APS Neutrino Study: Reactor Working Group Beyond   Gabriela Barenboim.

Slides:

Advertisements

Similar presentations

Double Chooz: Collaboration, Experimental concept, Detector, Physics Prospect, Status & Schedule, Summary.

Advertisements

Neutrino mixing angle θ 13 In a SUSY SO(10) GUT Xiangdong Ji Peking University University of Maryland.

Neutrinos Louvain, February 2005 Alan Martin Arguably the most fascinating of the elementary particles. Certainly they take us beyond the Standard Model.

Teppei Katori, Indiana University1 PRD74(2006) Global 3 parameter Lorentz Violation model for neutrino oscillation with MiniBooNE Teppei Katori,

Neutrino oscillations/mixing

Recent Discoveries in Neutrino Physics: Understanding Neutrino Oscillations 2-3 neutrino detectors with variable baseline 1500 ft nuclear reactor Determining.

Neutrino emission =0.27 MeV E=0.39,0.86 MeV =6.74 MeV ppI loss: ~2% ppII loss: 4% note: /Q= 0.27/26.73 = 1% ppIII loss: 28% Total loss: 2.3%

Status of Neutrino Science Hitoshi Murayama LBNLnu April 11, 2003.

G. Sullivan - Princeton - Mar 2002 What Have We Learned from Super-K? –Before Super-K –SK-I ( ) Atmospheric Solar –SNO & SK-I Active solar –SK.

Observational Cosmology - a laboratory for fundamental physics MPI-K, Heidelberg Marek Kowalski.

Solar Neutrinos, Neutrino Cross Sections, and NUSEL Developments A.B. Balantekin ORNL SNS Workshop August 28, 2003.

Neutrino Mass and Mixing David Sinclair Carleton University PIC2004.

Observational Cosmology - a unique laboratory for fundamental physics Marek Kowalski Physikalisches Institut Universität Bonn.

Neutrino Physics - Lecture 1 Steve Elliott LANL Staff Member UNM Adjunct Professor ,

3 Neutrino Oscillation and Off-axis Experiments David Barnhill UCLA May 30, 2003.

CP-phase dependence of neutrino oscillation probability in matter 梅 (ume) 田 (da) 義 (yoshi) 章 (aki) with Lin Guey-Lin ( 林貴林 ) National Chiao-Tung University.

Mass-varying neutrino oscillations Danny Marfatia University of Kansas with V. Barger and K. Whisnant (hep-ph/ )

Reactor & Accelerator Thanks to Bob McKeown for many of the slides.

1 Evidence of Neutrino Oscillation from Super-Kamiokande and K2K Neutrino physics at Super-Kamiokande –Detector overview –Atmospheric neutrinos –Solar.

Neutrino Physics Steve Elliott LANL Nuclear Physics Summer School 2005.

A LOOK INTO THE PHYSICS OF NEUTRINOS J A Grifols, UAB Viña del Mar, Dec 06.

Reactor Working Group Report

J. Goodman – May 2003 Quarknet Symposium May 2003 Neutrinos, Dark Matter and the Cosmological Constant The Dark Side of the Universe Jordan Goodman University.

The International Linear Collider Barry Barish IUPAP General Assembly Cape Town 26-Oct-05.

Neutrino emission =0.27 MeV E=0.39,0.86 MeV =6.74 MeV ppI loss: ~2% ppII loss: 4% note: /Q= 0.27/26.73 = 1% ppIII loss: 28% Total loss: 2.3%

NEUTRINO PROPERTIES J.Bouchez CEA-Saclay Eurisol town meeting Orsay, 13/5/2003.

The Importance of Low-Energy Solar Neutrino Experiments Thomas Bowles Los Alamos National Laboratory Markov Symposium Institute for Nuclear Research 5/13/05.

Recent Results from Super-Kamiokande and Sudbury Neutrino Observatory R. D. McKeown California Institute of Technology January 17, 2004 IHEP Beijing.

