Study of cosmic rays at the Yakutsk EAS array: energy spectrum and mass composition

Кнуренко, С. П.; Sabourov, A. V.

doi:10.1016/j.nuclphysbps.2011.03.033

Cited by 20 publications

(20 citation statements)

References 29 publications

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“…Other two faint features, a hardening slightly above 10 16 eV and a steepening around 10 17 eV, have been observed in the all particle spectrum. These features have been claimed by the KASCADE-Grande experiment [10] and then confirmed by the Ice Top [4], TUNKA-133 [1], Yakutsk [15] and TALE [2] experiments. The spectral shapes agree quite well, the differences in the corresponding energies are smaller than the systematic error due to the energy calibration.…”

Section: Resultssupporting

confidence: 55%

Summary of Cosmic Ray Spectrum and Composition Below 10¹⁸ eV

Чиавасса

2018

Proceedings of 2016 International Conference on Ultra-High Energy Cosmic Rays (UHECR2016)

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In this contribution I will review the main results recently obtained in the study of the cosmic ray spectrum and composition below 10 18 eV. The interest in this range is growing being related to the search of the knee of the iron component of cosmic ray and to the study of the transition between galactic and extra-galactic primaries. The all particle spectrum measured in this energy range is more structured than previously thought, showing some faint features: a hardening slightly above 10 16 eV and a steepening below 10 17 eV. The studies of the primary chemical composition are quickly evolving towards the measurements of the primary spectra of different mass groups: light and heavy primaries. A steepening of the heavy primary spectrum and a hardening of the light ones has been claimed. I will review these measurements and I will try to discuss the main sources of systematic errors still affecting them.

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Section: Resultssupporting

confidence: 55%

Summary of Cosmic Ray Spectrum and Composition Below 10¹⁸ eV

Чиавасса

2018

Proceedings of 2016 International Conference on Ultra-High Energy Cosmic Rays (UHECR2016)

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“…. Average logarithmic mass of cosmic ray derived from X max measurements from [75] with data from Tunka [76], Yakutsk [77,78], CASA-BLANCA [79], HiRes/MIA [80], HiRes [81], KASCADE-Grande [72], Auger [15] and TA [73] for hadronic interaction model EPOS v1.99 [57] compare with simulation predictions (red lines) as in Fig. 4.…”

Section: Resultsmentioning

confidence: 99%

Ultrahigh energy cosmic ray nuclei from extragalactic pulsars and the effect of their Galactic counterparts

Fang

Kotera

Olinto

2013

J. Cosmol. Astropart. Phys.

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Abstract. The acceleration of ultrahigh energy nuclei in fast spinning newborn pulsars can explain the observed spectrum of ultrahigh energy cosmic rays and the trend towards heavier nuclei for energies above 10 19 eV as reported by the Auger Observatory. Pulsar acceleration implies a hard injection spectrum (∼ E −1 ) due to pulsar spin down and a maximum energy E max ∼ Z 10 19 eV due to the limit on the spin rate of neutron stars. We have previously shown that the escape through the young supernova remnant softens the spectrum, decreases slightly the maximum energy, and generates secondary nuclei. Here we show that the distribution of pulsar birth periods and the effect of propagation in the interstellar and intergalactic media modifies the combined spectrum of all pulsars. By assuming a normal distribution of pulsar birth periods centered at 300 ms, we show that the contribution of extragalactic pulsar births to the ultrahigh energy cosmic ray spectrum naturally gives rise to a contribution to very high energy cosmic rays (VHECRs, between 10 16 and 10 18 eV) by Galactic pulsar births. The required injected composition to fit the observed spectrum depends on the absolute energy scale, which is uncertain, differing between Auger Observatory and Telescope Array. The contribution of Galactic pulsar births can also bridge the gap between predictions for cosmic ray acceleration in supernova remnants and the observed spectrum just below the ankle, depending on the composition of the cosmic rays that escape the supernova remnant and the diffusion behavior of VHECRs in the Galaxy.

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“…Through these measurements a lateral distribution of charged particles and muons with thr. ≥ 1 GeV [2,3] was studied and longitudinal development of air showers was reconstructed by measuring the lateral distribution of Cherenkov light emitted in EAS [4,5].…”

Section: Introductionmentioning

confidence: 99%

Fluctuations of the depth of maximum in extensive air showers and cross-section of p-air inelastic interaction for energy range 10¹⁵–10¹⁷eV

Кнуренко

Sabourov

2013

EPJ Web of Conferences

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Study of cosmic rays at the Yakutsk EAS array: energy spectrum and mass composition

Cited by 20 publications

References 29 publications

Summary of Cosmic Ray Spectrum and Composition Below 10¹⁸ eV

Summary of Cosmic Ray Spectrum and Composition Below 10¹⁸ eV

Ultrahigh energy cosmic ray nuclei from extragalactic pulsars and the effect of their Galactic counterparts

Fluctuations of the depth of maximum in extensive air showers and cross-section of p-air inelastic interaction for energy range 10¹⁵–10¹⁷eV

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Study of cosmic rays at the Yakutsk EAS array: energy spectrum and mass composition

Cited by 20 publications

References 29 publications

Summary of Cosmic Ray Spectrum and Composition Below 1018 eV

Summary of Cosmic Ray Spectrum and Composition Below 1018 eV

Ultrahigh energy cosmic ray nuclei from extragalactic pulsars and the effect of their Galactic counterparts

Fluctuations of the depth of maximum in extensive air showers and cross-section of p-air inelastic interaction for energy range 1015–1017eV

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Summary of Cosmic Ray Spectrum and Composition Below 10¹⁸ eV

Summary of Cosmic Ray Spectrum and Composition Below 10¹⁸ eV

Fluctuations of the depth of maximum in extensive air showers and cross-section of p-air inelastic interaction for energy range 10¹⁵–10¹⁷eV