First Estimate of the Primary Cosmic Ray Energy Spectrum above 3 EeV from the Pierre Auger Observatory

Collaboration, The Pierre Auger

doi:10.48550/arxiv.astro-ph/0507150

Cited by 1 publication

(4 citation statements)

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“…17. Spectra of modification factor for the f (R) gravity Starobinsky model along with that for the ΛCDM model with γg = 2.7, which are in comparison with different experimental data such as AKENO-AGASA [52,53], HiRes [54], YAKUTSK [57] and AUGER [55] experiments.…”

Section: B Projections Of Starobinsky F (R) Gravity Modelmentioning

confidence: 69%

“…20. Calculated E 3 magnified spectra of UHECR protons for the ΛCDM model (black dotted line), the f (R) gravity power-law model (blue line) and the Starobinsky model (red line) in comparison with the AKENO-AGASA [52,53], HiRes [54] and AUGER [56] detectors' data (left panel), and the modification factors of the same in comparison with the AKENO-AGASA [52,53], HiRes [54], AUGER [55] and YAKUTSK [57] detectors' data.…”

Section: Discussionmentioning

confidence: 99%

“…11. Spectra of modification factor with γg = 2.7 in comparison with different experimental data such as AKENO-AGASA [52,53], HiRes [54], YAKUTSK [57] and AUGER [55] for the ΛCDM and f (R) gravity power-law model. data for the bump in the spectrum is seen.…”

Section: A Projections Of F (R) Power-law Modelmentioning

confidence: 95%

“…In section V, we calculate the number density of particles and hence the enhancement factor. Here the differential flux and modification factor for the both two models are calculated and are compared the results with AKENO-AGASA [52,53], HiRes [54], AUGER [55,56] and YAKUTSK [57] arrays data. Finally, we compare the results for the ΛCDM, power-law and Starobinsky models and then conclude our paper with a fruitful discussion in section VI.…”

Section: Introductionmentioning

confidence: 99%

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Even though the sources of the ultra high energy cosmic rays (UHECRs) are yet to be known clearly, the high-quality data collected by the most recent CRs observatories signal that the sources of these CRs should be of the extragalactic origin. As the intergalactic mediums are thought to be filled with the turbulent magnetic fields (TMFs), these intergalactic magnetic fields may have a significant impact on how UHECRs travel across the Universe, which is currently expanding with acceleration. Thus the inclusion of these points in the theory is crucial for understanding the experimental findings on UHECRs. Accordingly, in this work we study the effect of diffusion of UHE particles in presence of TMFs in the light of f (R) theory of gravity. The f (R) theory of gravity is a successful modified theory of gravity in explaining the various aspects of the observable Universe including its current state of expansion. For this work we consider two most studied f (R) gravity models, viz., the power-law model and the Starobinsky model. With these two models we study the diffusive character of propagation of UHECR protons in terms of their density enhancement. The Greisen-Zatsepin-Kuzmin (GZK) cutoff, the dip and the bump are all spectrum characteristics that UHE extragalactic protons acquire when they propagate through the cosmic microwave background (CMB) radiation in presence of TMFs. We analyse all these characteristics through the diffusive flux as well as its modification factor. Model dependence of the modification factor is minimal compared to the diffusive flux. We compare the UHECR protons spectra that are calculated for the considered f (R) gravity models with the available data of the AKENO-AGASA, HiRes, AUGER and YAKUTSK experiments of UHECRs. We see that both the models of f (R) gravity provide the energy spectra of UHECRs with all experimentally observed features, which lay well within the range of combine data of all experiments throughout the energy range of concern, in contrast to the case of the ΛCDM model.

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