'Magnetic field amplification' diaporamas de présentation

ACCELERATION AND PROPAGATION OF GALACTIC COSMIC RAYS

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ACCELERATION IN SHOCKS Introduction ISM and magnetic fields Generalities on SNRs

COSMIC RAYS An Introduction Pham Ngoc Diep Vietnam Auger Training LaboratorY (VATLY) Institute for Nuclear Science and Technology (INST) Quy Nhon, August, 2013. ACCELERATION IN SHOCKS Introduction ISM and magnetic fields Generalities on SNRs Generalities on shocks

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Alexander V. Getling

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Shock acceleration II

Shock acceleration II. Toward a more realistic picture of shock acceleration. Expected shape of spectrum : Differential index a ~ 2.1 for diffusive shock acceleration a observed ~ 2.7 ; a source ~2.1; Da ~ 0.6 ? t esc (E) ~ E -0.6 c t esc ? T disk ~100 TeV ? Isotropy problem

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Diffusive shock acceleration & magnetic field amplification Tony Bell University of Oxford

Diffusive shock acceleration & magnetic field amplification Tony Bell University of Oxford Rutherford Appleton Laboratory. SN1006: A supernova remnant 7,000 light years from Earth

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Evolutionary tracks of magnetic bright points as seen by IMaX/Sunrise

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High Energy ? -rays

High Energy ? -rays. Roger Blandford KIPAC Stanford. The Electromagnetic Spectrum. ir. o. uv. x. g. mm. r. smm. 100TeV. m e c 2. m p c 2. 100neV. 1GeV. High Energy ? -rays. Multi-Messenger Science. High Energy ? -rays. Signals!. Electromagnetic. Cosmic Rays. Strong

311 views • 16 slides