UHE nuclei propagation and the interpretation of the ankle  in the cosmic-ray spectrum

Allard, Denis; Parizot, E.; Khan, E.; Goriely, Stéphane; Olinto, Angela V.

doi:10.1051/0004-6361:200500199

Cited by 166 publications

(269 citation statements)

References 22 publications

(31 reference statements)

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“…In fact, recent analyses [27,70] show that the X max data, as well as the data on the energy spectrum from both HiRes [71] and the Pierre Auger Observatory [72], can simultaneously be reproduced if the extra-galactic cosmic rays contain a substantial fraction of heavy nuclei, and the Galactic/extra-galactic transition occurs, as was believed originally, at the "ankle" in the spectrum.…”

Section: Figmentioning

confidence: 99%

High energy neutrinos from astrophysical accelerators of cosmic ray nuclei

Anchordoqui

Hooper

Sarkar

et al. 2008

Astroparticle Physics

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Ongoing experimental efforts to detect cosmic sources of high energy neutrinos are guided by the expectation that astrophysical accelerators of cosmic ray protons would also generate neutrinos through interactions with ambient matter and/or photons. However there will be a reduction in the predicted neutrino flux if cosmic ray sources accelerate not only protons but also significant numbers of heavier nuclei, as is indicated by recent air shower data. We consider plausible extragalactic sources such as active galactic nuclei, gamma-ray bursts and starburst galaxies and demand consistency with the observed cosmic ray composition and energy spectrum at Earth after allowing for propagation through intergalactic radiation fields. This allows us to calculate the expected neutrino fluxes from the sources, normalized to the observed cosmic ray spectrum. We find that the likely signals are still within reach of next generation neutrino telescopes such as IceCube.PACS numbers: 95.85. Ry, 98.70.Rz, 98.54.Cm, 98.54.Ep

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Section: Figmentioning

confidence: 99%

High energy neutrinos from astrophysical accelerators of cosmic ray nuclei

Anchordoqui

Hooper

Sarkar

et al. 2008

Astroparticle Physics

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“…As the energy losses of complex nuclei and their energy evolution are different from the proton case, one does not expect such a feature in their propagated spectra. One can show that the possibility of observing a pair production dip in the extragalactic cosmic-ray spectrum requires the abundance of complex nuclei at the source to be less than 10-20% (depending on the mixture of complex nuclei assumed) [57,41,64].…”

Section: Mixed and Nuclei Dominated Compositionsmentioning

confidence: 99%

“…[41] proposed to study the case of a mixed composition equivalent to that of low energy galactic cosmic-rays as a possible composition (see also [66] for more details). Even though there is no strong reason for the composition at the extragalactic source to be exactly the same as that of low energy galactic cosmic-rays (which moreover is not known extremely precisely, as it has to be reconstructed from the observations [65]), the hierarchy of the relative abundances between the different elements could be somewhat preserved.…”

Section: Mixed and Nuclei Dominated Compositionsmentioning

confidence: 99%

Extragalactic propagation of ultrahigh energy cosmic-rays

Allard

2012

Astroparticle Physics

122

136

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In this paper we review the extragalactic propagation of ultrahigh energy cosmic-rays (UHECR). We present the different energy loss processes of protons and nuclei, and their expected influence on energy evolution of the UHECR spectrum and composition. We discuss the possible implications of the recent composition analyses provided by the Pierre Auger Observatory. The influence of extragalactic magnetic fields and possible departures from the rectilinear case are also mentioned as well as the production of secondary cosmogenic neutrinos and photons and the constraints their observation would imply for the UHECRs origin. Finally, we conclude by briefly discussing the relevance of a multi messenger approach for solving the mystery of UHECRs.

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“…This is because of the GZK cutoff [15,16]: higher energy protons would interact with photons of the cosmic microwave background and loose energy. For heavier nuclei there exist similar, but slightly different cutoffs, e.g., due to photo dissociation [17].…”

Section: Origin Of Cosmic Raysmentioning

confidence: 98%

Instruments and Methods for the Radio Detection of High Energy Cosmic Rays

Schröder¹

2012

Springer Theses

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Instruments and Methods for the Radio Detection of High Energy Cosmic RaysCosmic rays at energies above 10 15 eV cannot be measured directly due to the low flux. Instead, the properties of the primary cosmic ray particles (arrival direction, energy, mass) have to be reconstructed from measurements of secondary particles forming an air shower. For this, digital radio antenna arrays, like LOPES at the Karlsruhe Institute of Technology (KIT), are a relatively new instrument. The radio emission mainly originates from the deflection of secondary air shower electrons and positrons in the Earth's magnetic field. The radio technique aims at achieving a similar quality in the reconstruction of air shower parameters as the established Cherenkov or fluorescence light detection methods, which in contrast to the radio technique are limited to dark, moonless nights.The present studies aim to advance the air shower radio detection in technological aspects and analysis methods. The developments are mainly applied to LOPES, but also provide a useful set of tools, which will soon be applied on the analysis of first AERA measurements. AERA is a next generation digital radio array at the Pierre Auger Observatory in Argentina. Moreover, this thesis reflects the recent progress in the understanding of the radio emission by air showers. The main results of the studies are:• A new method for time calibration with a reference beacon has been developed.It allows a time resolution of ∼ 1 ns even with large antenna arrays. This is necessary for digital radio interferometry which improves the signal-to-noise ratio and the reconstruction accuracy of the primary particle properties. This method is essential for the measurement of cosmic rays with LOPES, and is going to be applied at AERA.• A per-event comparison of lateral distributions measured with LOPES and REAS3 simulations reflects a significantly improved understanding of the radio emission mechanisms. For the first time a Monte Carlo simulation of the radio emission by air showers can in average reproduce measured data. A detailed investigation of systematic effects was performed to accurately reconstruct LOPES lateral distributions. In particular, a method has been developed to appropriately treat the influence of radio noise on measured lateral distributions.• It is shown that a conical radio wavefront fits LOPES measurements and REAS3 simulations better than a spherical wavefront, which up to now has been assumed for LOPES beamforming analyses. Furthermore, the atmospheric depth of the shower maximum X max can be reconstructed by determining the opening angle of the conical wavefront. However, due to the small lateral extension of LOPES of about 200 m and the high radio background at KIT, the measurement uncertainty (∆X max ≈ 200 g/cm 2 ) is too large for a per-event reconstruction of the primary mass. This will improve at AERA, but could not be examined in detail because of a delay in the construction. • Eine neue Methode zur Zeitkalibration mit einen Rerefenzsender (Beaco...

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UHE nuclei propagation and the interpretation of the ankle in the cosmic-ray spectrum

Cited by 166 publications

References 22 publications

High energy neutrinos from astrophysical accelerators of cosmic ray nuclei

High energy neutrinos from astrophysical accelerators of cosmic ray nuclei

Extragalactic propagation of ultrahigh energy cosmic-rays

Instruments and Methods for the Radio Detection of High Energy Cosmic Rays

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