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

Slides:



Advertisements
Similar presentations
1 Neutrino Oscillations Gianluigi Fogli Università di Bari [ The most exciting Adventure in Physics of the last ten years ] Laurea ad Honorem to Prof.
Advertisements

Neutrinos Beck Róbert Fizikus MSc II. ELTE TTK.
High Energy Neutrino Telescopes. The current status of knowledge..
Neutrino oscillations/mixing
Neutrinos 2. Neutrino scattering
Possible anomalous magnetic moment and spin- flavor neutrino precession Lev I. Dorman a,b (a) Israel Cosmic Ray and Space Weather Center and Emilio Segre’
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%
 Rafael Sierra. 1) A short review of the basic information about neutrinos. 2) Some of the history behind neutrinos and neutrino oscillations. 3) The.
By Miriam Aczel. What are neutrinos? They are almost massless— hardly feel the force of gravity They have no electric charge— don’t feel the electromagnetic.
Queen’s University, Kingston, ON, Canada
Atmospheric Neutrino Anomaly
Solar & Atmospheric. June 2005Steve Elliott, NPSS Outline Neutrinos from the Sun The neutrinos Past experiments What we know and what we want to.
11/4/03Prof. Lynn Cominsky1 Class web site: Office: Darwin 329A and NASA E/PO (707) Best way to reach.
8/5/2002Ulrich Heintz - Quarknet neutrino puzzles Ulrich Heintz Boston University
APS Neutrino Study: Reactor Working Group Beyond   Gabriela Barenboim.
Neutrino Mass By Ben Heimbigner.
Lecture 1: Neutrinos and their masses
Peggy Norris, Black Hills State Univ/Sanford Underground Laboratory at Homestake.
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%
Chapter three Sun’s model Major contributions in building the Sun’s model have been made by Eddington (1930’s), Hoyle (1950’s),Bahcall, Clayton (1980’s)
Zachary Robinson Phys 406.  What creates the sun’s energy? ◦ Composition of Sun ◦ Fusion in the Sun (and other stars)  Creation of the elements  Studying.
T HE D AVIS E XPERIMENT AT H OMESTAKE Physics of Atomic Nuclei Peggy Norris,
Solar Neutrinos Dr Robert Smith Astronomy Centre University of Sussex.
The Solar Neutrino Problem Barbara Sylwester Zakład Fizyki Słońca CBK PAN.
Welcome to SNOLAB And to the Neutrino Geoscience Conference Art McDonald Queen’s University, Kingston Director, SNO Institute (+)
O n t h e T r a c k o f M o d e r n P h y s i c s Wolfgang Pauli was a scientist with "NO" in his mind. Pauli's exclusion principle, that two electrons.
Methods and problems in low energy neutrino experiments (solar, reactors, geo-) I G. Ranucci ISAPP 2011 International School on Astroparticle physics THE.
Class Reference: K&R Chapter 3.1 and links given in these slides NOT the FULL ppt. Look at the pdf for the lecture slides, and look here for those subset.
Made by Stanislav Hristov. Why Solar Neutrino?  Examining solar neutrino allows us to find what the physics of the Sun’s core is.  The Sun produces.
The Standard Solar Model and Experiments Predictions versus experiments Uncertainties in predictions Challenges and open questions BP00: astro-ph/
Wednesday, Feb. 14, 2007PHYS 5326, Spring 2007 Jae Yu 1 PHYS 5326 – Lecture #6 Wednesday, Feb. 14, 2007 Dr. Jae Yu 1.Neutrino Oscillation Formalism 2.Neutrino.
Neutrino Nobel Prize overview
Analysis of Alpha Background in SNO Data Using Wavelet Analysis
Cecilia Lunardini Institute for Nuclear Theory University of Washington
Black-body radiation: Planck distribution (Rayleigh-Jeans, Wien distributions) Wien’s Law Stefan(-Boltzmann) Law.
