feet. Several members of the two families reported in this paper showed the following variations: the third web spaces of the hands showing syndactyly without the polydactyly, normal feet, concurrent polydactyly of the little finger, concurrent clinodactyly of the little finger and the 'homozygous' phenotype. It was concluded that variable expressions of type II familial synpolydactyly are common and awareness of such variations is important to clinicians. PMID:20717165

Al-Qattan, Mohammad M

2011-01-01

460

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

E-print Network

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

Yi-Lei Tang

2014-11-28

461

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

E-print Network

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

Kenzo Ishikawa; Yutaka Tobita

2012-09-25

462

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

463

Family History  

MedlinePLUS

... Brain Aneurysm Statistics and Facts Seeking Medical Attention Pediatric Aneurysms Brain Aneurysm Causes and Risk Factors Family History Early Detection and Screening Unruptured Brain Aneurysms Subarachnoid Hemorrhage Treatment Options Aneurysm Complications Post ...

464

Tomorrow's Family  

ERIC Educational Resources Information Center

Author states that "...the traditional form of family which has been the norm in recent times in the West will persist, but will be forced to "move over" to accommodate other forms of domestic life." (Author)

Pickett, Robert S.

1977-01-01

465

Family Issues  

MedlinePLUS

... Bullying Prevention Preparedness Tips for Families Tips for First Responders Serving Victims of Crime Take Me Home Emergency Preparedness Related Links Safe and Sound Task Force Voices Blog DONATE BECOME A MEMBER ...

466

FAMILIES FIRST: Keys to Successful Family Functioning Family Roles  

E-print Network

FAMILIES FIRST: Keys to Successful Family Functioning Family Roles Rick Peterson, Extension or family status. An equal opportunity/affirmative action employer. Issued in furtherance of Cooperative. publication 350-093 Types of family Roles Family roles are the recurrent patterns of behavior by which

Liskiewicz, Maciej

467

Family Limitation  

PubMed Central

Dr Robert Smith surveys the history of birth control and sounds a warning for the future of mankind, if the population explosion is allowed to continue unchecked. He stresses the importance of the role of the general practitioner in the limitation of births. Sir Theodore Fox describes the work of the Family Planning Association and stresses that, increasingly, this is a specialist service covering all aspects of fertility. He also feels that the general practitioner has a role in family planning. PMID:5954261

Smith, Robert

1966-01-01

468

Neutrinos and cosmology: a lifetime relationship  

SciTech Connect

We consider the example of neutrino decays to illustrate the profound relation between laboratory neutrino physics and cosmology. Two case studies are presented: In the first one, we show how the high precision cosmic microwave background spectral data collected by the FIRAS instrument on board of COBE, when combined with Lab data, have greatly changed bounds on the radiative neutrino lifetime. In the second case, we speculate on the consequence for neutrino physics of the cosmological detection of neutrino masses even as small as {approx}0.06 eV, the lower limit guaranteed by neutrino oscillation experiments. We show that a detection at that level would improve by many orders of magnitude the existing limits on neutrino lifetime, and as a consequence on some models of neutrino secret interactions.

Serpico, Pasquale D.; /Fermilab

2008-06-01

469

Neutrino physics: What makes the Sun shine  

NASA Astrophysics Data System (ADS)

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

Haxton, Wick

2014-08-01

470

Estimates of Radiation by Superluminal Neutrinos  

E-print Network

We show that the more energetic superluminal neutrinos with quadratically dispersed superluminalities \\delta=\\beta^2-1, for \\beta=v/c where v is the neutrino velocity, also lose significant energy to radiation to the \

B. F. L. Ward

2012-04-07

471

Nuclear physics for geo-neutrino studies  

E-print Network

Geo-neutrino studies are based on theoretical estimates of geo-neutrino spectra. We propose a method for a direct measurement of the energy distribution of antineutrinos from decays of long-lived radioactive isotopes. We present preliminary results for the geo-neutrinos from Bi-214 decay, a process which accounts for about one half of the total geo-neutrino signal. The feeding probability of the lowest state of Bi-214 - the most important for geo-neutrino signal - is found to be p_0 = 0.177 \\pm 0.004 (stat) ^{+0.003}_{-0.001} (sys), under the hypothesis of Universal Neutrino Spectrum Shape (UNSS). This value is consistent with the (indirect) estimate of the Table of Isotopes (ToI). We show that achievable larger statistics and reduction of systematics should allow to test possible distortions of the neutrino spectrum from that predicted using the UNSS hypothesis. Implications on the geo-neutrino signal are discussed.

