33_-_Ultra_High_Energy - Ultra High Energy Cosmic Rays B r...

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Unformatted text preview: Ultra High Energy Cosmic Rays B r e a k i n g N e w s ! 2 2 Outline High Energy Cosmic Ray Data Acceleration Issues Particle Attenuation Pierre Auger Observatory Interim Results AGN Milky Way Conclusions References 3 3 Units 1 EeV = 1 Exa-electron Volt = 1x10 18 eV. The interesting range is 60 to 200 EeV! Typical flux (E>100 EeV) < 1 / km 2 century. A very large area detector is required! The state of Rhode Island for example. 4 4 The Low Energy Cosmic Ray Spectrum 100 GeV 1 TeV LHC 5 5 Observed High Energy CR Spectrum 1TeV 1PeV 100 GeV 1EeV Todays Topic! LHC Tevatron 1 TeV 1PeV 12.5 mag F E-2.5 6 6 Questions How are particles, protons, accelerated to such high energies? What are the key sources of opacity? Does the arrival direction point back to the source location? 7 7 Acceleration (Fermi 1954) The only handle we have is the EM field. Fermis insight: (1954) a proton is tied to a single magnetic flux line, that flux line, and its neighbors, are imbedded in the ionized gas, gas dynamics, shocks, can increase the flux density enough to reverse the direction of the proton, this process can shuttle the proton back and forth if the mirrors are moving toward each other, the protons energy in increased at each reflection....
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This note was uploaded on 04/05/2009 for the course ASTRO 3332 taught by Professor Houck,j during the Spring '09 term at Cornell University (Engineering School).

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33_-_Ultra_High_Energy - Ultra High Energy Cosmic Rays B r...

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