The Elementary Particles. e−e− e−e− γγ u u γ d d The Basic Interactions of Particles g u, d W+W+ u d Z0Z0 ν ν Z0Z0 e−e− e−e− Z0Z0 e−e− νeνe W+W+ Electromagnetic.

Solar neutrino measurement at Super Kamiokande ICHEP'04 ICRR K.Ishihara for SK collaboration Super Kamiokande detector Result from SK-I Status of SK-II.

Neutrino oscillation physics II Alberto Gago PUCP CTEQ-FERMILAB School 2012 Lima, Perú - PUCP.

February 23, 2005Neutrino Telescopes, Venice Comparing Solar and KamLAND Data Comparing Solar and KamLAND Data Carlos Pena Garay IAS, Princeton ~

PHY306 1 Modern cosmology 4: The cosmic microwave background Expectations Experiments: from COBE to Planck  COBE  ground-based experiments  WMAP  Planck.

C. W. Kim KIAS The Johns Hopkins University Neutrino Physics and Cosmology SDSS-KSG Workshop.

The Standard Solar Model and Experiments Predictions versus experiments Uncertainties in predictions Challenges and open questions BP00: astro-ph/

Bruno Pontecorvo Pontecorvo Prize is very special for us: All the important works done by Super- Kamiokande point back to Bruno Pontecorvo – 1957 First.

Neutrino oscillation physics Alberto Gago PUCP CTEQ-FERMILAB School 2012 Lima, Perú - PUCP.

Tests of non-standard neutrino interactions (NSI) Cecilia Lunardini Institute for Nuclear Theory University of Washington, Seattle.

Francis Ngouniba Ki Tezpur University, Ind ia Quasi-Degenerate Neutrinos and Leptogenesis Ist IAS-CERN, NTU-SINGAPORE Jan 26, 2012 Specialized Knowledge.

J. Goodman – January 03 The Solution to the Solar Problem Jordan A. Goodman University of Maryland January 2003 Solar Neutrinos MSW Oscillations Super-K.

NEUTRINO MASSES AND OSCILLATIONS NEUTRINO MASSES AND OSCILLATIONS Triumphs and Challenges R. D. McKeown Caltech.

1 Neutrino Phenomenology Boris Kayser Scottish Summer School August 10,

NEUTRINOS: PAST PRESENT FUTURE Heidi Frank Merritt Fest

Impact of Neutrino Oscillation Measurements on Theory Hitoshi Murayama NuFact 03 June 10, 2003.

THE CONNECTION OF NEUTRINO PHYSICS WITH COSMOLOGY AND ASTROPHYSICS STEEN HANNESTAD CERN, 1 OCTOBER 2009 e    

J. Goodman – May 2003 Quarknet Symposium May 2003 Neutrinos, Dark Matter and the Cosmological Constant The Dark Side of the Universe Jordan Goodman University.

Karsten Heeger, LBNL INPAC, October 3, 2003 Reactor Neutrino Oscillation Experiments Karsten M. Heeger Lawrence Berkeley National Laboratory.

Neutrino mass and mixing parameters - a short review - Eligio Lisi INFN, Bari, Italy Rencontres de MoriondMarch 2005 Special thanks to: G.L. Fogli, A.

May 19, 2005UAM-IFT, Madrid : Neutrino physics in underground labs Carlos Pena Garay IAS ~

Michel Gonin – Ecole Polytechnique – France : SUPER NOVA SN1987A Super-Kamiokande Introduction neutrino oscillations mixing matrices Introduction.

Kam-Biu Luk 28 Nov, 2003 Neutrino at Daya Bay Kam-Biu Luk University of California, Berkeley and Lawrence Berkely National Laboratory.

Solar Neutrinos & Homestake or Something new under the Sun Kevin T. Lesko Lawrence Berkeley National Laboratory Berkeley, CA.

Neutrino physics: The future Gabriela Barenboim TAU04.

