'High energy neutrinos' presentation slideshows

HE2: Muons and Neutrinos

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HE2: Muons and Neutrinos

655 views • 65 slides

Multi-Messenger Astronomy

Multi-Messenger Astronomy. AY 17 10/19/2011. Outline. What is Multi-messenger astronomy? Photons Cosmic Rays Neutrinos Gravity-Waves Sample-Return. Outline. What is Multi-messenger astronomy? Photons Cosmic Rays Neutrinos Gravity-Waves Sample-Return.

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682 views • 46 slides

ASTROPARTICLE PHYSICS LECTURE 1

ASTROPARTICLE PHYSICS LECTURE 1. Susan Cartwright University of Sheffield. Overview. What is Astroparticle Physics?. What is Astroparticle Physics?. Various definitions! Mine is the use of particle physics technology to study astrophysical phenomena Included: neutrino astrophysics

541 views • 38 slides

Dan Hooper Particle Astrophysics Center Fermi National Accelerator Laboratory dhooper@fnal

Indirect Searches For Particle Dark Matter. Dan Hooper Particle Astrophysics Center Fermi National Accelerator Laboratory dhooper@fnal.gov. SUSY 2007 August 1, 2007. Dark Matter.

386 views • 38 slides

Thoughts about tagged neutrino beam, GELATRINO proposal at LHC

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The search for extra-terrestrial sources of high energy neutrinos with IceCube

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Astroparticle Physics

Astroparticle Physics. The 2011 ASPERA Roadmap. Christian Spiering, DESY VLVNT-2011, Erlangen, October 14, 2011. ApPEC/ASPERA Roadmap process. Detailed Description Glossy Paper Actual Status &

402 views • 27 slides

Neutrino Astronomy at the South Pole

Neutrino Astronomy at the South Pole. David Boersma UW Madison Lake Louise Winter Institute Chicago, 23 February 2006. IceCube Collaboration. Alabama University, USA University of Alaska, Anchorage, USA Bartol Research Institute, Delaware, USA Pennsylvania State University, USA

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Dan Hooper Particle Astrophysics Center Fermi National Accelerator Laboratory dhooper@fnal

Ultrahigh Energy Cosmic Ray Nuclei and Neutrinos. Dan Hooper Particle Astrophysics Center Fermi National Accelerator Laboratory dhooper@fnal.gov. Aspen Workshop on Cosmic Rays April 2007. The Origin of the Highest Energy Cosmic Rays.

411 views • 26 slides

?.?. ????????, ??? ??? "?????? ???? ?????? ???????? ??????? ??????? (1957-1963)

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Alessandro MIRIZZI (MPI, Munich, Germany)

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Event selection / characterization software package (OpCarac) Alessandro Bertolin (INFN - Padova)

OPERA Collab. Meeting (2/4/09). Event selection / characterization software package (OpCarac) Alessandro Bertolin (INFN - Padova) Ngoc-Tiem Tran (IN2P3 - Lyon) Special thanks section: A. Cases (OpRelease support) S. Dusini (MC generation, useful feedback)

270 views • 17 slides

Ultra-high Energy Neutrinos and Slow Jets of Core Collapse Supernovae

Ultra-high Energy Neutrinos and Slow Jets of Core Collapse Supernovae. Atsushi Watanabe (Harish-Chandra Research Institute). In collaboration with Raj Gandhi (HRI) Abhijit Samanta (HRI). 8 th Jan, 2009 @ NuHoRIzons, HRI, Allahabad. Cosmic neutrinos.

273 views • 16 slides

TeV ? -rays and ? from nuclei photodissociation

TeV ? -rays and ? from nuclei photodissociation. TeV Particle Astrophysics II 28-31 August 2006, Madison, WI, USA. in collaboration with Luis Anchordoqui, John Beacom, Haim Goldberg and Tom Weiler. HE ? -rays. Electromagnetic processes. Hadronic processes. Nuclei photodisintegration.

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A Search for Point Sources of High Energy Neutrinos with AMANDA-B10

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Eliminating Nuclear Bombs with Ultra-High Energy Neutrinos

Eliminating Nuclear Bombs with Ultra-High Energy Neutrinos. Hiroyuki Hagura (KEK) Hirotaka Sugawara (Univ. of Hawaii) Toshiya Sanami (KEK). Outline. Introduction Mean free paths of neutrinos What is a nuclear weapon?

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Ultra-high energy upward going muons in Super-Kamiokande II Ariana S. Minot (Duke University)

Super Kamiokande. Tokyo. Ultra-high energy upward going muons in Super-Kamiokande II Ariana S. Minot (Duke University). Ultra-high energy upward-going muons (E>1 TeV) are created by the interactions of very high energy neutrinos inside the Earth. They could be produced

131 views • 1 slides

IceCube

single neutrinos average of two neutrinos. 2 o x 2 o. 250 n m a day for IceCube. GRB/SN time -window:100 sec. Detecting high energy neutrinos from Supernovae. While core-collapse SNe are guaranteed sources of low-energy neutrinos,

206 views • 1 slides