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SUMMARY:TeV-PeV Cosmic Rays Propagating in our Galaxy: The Diffusion Appro
 ximation and Beyond
DTSTART;VALUE=DATE-TIME:20120425T100000Z
DTEND;VALUE=DATE-TIME:20120425T111500Z
DTSTAMP;VALUE=DATE-TIME:20130521T221125Z
UID:indico-event-162649@cern.ch
DESCRIPTION:evo connection URL:http://evo.caltech.edu/evoNext/koala.jnlp?m
 eeting=MvM2Ml2v2tD9Di9D9eDe9v\nAbstract:\n"The Cosmic Ray (CR) flux at Ear
 th mostly consists of energetic protons and nuclei. CRs with TeV-PeV energ
 ies are thought to be accelerated in Galactic supernovae remnants\, althou
 gh an unambiguous proof is still missing. On their way to the observer\, C
 Rs scatter on inhomogeneities of the Galactic magnetic field. Consequently
 \, the propagation of CRs in the Milky Way resembles a random walk\, and c
 an be described as a diffusive process through the "diffusion approximatio
 n". After reviewing the current knowledge in the field\, we will discuss t
 wo important and topical cases in which the diffusion approximation starts
  to fail. First\, we will propose an explanation for the enigmatic anisotr
 opies that are observed at small angular scales on the sky in the CR arriv
 al directions at Earth. Second\, we will show that CR densities around the
 ir sources should be expected to be -moderately to strongly- anisotropic\,
  which in turn has important implications for gamma ray astronomy."\n\nhtt
 p://indico.cern.ch/conferenceDisplay.py?confId=162649
LOCATION:bergen 366
URL:http://indico.cern.ch/conferenceDisplay.py?confId=162649
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