A model for large non-standard interactions of neutrinos leading to the LMA-dark solution Yasaman Farzan IPM, Tehran.

Neutrino Physics II Hitoshi Murayama University of Pisa February 25, 2003.

A. Y. Smirnov SNO: establishing flavor conversion of the Solar neutrinos BOREXINO direct measurement of the pp-neutrinos 2004 – KAMLAND.

Precise Neutrino Mass Difference Hagen Kleinert, FU BERLIN ICRANet Pescara World`s HIGHEST-FLUX Neutrino Source.

1 A.Zalewska, Epiphany 2006 Introduction Agnieszka Zalewska Epiphany Conference on Neutrinos and Dark Matter, Epiphany Conference on Neutrinos.

(nikhef elevator to 3rd floor)

The (Past &) Future of Neutrino Physics

Non-unitary deviation from the tri-bimaximal mixing and neutrino oscillations Shu Luo The Summer Topical Seminar on Frontier of Particle Physics.

Neutrinos and the Evolution

Neutrino: Completely polarized particle

Probing the Coupling between Dark Components of the Universe

Neutrino mass and mixing: 2006 Status

Neutrino Masses, Leptogenesis and Beyond

Neutrino oscillation physics

Neutrino Masses and Mixings

Neutrino Physics & Astrophysics : Overview

Yifang Wang Institute of High Energy Physics

Presentation transcript:

APS Neutrino Study: Reactor Working Group Beyond   Gabriela Barenboim

K2K  “Indication of neutrino oscillations in a 250 km …” “First Results from KamLAND: Evidence for Reactor …” Nobel Prize award to R. Davis Jr. and M. Koshiba WMAP: First year Wilkinson microwave anysotropy probe observations: determination of cosmological parameters “Precise measurements of the solar neutrino D/N and seasonal variations in Super-Kamiokande” SNO salt phase results: “Measurements of the Total…” Sloan Digital Sky Survey: “Cosmological parameters…”

 m 2 23 = (1.3 – 3.0) eV 2 sin 2 (2  23 ) >.9  m 2 12 = (5.8 – 8.4) eV 2 tan 2 (  12 ) <.52

 the mass hierarchy  the connecting angle    the CP violating phase 

Is there any physics beyond  13 ?

Measure or bound neutrino magnetic moment

Search for oscillation effects of sterile neutrinos

Measure or bound neutrino magnetic moment Search for oscillation effects of sterile neutrinos Measure sin 2  w (check NuTeV result)

Measure or bound neutrino magnetic moment Search for oscillation effects of sterile neutrinos Measure sin 2  w (check NuTeV result) FINeSE at a reactor ?

Measure or bound neutrino magnetic moment Search for oscillation effects of sterile neutrinos Measure sin 2  w (check NuTeV result) FINeSE at a reactor ? Anything interesting about structure functions ?

Measure or bound neutrino magnetic moment Search for oscillation effects of sterile neutrinos Measure sin 2  w (check NuTeV result) FINeSE at a reactor ? Anything interesting about structure functions ? What about supernovas ?

Measure or bound neutrino magnetic moment Search for oscillation effects of sterile neutrinos Measure sin 2  w (check NuTeV result) FINeSE at a reactor ? Anything interesting about structure functions ? What about supernovas ? CPT tests (reactor vs solar neutrinos)

We have measured a cosmological constant that is different from zero

Low Homestake rate ? Absence of the upturn of the spectrum ?

Turn down at low energies ?

Low Homestake rate ? Absence of the upturn of the spectrum ? Next KamLAND data release: still some shift in  m 2 is not excluded….

There is a rich non-  13 program which might help make the  13 program happen.

Measure or bound neutrino magnetic moment Search for oscillation effects of sterile neutrinos Measure sin 2  w (check NuTeV result) FINeSE at a reactor ? Anything interesting about structure functions ? What about supernovas ? CPT tests (reactor vs solar neutrinos)