By Maurice M. Shapiro, Todor Stanev, John P. Wefel
This quantity includes the Lectures and chosen player contributions to the 14th process the overseas institution of Cosmic Rays Astrophysics, a NATO complicated examine Institute. popular astrophysicists and astronomers speak about varied elements of the new release of excessive power signs in robust astrophysical gadgets targeting the construction of neutrinos and gamma rays from excessive strength particle interactions. fresh effects from new experiments and observatories are awarded. themes hide a variety together with the Spitzer infrared observatory, TeV gamma ray observations, darkish topic, and neutrino telescopes. the mix of easy wisdom concerning the construction of excessive power signs with information regarding the information research of ongoing observations locations the booklet among the standard degrees of a textbook and a convention complaints. it is going to provide the reader a great advent to the present box of astroparticle physics, and a few of the attention-grabbing astrophysics being addressed.
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2004 and Bergman, 2004. Because of the uncertainties in the interaction models above accelerator energies coupled with statistical and systematic limitations of the experiments, the primary composition as a function of energy above 1017 eV remains an open question (Watson, 2004). 5 20 Figure 8. Plot of data on mean depth of maximum vs energy. , 1993). , 2001). This figure also appears in Ref. (Gaisser & Stanev, 2005). Highest energy cosmic rays Protons lose energy by three loss processes during propagation through the cosmos.
2004) is consistent with the GZK shape. The discrepancy between the two experiments is not as great as it appears in Fig. 9. The difference is amplified quadratically when the differential spectrum is multiplied by E 3 in the plot. A 20-30% shift in energy assignment (downward for AGASA or upward for HiRes) brings the two data sets into agreement below 5 × 1019 eV. A quantitative estimate of the statistical significance of the difference above 5 × 1019 eV is ambiguous because it depends on what is assumed for the true spectrum.
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