A precise determination of the number of families with light neutrinos and of the Z boson partial widths

Décamp, D.; Deschizeaux, B.; Lees, J. P.; Minard, M.-N.; Crespo, J.M.; Delfino, M.; Fernández, E.; Martı́nez, M.; Miquel, R.; Mir, L. M.; Orteu, S.; Pacheco, A.; Perlas, J. A.; Tubau, E.; Catanesi, M. G.; Palma, M. De; Farilla, A.; Iaselli, G.; Mäggi, G.; Natali, S.; Nuzzo, S.; Ranieri, A.; Raso, G.; Romanò, F.; Ruggieri, F.; Selvaggi, G.; Silvestris, L.; Tempesta, P.; Zito, G.; Hu, H.; Huang, D.; Lin, J.; Ruan, T.; Wang, T.; Wu, W.; Xie, Y.; Xu, D.; Xu, R.; Zhang, J.; Zhao, W.; Albrecht, H.; Atwood, W. B.; Bird, F.; Blucher, E.; Burnett, T. H.; Charity, T.; Drevermann, H.; Garrido, Ll.; Grab, C.; Hagelberg, R.; Haywood, S. J.; Jost, B.; Kasemann, M.; Kellner, G.; Knobloch, J.; Lacourt, A.; Lehraus, I.; Löhse, T.; Lüke, D.; Marchioro, A.; Mató, P.; May, J.; Minten, A.; Miotto, A.; Palazzi, P.; Pepe-Altarelli, M.; Ranjard, F.; Roth, A.; Rothberg, J.; Rotscheidt, H.; Rüden, W. von; Denis, R. St.; Schlatter, D.; Takashima, M.; Talby, M.; Taureg, H.; Tejessy, W.; Wachsmuth, H.; Wheeler, S.; Wiedenmann, W.; Witzeling, W.; Wotschack, J.; Ajaltouni, Z.; Bardadin-Otwinowska, M.; Falvard, A.; Henrard, P.; Jousset, J.; Michel, B.; Montret, J. C.; Pallin, D.; Perret, P.; Proriol, J.; Prujhière, F.; Hansen, J. D.; Hansen, P. H.; Möllerud, R.; Petersen, G.; Simopoulou, E.; Vayaki, A.; Badier, J.; Blondel, A.; Bonneaud, G. R.; Bourotte, J.; Braems, F.; Brient, J. C.; Ciocci, M. A.; Fouque, G.; Guirlet, R.; Rougé, A.; Rumpf, M.; Tanaka, R.; Videau, H.; Videau, I.; Candlin, D. J.; Conti, A.; Parrini, G.; Corden, M.; Georgiopoulos, C.; Goldman, J.H.; Ikeda, M.; Lannutti, J.; Levinthal, D.; Mermikides, M.; Sawyer, L.; Stimpfl, G.; Antonelli, A.; Baldini, R.; Bencivenni, G.; Bologna, G.; Bossi, F.; Campana, P.; Capon, G.; Chiarella, V.; Ninno, G. De; D’Ettorre-Piazzoli, B.; Felici, G.; Laurelli, P.; Mannocchi, G.; Murtas, F.; Murtas, F.; Nicoletti, G.; Picchi, P.; Zografou, P.; Altoon, B.; Boyle, O.; Halley, A.W.; Have, I. ten; Hearns, J. L.; Hughes, I. S.; Lynch, J.G.; Morton, W. T.; Raine, C.; Scarr, J. M.; Smith, K. M.; Thompson, A. S.; Brandl, B.; Braun, O.; Geiges, R.; Geweniger, C.; Hanke, P.; Hepp, V.; Kluge, E. E.; Maumary, Y.; Panter, M.; Putzer, A.; Rensch, B.; Stahl, A.; Tittel, K.; Wunsch, M.; Belk, A. T.; Beuselinck, R.; Binnie, D. M.; Cameron, W.; Cattaneo, M.; Dornan, P. J.; Dugeay, S.; Forty, R.; Greene, A. M.; Hassard, J. F.; Patton, S.; Sedgbeer, J. K.; Taylor, G. P.; Tomalin, I. R.; Wright, Alison; Girtler, P.; Kühn, D.; Rudolph, G.; Bowdery, C. K.; Brodbeck, T. J.; Finch, A. J.; Foster, F.; Hughes, G.; Keemer, N. R.; Nuttall, M.; Rowlingson, B. S.; Sloan, T.; Snow, W. M.; Barczewski, T.; Bauerdick, L. A. T.; Kleinknecht, K.; Renk, B.; Roehn, S.; Sander, H. G.; Schmelling, M.; Steeg, F.; Albanèse, J.P.; Aubert, J.J.; Benchouk, C.; Bonissent, A.; Courvoisier, D.; Etienne, F.; Matsinos, E.; Papalexiou, S.; Payre, P.; Pietrzyk, B.; Qian, Z.; Blum, W.; Cattaneo, P. W.; Cowan, G.; Dehning, B.; Dietl, H.; Fernández-Bosman, M.; Hauff, D.; Jahn, A.; Lange, E.; Lütjens, G.; Lütz, G.; Männer, W.; Guenther, J.; Richter, R.; Schwarz, A. S.; Settles, R.; Stiegler, U.; Stierlin, U.; Thomas, J. P.; Waltermann, G.; Bertín, V.; Bouard, G. de; Boucrot, J.; Callot, O.; Chen, X.; Cordier, A.; Davier, M.; Ganis, G.; Grivaz, J.-F.; Heusse, P.; Janot, P.; Journé, V.; Kim, D. W.; Lefrançois, J.; Lutz, A.M.; Veillet, J. J.; Zomer, F.; Amendolia, S. R.; Bagliesi, G.; Batignani, G.; Bosisio, L.; Bottigli, U.; Bradaschia, C.; Ferrante, I.; Fidecaro, F.; Foà, L.; Focardi, E.; Forti, F.; Giassi, A.; Giorgi, M. A.; Ligabue, F.; Lusiani, A.; Mannelli, E. B.; Marrocchesi, P. S.; Messineo, A.; Palla, F.; Sanguinetti, G.; Scapellato, S.; Steinberger, J.; Тенчини, Р.; Tonelli, G.; Triggiani, G.; Carter, J. M.; Green, M. G.; March, P.V.; Medcalf, T.; Saich, M.; Strong, J. A.; Thomas, R. M.; Wildish, T.; Botterill, D.; Clifft, R. W.; Edgecock, R.; Edwards, M.; Fisher, S. M.; Harvey, J.; Jones, T. J.; Norton, P. R.; Salmon, D. P.; Thompson, J.C.; Aubourg, E.; Bloch-Devaux, B.; Colas, P.; Klopfenstein, C.; Lançon, E.; Locci, E.; Loucatos, S.; Mirabito, L.; Monnier, E.; Pérez, P.; Perrier, Frédéric; Rander, J.; Renardy, J. F.; Roussanrie, A.; Schuller, J. P.; Ashman, J. G.; Booth, C. N.; Combley, F.; Dinnsdale, M.; Martin, J. P.; Parker, D.; Thompson, L.F.; Brandt, Siegmund; Burkhardt, Hans; Grupen, C.; Meinhard, H.; Neugebauer, E.; Schäfer, U.; Seywerd, H.; Gobbo, B.; Liello, F.; Millotti, E.; Ragusa, F.; Rolandi, G.; Bellantoni, L.; Boudreau, J.; Cinabro, D.; Conway, J.; Cowen, D. F.; Feng, Z.; Harton, J. L.; Hilgart, J.; Jared, R. C.; Johnson, R.P.; LeClaire, B. W.; Pan, Y.; Parker, T.E.; Pater, J. R.; Saadi, Y.; Sharma, V.; Wear, J.; Weber, F. V.; Wu, S. L.; Xue, S.; Zobernig, G.