J. Goodman – January 03 The Solution to the Solar Problem Jordan A. Goodman University of Maryland January 2003 Solar Neutrinos MSW Oscillations Super-K.
Neutrinos: What we’ve learned and what we still want to find out Jessica Clayton Astronomy Club November 10, 2008.
Particle Physics: Status and Perspectives Part 7: Neutrinos Manfred Jeitler.
The Troublesome Kid An introductory course on neutrino physics (III) J.J. Gómez-Cadenas IFIC-Valencia Summer Student School CERN, July,2006.
Masatoshi Koshiba Raymond Davis Jr. The Nobel Prize in Physics 2002 "for pioneering contributions to astrophysics, in particular for the detection of cosmic.
Neutrino Pendulum A mechanical model for 3-flavor Neutrino Oscillations Michael Kobel (TU Dresden) Obertrubach, Schule für Astroteilchenphysik.
Seeing the Sky Underground The Birth of Neutrino Astronomy Chiaki Yanagisawa Stony Brook University October 13, 2007 Custer Institute.
Super-Kamiokande and Neutrino Oscillation
Kam-Biu Luk 28 Nov, 2003 Neutrino at Daya Bay Kam-Biu Luk University of California, Berkeley and Lawrence Berkely National Laboratory.
Particle Physics Timeline 1895 X-rays discovered by W. Roentgen 1897 Electron discovered by J.J. Thompson 1905 Photons proposed by A. Einstein 1911 Nucleus.
Birth of Neutrino Astrophysics
P Spring 2002 L18Richard Kass The Solar Neutrino Problem M&S Since 1968 R.Davis and collaborators have been measuring the cross section of:
Solar Neutrinos By Wendi Wampler. What are Neutrinos? Neutrinos are chargeless, nearly massless particles Neutrinos are chargeless, nearly massless particles.
Neutrino. Game Board FERMILABHAPPENINGSFIRSTSNEUTRINOSDETECTION.
STELLAR EVOLUTION – THE STANDARD SOLAR MODEL AND SOLAR NEUTRINOS – MARIE ZECH.
Solar Neutrinos Learning about the core of the Sun Guest lecture: Dr. Jeffrey Morgenthaler Jan 26, 2006.
Solar Neutrinos & Homestake or Something new under the Sun Kevin T. Lesko Lawrence Berkeley National Laboratory Berkeley, CA.
Georg Raffelt, MPI Physics, Munich Neutrinos in Astrophysics and Cosmology, NBI, 23–27 June 2014 Crab NebulaNeutrinos in Astrophysics and Cosmology Introductory.
Solar neutrino physics The core of the Sun reaches temperatures of  15.5 million K. At these temperatures, nuclear fusion can occur which transforms 4.
Neutrino Masses and Flavor Mixing H. Fritzsch LMU Munich.
The (Past &) Future of Neutrino Physics
Flavor Mixing of quarks.
HCP: Particle Physics Module, Lecture 4
Solar Neutrino Problem
Pauli´s new particle * nt nm ne e m t Beta-Decay Pa 234 b (electron)
Solar neutrinos: form their production to their detection
Field Photos
Testing Seesaw at LHC 郑亚娟.
7. Internal structure. II.
Neutrino Physics & Astrophysics : Overview
2. Solar Neutrinos 2.1 Super-K
1930: Energy conservation violated in β-decay
Solar neutrinos and oscillations
Neutrino JEOPARDY!.
Presentation transcript:

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

Homestake Mine ,800 feet underground 100,000 gallon tank perchloroethylene Found only 1/3 of theoretically expected solar neutrinos John Bahcall and Raymond Davis Solar Neutrino Problem (Cl becomes Ar )

Kamiokande in Japan SAGE in Russia GALLEX in Italy Super Kamiokande in Japan SNO (Sudbury Neutrino Observatory) in Ontario, Canada detected neutrino oscillation 2002 Nobel Prize Davis Koshiba Cosmic Neutrinos photo- multiplyers

Pontecorvo Neutrino Oscillations km/GeV

Action

GSI Experiment Paul Kienle et al.

But:

Presented at 3 rd Stueckelberg Workshop on Presented at 3 rd Stueckelberg Workshop on Relativistic Field Theories July 2008 Relativistic Field Theories July 2008

THE END