University of Novi Sad Department of Physics

Slides:

Advertisements

Similar presentations

ICECUBE & Limits on neutrino emission from gamma-ray bursts IceCube collaboration Journal Club talk Alex Fry.

Advertisements

The electromagnetic (EM) field serves as a model for particle fields

Announcements 11/14 Today: 9.6, 9.8 Friday: 10A – 10E Monday: 10F – 10H 9.6 Only do differential cross-section See problem 7.7 to do most of the work for.

Lecture 3 – neutrino oscillations and hadrons

 Rafael Sierra. 1) A short review of the basic information about neutrinos. 2) Some of the history behind neutrinos and neutrino oscillations. 3) The.

1 Deep Sea Neutrino Telescope Detection Principle.

Efectos de las oscilaciones de sabor sobre el desacoplamiento de neutrinos c ó smicos Teguayco Pinto Cejas AHEP - IFIC Teguayco Pinto Cejas

The electromagnetic (EM) field serves as a model for particle fields  = charge density, J = current density.

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

P461 - particles VII1 Glashow-Weinberg-Salam Model EM and weak forces mix…or just EW force. Before mixing Bosons are massless: Group Boson Coupling Quantum.

Neutrino Physics - Lecture 2 Steve Elliott LANL Staff Member UNM Adjunct Professor ,

Neutrino Physics Steve Elliott LANL Nuclear Physics Summer School 2005.

Neutrinos Jason Cook. Topics of Interest Neutrinos  History  Sources  Detection  Solar Neutrino Problem  Neutrino Oscillation  Practicality of Neutrinos.

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

Theoretical Particle Physics: Beyond the Standard Model Jonathan Feng UC Irvine UCI Pizza Talk 18 April 2003.

1 The elusive neutrino Piet Mulders Vrije Universiteit Amsterdam Fysica 2002 Groningen.

Neutrino Physics - Lecture 3 Steve Elliott LANL Staff Member UNM Adjunct Professor ,

The International Linear Collider Barry Barish iThemba Cape Town 21-Oct-05.

Modern Physics LECTURE II.

A New Theory of Neutrino Oscillations Netta Engelhardt

P461 - particles VIII1 Neutrino Physics Three “active” neutrino flavors (from Z width measurements). Mass limit from beta decay Probably have non-zero.

A Summer at Fermi National Laboratory In which one math teacher struggles to do pretty much anything…

Massive neutrinos Dirac vs. Majorana

Physics for Scientists and Engineers, 6e Chapter 46 - Particle Physics and Cosmology.

Testing Relativity Theory With Neutrinos Brett Altschul University of South Carolina May 15, 2008.

Option 212: UNIT 2 Elementary Particles Department of Physics and Astronomy SCHEDULE 26-Jan pm LRB Intro lecture 28-Jan pm LRBProblem solving.

Physics Priorities S. Dawson July 11, 2007 Fermilab Steering Committee Meeting.

COSMOLOGY SL - summary. STRUCTURES Structure  Solar system  Galaxy  Local group  Cluster  Super-cluster Cosmological principle  Homogeneity – no.

Weighing neutrinos with Cosmology Fogli, Lisi, Marrone, Melchiorri, Palazzo, Serra, Silk hep-ph , PRD 71, , (2005) Paolo Serra Physics Department.

Neutrino Oscillations in vacuum Student Seminar on Subatomic Physics Fundamentals of Neutrino Physics Dennis Visser

Neutrino Nobel Prize overview

1 FK7003 Lecture 6 ● Isospin ● SU(2) and SU(3) ● Parity.

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

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

weak decays beta decay ofneutron problem energy and momentum not conserved e n p.

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

Super-Kamiokande and Neutrino Oscillation

Feynman Diagrams Richard Feynman invented the concept of virtual photons as part of his theory of quantum electrodynamics. The maths is complicated – but,

Weak Interactions (continued)

High Energy Observational Astrophysics. 1 Processes that emit X-rays and Gamma rays.

CHAPTER 14 Elementary Particles

Lecture 7 Parity Charge conjugation G-parity CP FK7003.

HOW TO TELL DIFFERENCE OF MAJORANA/DIRAC NEUTRINOS

Neutrino Oscillations and T2K

Jan Hamann Rencontres de Moriond (Cosmology) 21st March 2016

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

Countries that signed the nuclear arms treaty with Iran

Physics with the ICARUS T1800 detector

Neutrinos in Cosmology & Astrophysics

The Physics of Neutrinos

Intro to Symmetries Gene Golowich Physics (UMass) Talk at NEPPSR-04

Non-Standard Interactions and Neutrino Oscillations in Core-Collapse Supernovae Brandon Shapiro.

How Particles Interact

Big World of Small Neutrinos

Patterns in Baryons and Mesons

Advanced Topics Nuclear Physics ElementaryParticles General Relativity

Particle Physics Theory

Pauli´s new particle * nt nm ne e m t Beta-Decay Pa 234 b (electron)

Modelling of non-thermal radiation from pulsar wind nebulae

Particle Physics Theory

Weak Interactions (continued)

Methods of Experimental Particle Physics

Future neutrino experiments

Frontiers of fundamental physics

University of Puerto Rico

Neutrino Physics & Astrophysics : Overview

1930: Energy conservation violated in β-decay

Fundamental Particles

Particle Physics and The Standard Model

Neutrino JEOPARDY!.

Presentation transcript:

University of Novi Sad Department of Physics Neutrino: Catch me if you can! University of Novi Sad Department of Physics Branislav Nikolić darthagal@gmail.com

place your bets... lane 1 lane 2

cast: neutrino! - spin 1/2 - smallest mass - only 1 force (W, Z) - very strange particle... photon

no left antineutrinos or right neutrinos! (???) weak force – only left neutrinos and right antineutrinos no left antineutrinos or right neutrinos! (???) - spin vector parallel to momentum vector (right particle) or antiparallel (left particle) left neutrinos and right antineutrinos why the asymetry?! (weak force) - implies non-zero mass of neutrino... ...which we can’t measure.

Solar neutrino problem - neutrinos from the Sun: detected only 1/3 of the predicted number solved: neutrino oscillations (mixing)

produce an electron neutrino and detect a muon neutrino mass states flavor states produce an electron neutrino and detect a muon neutrino neutrino mixing (oscillations) – fundamental problem of New QM

different for antineutrinos! (? CP violation...?)

why neutrinos? why oscillations? nucleosynthesis – sensitive to neutrino oscillations! no neutrinos – no supernovae II (past decade research) > 95% of grav. energy carried away by neutrinos only! “neutrino driven wind” – the essence of explosion!

- neutrinos from the Early Universe - if oscillations then when decoupled from radiation? Cosmic Neutrino Background? Maybe one day... (deeper into past than CMB – even before nucleosynthesis!)

wait a nanosecond...a superluminal neutrino??? GOAL wait a nanosecond...a superluminal neutrino??? wins by 60 nanoseconds!

where is the beauty in that?! - new energies for supernovae - more adjusted explosion mechanisms for supernovae - new energies for nucleosynthesis - new models for nucleosynthesis - no more STR, no more E=mc^2, no more GTR, no more QFT....????? - good bye to Lorentz invariance on macroscopic level?!?! where is the beauty in that?!

- exploring both theoretical (fundamental) and experimental concequences in either case (superluminal or not) are a way to the holy grail in physics and prhaps in astrophysics-cosmology. conclusion: if you want to talk about the connection of micro and makroscopic world, you might want to consider neutrinos.