doi:10.1016/0370-2693(90)91984-j

Cited by 110 publications

(12 citation statements)

References 24 publications

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“…For example, all fi masses are bound to be larger than~43 GeV because of this measurement. This is similar to the bound on the number of light neutrino species [17].…”

Section: -Osupporting

confidence: 59%

Supersymmetric versions of the standard model

Gouvea¹,

Andre²

1999

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“…For example, all fi masses are bound to be larger than~43 GeV because of this measurement. This is similar to the bound on the number of light neutrino species [17].…”

Section: -Osupporting

confidence: 59%

Supersymmetric versions of the standard model

Gouvea¹,

Andre²

1999

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“…In fact, measurements of the invisible Z-boson decay width (see e.g. [1]) and cosmological considerations (see e.g. [2]) tell us that there are only three active neutrino species, which are ν eL , ν µL , ν τ L (along with their antiparticles), and therefore right-handed Dirac neutrinos should be nearly sterile in any extension of the SM (with any additional particles and interactions).…”

Section: Introductionmentioning

confidence: 99%

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

Lychkovskiy

Блинников

2010

Phys. Atom. Nuclei

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Neutrino with magnetic moment can experience a chirality flip while scattering off charged particles. This effect may lead to important consequences for the dynamics and the neutrino signal of the core-collapse supernova. It is known that if neutrino is a Dirac fermion, then nu_L->nu_R transition induced by the chirality flip leads to the emission of sterile right-handed neutrinos. The typical energies of these neutrinos are rather high, E ~ (100-200)MeV. Neutrino spin precession in the magnetic field either inside the collapsing star or in the interstellar space may lead to the backward transition, nu_R->nu_L. Both possibilities are known to be interesting. In the former case high-energy neutrinos can deliver additional energy to the supernova envelope, which can help the supernova to explode. In the latter case high-energy neutrinos may be detected simultaneously with the "normal" supernova neutrino signal, which would be a smoking gun for the Dirac neutrino magnetic moment. We report the results of the calculation of the supernova right-handed neutrino luminosity up to 250 ms after bounce. They allow to refine the estimates of the energy emitted in right-handed neutrinos. Also the sensitivity of water Cherenkov detectors to the Dirac neutrino magnetic moment is estimated. For mu_Dirac=10^{-13}mu_B Super-Kamiokande is expected to detect at least few high-energy events from a galactic supernova explosion. Also we briefly discuss the case of Majorana neutrino magnetic moment. It is pointed out that spin flips may quickly equilibrate electron neutrinos with non-electron antineutrinos if mu_Majorana~10^{-12}mu_B. This may lead to various consequences for supernova physics.Comment: Submitted to a special issue of Yadernaya Fizika (Physics of Atomic Nuclei) dedicated to 80th birthday of L.B. Oku

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“…The discovery of the tau lepton in 1975 [9] led to the prediction of the associated tau neutrino (ν τ ). The first indirect evidence for the ν τ came in 1989 when the ALEPH collaboration made measurements of the mass and decay width of the Z gauge boson [10]. From the width of the mass peak (shown in Figure 1.2), they were able to place a limit on the number of light (m ν < m Z /2) neutrinos to be 2.9840 ± 0.0082 corresponding to the three generations of leptons that had been discovered.…”

Section: Brief History Of Neutrino Physicsmentioning

confidence: 99%

Measurement of the Inclusive Electron-Neutrino Charged-Current Cross Section in the NO$\nu$A Near Detector

Judah

2019

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MEASUREMENT OF THE INCLUSIVE ELECTRON-NEUTRINO CHARGED-CURRENT CROSS SECTION IN THE NOνA NEAR DETECTORThis thesis describes the methods used to extract the inclusive ν e charged-current cross section in the NOνA near detector using data collected from November 2014 to February 2017, corresponding to an exposure of 8.09 ×10 20 protons-on-target of a primarily neutrino beam. The near detector is located at Fermilab, 800 m from the primary target. The neutrino beam peaks near 2 GeV and is able to probe a variety of different neutrino-nucleus interactions through their finalstate characteristics. The flux-integrated double-differential cross section is measured with respect to the final-state electron kinematics, as well as the total cross-section as a function of neutrino energy integrated over the same phase space used for the double-differential measurement.6.1 Flow chart of the single node temperature monitoring software .

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A precise determination of the number of families with light neutrinos and of the Z boson partial widths

Cited by 110 publications

References 24 publications

Supersymmetric versions of the standard model

Supersymmetric versions of the standard model

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

Measurement of the Inclusive Electron-Neutrino Charged-Current Cross Section in the NO$\nu$A Near Detector

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