Titlebook: Origin of Cosmic Rays; Giancarlo Setti,Gianfranco Spada,Arnold W. Wolfend Book 1981 International Astronomical Union 1981 active galactic

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Debrief

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Isotopes of Cosmic Ray Elements from Neon to Nickel,an and Waddington (1975), Young (1979), measures elemental charge from scintillation and Cherenkov signals and mass from Cherenkov and total energy determined from a measure of residual range in nuclear emulsion. The charge resolution obtained ranged from 0.19 to 0.21 charge units between neon and n

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Wolf Rayet Stars and the Origin of the 22Ne Excess in Cosmic Rays,ould be influential in the bulk energization of the local cosmic radiation (Cassé and Paul, 1980). Since wind acceleration is not supposed to accelerate thermal particles, a continuous injection of low energy particles (E ~ 1 to 10 MeV/n) is required. We keep open the possibility that these particle

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CR-39 Plastic Track Detector Experiment for Measurement of Charge Composition of Primary Cosmic Rayormation concerning their origin, acceleration and interstellar propagation. In recent years solid state nuclear track detectors have been employed extensively to study heavy primary cosmic rays. Plastic track detectors necessarily have large geometric factors for heavy primaries, and a continuous s

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Supernova and Cosmic Rays, astronomy and high energy astrophysics, but the theoretical explanation of SN involves virtually every branch of physics. Supernovae, however, offer more than a challenging physics problem because SN are involved in the origin of most of the heavy elements, are the birthplaces of neutron stars, pul

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What Can We Learn about Cosmic Rays from the UV, Optical, Radio and X-ray Observations of Supernovaeration of high energy particles. So far only optical information about SNe has been available and from it there is no direct evidence of Cosmic Rays. It is not surprising then that models of Cosmic Ray production are still rich in free parameters. On April 19th 1979 a very bright (~12 mag) SN, labe

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