Identification of gamma ultra high energy cosmic rays by simulating extensive air showers

Geranios, A; Fokitis, E; Maltezos, S; Mastichiadis, A; Malandraki, OE; Antoniadou, I

dc.contributor.author	Geranios, A	en
dc.contributor.author	Fokitis, E	en
dc.contributor.author	Maltezos, S	en
dc.contributor.author	Mastichiadis, A	en
dc.contributor.author	Malandraki, OE	en
dc.contributor.author	Antoniadou, I	en
dc.date.accessioned	2014-03-01T02:50:24Z
dc.date.available	2014-03-01T02:50:24Z
dc.date.issued	2006	en
dc.identifier.issn	0094243X	en
dc.identifier.uri	https://dspace.lib.ntua.gr/xmlui/handle/123456789/35110
dc.title	Identification of gamma ultra high energy cosmic rays by simulating extensive air showers	en
heal.type	conferenceItem	en
heal.identifier.primary	10.1063/1.2348033	en
heal.identifier.secondary	http://dx.doi.org/10.1063/1.2348033	en
heal.publicationDate	2006	en
heal.abstract	Among the most interesting tasks for the identification of Ultra High Energy Cosmic Rays (origin, mechanisms of acceleration, top down model, direction, and maximum energy) is their isotopic composition. For example, if they are protons, heavier nuclei, gammas or even exotic. Air Shower Extended Simulation code (AIRES) is used to simulate the Extended Atmospheric Showers. This code gives, among others, the maximum number of secondary particles within the atmosphere along the longitudinal direction of the showers. From the distribution of the depths of maximum number of shower particles and their content in muons, we can distinguish between proton and gamma primary cosmic rays, both of energy of 100 EeV. The results show a maximum at lower atmospheric depths for protons and at higher for gammas, respectively. Due to the bremsstrahlung and pair production effects, the muon content of gamma showers is much poorer than of protons. Both facts enable the distinction between proton and gamma cosmic rays. For the simulation of the atmospheric EAS due to the passage of an Ultra High Energy Cosmic Ray, the Linsley standard atmospheric model is used. © 2006 American Institute of Physics.	en
heal.journalName	AIP Conference Proceedings	en
dc.identifier.doi	10.1063/1.2348033	en
dc.identifier.volume	848	en
dc.identifier.spage	580	en
dc.identifier.epage	586	en