Gianni Fiorentini; Aldo Ianni; George Korga; Marcello Lissia; Fabio Mantovani; Lino Miramonti; Lothar Oberauer; Michel Obolensky; Oleg Smirnov; Yury Suvorov

2009-08-24

472

Decaying neutrinos: The long way to isotropy  

SciTech Connect

We investigate a scenario in which neutrinos are coupled to a pseudoscalar degree of freedom {phi} and where decays {nu}{sub 1{yields}{nu}2}+{phi} and inverse decays are the responsible mechanism for obtaining equilibrium. In this context we discuss the implication of the invisible neutrino decay on the neutrino-pseudoscalar coupling constant and the neutrino lifetime. Assuming the realistic scenario of a thermal background of neutrinos and pseudoscalar we update the bound on the (off-diagonal) neutrino-pseudoscalar coupling constant to g<2.6x10{sup -13} and the bound on the neutrino lifetime to {tau}>1x10{sup 13} s. Furthermore we confirm analytically that kinetic equilibrium is delayed by two Lorentz {gamma} factors--one for time dilation of the (decaying) neutrino lifetime and one from the opening angle. We have also confirmed this behavior numerically.

Basboell, Anders [Department of Physics and Astronomy, University of Sussex, Brighton, BN1 9QH (United Kingdom); Department of Physics and Astronomy, Aarhus University, DK-8000 Aarhus C (Denmark); Bjaelde, Ole Eggers [Institut fuer Theoretische Physik E, RWTH Aachen University, D-52056 Aachen (Germany); Department of Physics and Astronomy, Aarhus University, DK-8000 Aarhus C (Denmark)

2010-06-15

473

Neutrino mixing, flavor states and dark energy  

E-print Network

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

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

2007-11-06

474

Probing the absolute mass scale of neutrinos  

E-print Network

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

Formaggio, Joseph A.

475

Annual modulation of cosmic relic neutrinos  

E-print Network

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

Safdi, Benjamin R.

476

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

477

Time variations in Kamiokande solar neutrinos data  

SciTech Connect

This paper reports on solar neutrino flux (E{sub nu} {ge} 7.5 MeV) data from 1st January to April 1990 as measured in Kamiokande solar neutrino experiment that have been analyzed statistically and have found that the solar neutrino data varies with the solar activity cycle with very high statistical significance ({gt}98% confidence level). Average solar neutrino flux data in the sunspot minimum range cannot be equal to twice the average solar neutrino flux data in the sunspot maximum range, which suggests that the neutrino flip through the magnetic field of the convection zone of the sun is not responsible for the solar neutrino flux variation. Thus the variation of solar neutrino flux with the solar activity cycle suggests that the solar activity cycle is due to the pulsating character of the nuclear energy generation inside the core of the sun.

Raychaudhuri, P. (Dept. of Applied Mathematics, Calcutta Univ., Calcutta 700009 (IN))

1991-07-20

478

The role of open adoption in the adjustment of adopted children and their families  

Microsoft Academic Search

Findings from a four-year study of over 700 adoptions by non-foster parents indicate that openness has decreased or ceased among a large proportion of adoptions, primarily among those adoptive families who chose openness at the recommendation or insistence of the adoption agency or agent. For all families in the fourth year of their adoption, satisfaction levels and other indicators of

Richard P. Barth; Barbara Needell

1998-01-01

479

Perceptions of School and Family Climates and Experiences of Relational Aggression  

ERIC Educational Resources Information Center

The role of family and school-level variables on relational aggression and relational victimization was investigated among 158 fourth- and fifth-grade children. Family cohesion, maternal and paternal responsiveness, and school climate were hypothesized to be significant predictors of relational aggression and relational victimization. The results…

Pernice-Duca, Francesca; Taiariol, Jennifer; Yoon, Jina

2010-01-01

480

Familial intracranial ependymomas. Report of three cases in a family and review of the literature.  

PubMed

Familial cases of intracranial ependymomas have been well documented in the literature. The authors present two cases from a family in which three members harbored intracranial ependymomas. A 54-year-old man with fourth ventricular ependymoma underwent resection of the tumor followed by radiation therapy. His son presented at age 36 years with a fourth ventricular tanycytic ependymoma and underwent total resection of the ependymoma with postoperative radiation therapy. The father's sister had been treated at another institution for a posterior fossa ependymoma.The association of ependymomas with molecular genetic alterations in chromosome 22 has been previously described. Further investigation of the genetic influences may lead to better therapeutic approaches for this relatively rare clinicopathological entity. PMID:16459998

