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1. Neutrino mass and the LHCMiha Nemevšek ICTP, Triestewith Maiezza, Melfo, Nesti, Senjanović, Tello, Vissani and Zhang Balkan Workshop 2011, Donji Milanovac 2. LHC a neutrino…
Slide 1 1 Deep Sea Neutrino Telescope Detection Principle Slide 2 2 Basic Properties of Neutrino Spin: ½ (fermion) Type: lepton Flavors: muonic, electronic, tau Masses:…
Detectors for Super-Beams and Neutrino Factories Kevin McFarland University of Rochester NUFACT ’03 10 June 2003 Kevin McFarland: Detectors Acknowledgements This summary…
Classic Tau Signature “Double Bang” Learned & Pakvasa 1995 νN interaction Tau lepton track ~50 m/PeV (neglecting energy loss) Tau decay TeV Astro II Windows for…
Classic Tau Signature “Double Bang” Learned & Pakvasa 1995 νN interaction Tau lepton track ~50 m/PeV (neglecting energy loss) Tau decay UHE Tau Neutrino Workshop…
49th Rencontres de Moriond Lucia A. Popa March 22-29, 2014 Tension between Planck constraints and local Universe measurements? Planck found quite large changes in some parameters…
Neutrino oscillation results from the T2K experiment ν Tokai Kamioka Neutrino oscillation results from the T2K experiment Kei Ieki, on behalf of the T2K collaboration INPA…
Recent neutrino cross-section measurements at T2K A hot topic... Oscillation measurements in far detector constrained from near detector (xsec x flux) different acceptance
Physics Potential of Future Supernova Neutrino ObservationsAmol Dighe Neutrino 2008 May 25-31, 2008, Christchurch, New Zealand Supernova for neutrino physics and astrophysics
NeutrinoNashville5-20-05.pptExperiment by Tom Kirk Brookhaven National Laboratory Nashville, TN May 23, 2005 T. Kirk May 23, 2005 Physics Case for the VLBNO Experiment •
Microsoft PowerPoint - Stat_DYB.pptxXin Qian BNL – Delayed: n + Gd 8 MeV with 30 us capture time • ~ 200 MeV per fission • ~ 6 anti-νe per fission from
Questions Concha Gonzalez-Garca (YITP-Stony Brook U. & ICREA-U.Barcelona) [email protected] 1 Show that only for a free massless fermion the chirality
Gautam Rupak Mississippi State University Wednesday, May 4, 2011 associated with SN 1680 Wednesday, May 4, 2011 Background -- Neutron star cools by neutrino emissions n→
0.000 0.005 0.010 0.015 0.020 0.025 Ν Μ Ν e MiniBooNE Νe LSND Νe MiniBooNE Νe Νe or Νe 32 best fit Νe or Νe 2Ν best fit NUCLEAR PHYSICS For
Christian Weinheimer Email: [email protected] The Karlsruhe TRItium Neutrino experiment KATRIN KATRIN´s background suppression, statistics & systematics
Microsoft Word - NSF06F.docTO MEASURE THE NEUTRINO LUMINOSITY OF THE SUN 1. INTRODUCTION Numerous experiments have recently shown that neutrino (ν) flavor states are not
Mohammad Rafi Alam† ††RCNP, Osaka University, Japan Outline 3 Results 4 Summary Introduction 3 Results 4 Summary Introduction Motivation τ leptons
Teil 7: Offene Fragen der Teil 7: Offene Fragen der TeilchenphysikTeilchenphysik Teilchenphysik im Experiment Standardmodell 2008 Elektron e-Neutrino Myon su d up-Quark down-Quark…
Experimental neutrino physics from the Finnish perspective Timo Enqvist University of Oulu Particle Physics Day 2016 JYFL – 119 – Experimental neutrino physics from the…
Status of Neutrino Masses and Mixing Carlo Giunti INFN Sezione di Torino and Dipartimento di Fisica Teorica Università di Torino giunti@toinfnit Torino 28 January 2005…