Primary Cosmic Radiation and Astrophysical Aspects

Grieder, P. K. F.

doi:10.1007/978-3-540-76941-5_11

Cited by 6 publications

(3 citation statements)

References 297 publications

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“…This primary interaction produces a jet of secondary particles which then results in successive interactions due to a chain reaction of particles. This phenomenon is called an extensive air shower (EAS) [5], and is schematically illustrated in Figure 1. The development of each air shower stops when the energy of the produced particle is too small to produce secondary particles.…”

Section: Physics Of Extensive Air Showersmentioning

confidence: 99%

High energy astroparticle physics for high school students

Krause¹,

Bretz²,

Classen³

et al. 2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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The questions about the origin and type of cosmic particles are not only fascinating for scientists in astrophysics, but also for young enthusiastic high school students. To familiarize them with research in astroparticle physics, the Pierre Auger Collaboration agreed to make 1% of its data publicly available. The Pierre Auger Observatory investigates cosmic rays at the highest energies and consists of more than 1600 water Cherenkov detectors, located near Malargüe, Argentina. With publicly available data from the experiment, students can perform their own hands-on analysis. In the framework of a so-called Astroparticle Masterclass organized alongside the context of the German outreach network Netzwerk Teilchenwelt, students get a valuable insight into cosmic ray physics and scientific research concepts. We present the project and experiences with students.

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Section: Physics Of Extensive Air Showersmentioning

confidence: 99%

High energy astroparticle physics for high school students

Krause¹,

Bretz²,

Classen³

et al. 2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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“…The origin of ultra-high energy cosmic rays (UHECRs) is a long-standing challenge for astrophysics. The energy spectrum of particles constituting cosmic rays (CRs) is measured up to and slightly above 10 20 eV (= 100 EeV) (Abbasi et al 2008;Salamida et al 2011;Egorova et al 2004), but no evidence has been revealed till now, either of the sources or the sort(s) of highest energy particles, owing mainly to the arrival direction distribution, which is nearly isotropic (Cronin 2005;Grieder 2010). However, some hints have been found recently of the possible correlation of UHECR arrival directions with nearby active galactic nuclei (AGN) at energies E > 56 EeV (PAO collaboration 2007).…”

Section: Introductionmentioning

confidence: 99%

A Method to Search for Correlations of Ultra-High Energy Cosmic-Ray Masses With the Large-Scale Structures in the Local Galaxy Density Field

Иванов

2013

ApJ

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One of the main goals of investigations using present and future giant extensive air shower (EAS) arrays is the mass composition of ultra-high energy cosmic rays (UHECRs). A new approach to the problem is presented, combining analysis of arrival directions with the statistical test of the paired EAS samples. An idea of the method is to search for possible correlations of UHECR masses with their separate sources, for instance, if there are two sources in different areas of the celestial sphere injecting different nuclei, but fluxes are comparable so that arrival directions are isotropic, the aim is to reveal a difference in the mass composition of CR fluxes. The method is based on a non-parametric statistical test -the Wilcoxon signed-rank routine -which does not depend on the populations fitting any parameterized distributions. Two particular algorithms are proposed: first, using measurements of the depth of EAS maximum position in the atmosphere; and second, relying on the age variance of air showers initiated by different primary particles. The formulated method is applied to the Yakutsk array data, in order to demonstrate the possibility of searching for a difference in average mass composition of the two UHECR sets, arriving particularly from the supergalactic plane and a complementary region.

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“…2.1), or as a sum of two exponentials according to the second method (as in Eq. 2.2) -in terms of the depth in the atmosphere, x = x 0 sec(θ ), g/cm 2 , in inclined showers [35,36,4]. Hence, two parameters in the formula are adjustable in order to fit the experimental data.…”

Section: Pos(icrc2017)550mentioning

confidence: 99%

Zenith angle distribution of cosmic ray showers measured with the Yakutsk array

Иванов¹

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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Primary Cosmic Radiation and Astrophysical Aspects

Cited by 6 publications

References 297 publications

High energy astroparticle physics for high school students

High energy astroparticle physics for high school students

A Method to Search for Correlations of Ultra-High Energy Cosmic-Ray Masses With the Large-Scale Structures in the Local Galaxy Density Field

Zenith angle distribution of cosmic ray showers measured with the Yakutsk array

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