Primary proton spectrum around the knee observed by the Tibet air-shower experiment

Amenomori, M.; Ayabe, S.; Chen, D.; Cui, S. W.; Danzengluobu,; Ding, L. K.; Ding, X. H.; Feng, C.; Feng, Z.; Gao, X. Y.; Geng, Q. X.; Guo, H. W.; He, H. H.; He, M.; Hibino, K.; Hotta, N.; Hu, Haibing; Hu, Hongbo; Huang, J.; Huang, Q.; Jia, H. Y.; Kajino, F.; Kasahara, K.; Katayose, Y.; Kato, C.; Kawata, K.; Labaciren,; Le, G. M.; Li, J. Y.; Lü, H.; Lu, S. L.; Meng, X. R.; Mizutani, K.; Mu, J.; Munakata, K.; Nagai, A.; Nanjo, H.; Nakamura, Masaki; Ohnishi, M.; Ohta, I.; Onuma, H.; Ouchi, T.; Ozawa, S.; Ren, J. R.; Saito, T.; Sakata, M.; Sasaki, Takashi; Shibata, M.; Shirai, T.; Sugimoto, H.; Takita, M.; Tan, Y. H.; Tateyama, N.; Torii, Shoji; Tsuchiya, H.; Udo, S.; Wang, H.; Wang, X.; Wang, Y. G.; Wu, H. R.; Xue, L.; Yamamoto, Y.; Yan, C. T.; Yang, X. C.; Yasue, S.; Ye, Z. H.; Yu, G. C.; Yuan, A. F.; Yuda, T.; Zhang, H. M.; Zhang, J. L.; Zhang, N. J.; Zhang, X. Y.; Zhang, Y.; Zhang, Yi; Zhaxisangzhu,; Zhou, X. X.

doi:10.1016/j.asr.2005.11.018

Cited by 9 publications

(4 citation statements)

References 18 publications

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“…compared to older measurements by Kascade). Nevertheless, our model matches reasonably the trend of the data, and in particular the peak around 100 PeV which is due, in our scenario, to the transition between the heaviest GCRs which are the only ones which WBCSN shocks can (Panov et al 2009;Adriani et al 2019;Yoon et al 2017;An et al 2019;Aartsen et al 2019;Antoni et al 2005;Apel et al 2013;Grebenyuk et al 2019;Amenomori et al 2006;Epimakhov et al 2013).…”

Section: Compositionsupporting

confidence: 87%

Massive star cluster origin for the galactic cosmic ray population at very-high energies

Vieu

Reville

2022

Monthly Notices of the Royal Astronomical Society

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We demonstrate that supernova remnant (SNR) shocks embedded within massive star clusters can reproduce both the cosmic-ray proton and all-particle spectra measured in the vicinity of the Earth up to hundreds of peta-electronvolts (PeV). We model two classes of massive star clusters. The first population are “loose clusters” which do not power a collective wind termination shock. SNR shocks then expand in a low-density and weakly magnetised medium, and this population mainly contributes up to the “knee” of the CR spectrum around 1 PeV. The second population are young compact clusters, which are powerful and compact enough to sustain a collective wind outflow. SNR shocks then expand from the cluster into the strongly magnetised wind and accelerate nuclei up to ultra-high energies. This population, representing only about 15% of all Galactic massive star clusters, nevertheless dominates the spectrum between ∼ 1 and 100 PeV. While these two components alone can reproduce the shape of the CR spectrum up to hundreds of PeV, adding a light sub-ankle extragalactic component motivated by composition and anisotropy measurements, allows to reproduce the spectrum up to the highest energies. Fitting parameters are systematically linked to physical variables whose values are in line with theoretical expectations.

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Section: Compositionsupporting

confidence: 87%

Massive star cluster origin for the galactic cosmic ray population at very-high energies

Vieu

Reville

2022

Monthly Notices of the Royal Astronomical Society

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“…This values can be deduced from the cut-off energy of the proton spectrum. Such data were obtained in the ASγ experiment (Tibet, 4300 m above sea level) [1] using the emulsion chambers and burst detectors which were accompanying with air shower array. It was obtained that the slope of the observed spectrum is steeper for primary energies E 0 > 10 14 eV than that extrapolated from the lower energy region, irrespective of the interaction models assumed in the simulation.…”

Section: Magnetic Rigidity Of the Knee Regionmentioning

confidence: 99%

“…The figure 1 at [1] shows the results obtained based on the simulation code CORSIKA with interaction models of QGSJET01 and SIBYLL 2.1.…”

Section: Magnetic Rigidity Of the Knee Regionmentioning

confidence: 99%

The composition of cosmic rays according to the data on EAS cores

Shaulov,

Ryabov,

Pyatovsky

et al. 2023

SciPost Phys. Proc.

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The main purpose of this work is to find the causes of the break of the cosmic ray spectrum at an energy of 3 PeV, which is called the knee. The solution of the problem is associated with the determination of the nuclear composition of cosmic rays in the knee area. The conclusions of this work are based on the analysis of the characteristics of the EAS cores obtained using X-ray emulsion chambers. According to these data, a number of anomalous effects are observed in the knee region, such as scaling violation in the spectra of secondary hadrons, an excess of muons in EAS with gamma families and others. At the same energies equivalent to 1-100 PeV the laboratory system colliders show scaling behavior. So analysis of the data on the EAS cores suggests that the knee in their spectrum is formed by a component of cosmic rays of a non-nuclear nature, possibly consisting of stable (quasi-stable) particles of hypothetical strange quark matter, which named strangelets. This is the only model of the knee compatible with the magnetic rigidity of the nuclear spectra break R=100 TV. In fact, stranglets are stable heavy quasi-nuclei with a positive electric charge of Z=30-1000, so the mechanism of their acceleration coincides with the nuclear one. The break of the cosmic ray spectrum can be associated with a significantly larger mass of strangelets compared to nuclei.

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“…But some contradictions in results of different experiments exist. Tibet ASγ array observed first knee (connected to protons) at about 200 TeV and supposed that hardening at 3 PeV is connected to elements heavier than Helium [3]. On the other hand, KASCADE group claimed the "knee" in primary spectrum is connected with proton acceleration cut-off.…”

Section: Introductionmentioning

confidence: 99%

Primary cosmic ray energy spectrum above 1 PeV as measured by the PRISMA-YBJ array

Stenkin¹,

Алексеенко²,

Shchegolev³

et al. 2018

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

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Primary cosmic ray energy spectrum above 1 PeV has been measured with PRISMA-YBJ being a prototype of PRISMA array at altitude of 4300 m a.s.l. It realized a novel type of EAS recording method measuring hadronic EAS component over the total array area through thermal neutron detection with a specially developed so-called en-detectors sensitive to electron and thermal neutron EAS components. Primary c. r. spectrum was recovered in 2 ways: through usual Ne procedure as well as through measurements of EAS size spectrum in thermal neutrons. Monte-Carlo simulations of the experiments allowed us recover the primary spectrum above 1 PeV. The both obtained spectra follow power law function with index close that measured by direct measurements below 1 PeV.

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Primary proton spectrum around the knee observed by the Tibet air-shower experiment

Cited by 9 publications

References 18 publications

Massive star cluster origin for the galactic cosmic ray population at very-high energies

Massive star cluster origin for the galactic cosmic ray population at very-high energies

The composition of cosmic rays according to the data on EAS cores

Primary cosmic ray energy spectrum above 1 PeV as measured by the PRISMA-YBJ array

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