Dimopoulos, Vassilios G; Fountas, Kostas N; Robinson, Joe Sam

2006-01-01

481

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

482

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

483

The solar neutrino problem and the neutrino magnetic moment  

NASA Astrophysics Data System (ADS)

The physics of the proposed solution to the solar neutrino puzzle based on the neutrino magnetic moment is reviewed. The magnetic moment transition mechanism from active to sterile neutrinos can be either resonant or non-resonant and its kinship to matter enhanced oscillations is shown. The transition probability in the adiabatic approximation is calculated and the limits to adiabaticity are discussed. The full probability incorporating both the adiabatic and non-adiabatic regimes is derived using the Landau-Zener approximation for the non-adiabatic regimes. The available experimental data from the three existing solar neutrino experiments (Davis, Kamiokande II and SAGE) are compared with the results of the theory. From this comparison one can predict for the flavour square mass difference ?2m21 = (0.5-1.5) x 10-8eV2 and for the magnetic moment ? > (6-7) × 10-12 ?B. The uncertainties in the solar magnetic field are considerable and the ansatz used takes a value of 10 5 G along the solar core and the radiation zone, decreasing then linearly along the convection zone. A change in B by one or two orders of magnitude has the main effect of modifying the lower bound on ? by the same proportion, while leaving ?2m21 practically unaltered. An anticorrelation between neutrino flux and solar activity, although consistent with the theory, cannot be clearly predicted.

Pulido, João

1992-02-01

484

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

485

Neutrino-proton and anti-neutrino-proton elastic scattering  

SciTech Connect

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

Fuess, Stuart Charles

1981-01-01

486

Observation of Electron Neutrino Appearance in a Muon Neutrino Beam  

E-print Network

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

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

2014-04-16

487

Transactions of the Fourth Symposium on Space Nuclear Power Systems  

Microsoft Academic Search

This paper contains the presented papers at the fourth symposium on space nuclear power systems. Topics of these papers include: space nuclear missions and applications, reactors and shielding, nuclear electric and nuclear propulsion, refractory alloys and high-temperature materials, instrumentation and control, energy conversion and storage, space nuclear fuels, thermal management, nuclear safety, simulation and modeling, and multimegawatt system concepts. (LSP)

Mohamed S. El-Genk; Mark D. Hoover

1987-01-01

488

16. Parker Dam, only top fourth of dam visible, at ...  

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

16. Parker Dam, only top fourth of dam visible, at 320' high, Parker Dam is one of the highest in the world. Much of this height is because dam penetrates well below river bottom to fasten to bedrock. - Parker Dam, Spanning Colorado River between AZ & CA, Parker, La Paz County, AZ

489

The optimal fourth moment theorem Ivan Nourdin and Giovanni Peccati  

E-print Network

[N4 ]. Also, the following upper bound on the total variation distance holds for every n: dT V (Fn, N the exact rates of convergence in total variation associated with the `fourth moment theorem' by Nualart Fields; Stein's method; Total variation. MSC 2010: 60F05; 60G15; 60H07 1 Introduction and main result

Paris-Sud XI, Université de

490

The Affirmative Action Plan for the NEA. [Fourth Edition].  

ERIC Educational Resources Information Center

This fourth revision of the Affirmative Action Plan (AAP) of the National Education Association (NEA) outlines NEA policy and regulations and incorporates quantitative information on current NEA employment levels and hiring goals for women and minorities. A brief policy statement is followed by a review of objectives, including the general…

National Education Association, Washington, DC.

491

Image Inpainting Using a Fourth-Order Total Variation Flow  

Microsoft Academic Search

We introduce a fourth-order total variation flow for image inpainting proposed in (5). The well-posedness of this new inpainting model is discussed and its ecient numerical real- ization via an unconditionally stable solver developed in (15) is presented.

Martin Burger; Lin He

492

The Online Classroom: Teaching with the Internet. Fourth Edition.  

ERIC Educational Resources Information Center

Presenting a wide array of Internet addresses and sample lessons, this fourth edition shows how teachers can integrate the Internet into their K-12 curriculum to actively involve students. The first section of the book (chapters 1-6) deals with the programs needed to use the Internet, as well as 100 great web sites for teachers, how to manage the…

Cotton, Eileen Giuffre

493

Published: From Animals to Animats, Fourth International Conference  

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Published: From Animals to Animats, Fourth International Conference on Simulation of Adaptive By: James M. Vaccaro CSE 254 June 4, 2002 Learning to Use Selective Attention and Short-Term Memory Information · New Algorithm: U-Tree Algorithm · U-Tree Algorithm Components 1. Utile Distinction Memory 2

Elkan, Charles