Spectrum and mass composition of cosmic rays in the energy range 10<sup>15</sup>–10<sup>18</sup>eV derived from the Yakutsk array data

Кнуренко, С. П.; Sabourov, A. V.

doi:10.1051/epjconf/20135304004

Cited by 8 publications

(6 citation statements)

References 7 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…With black squares on the same panel is shown energy spectrum obtained by the measurement of Cherenkov light emission at the YEASa -with both Main ChA and Small ChA (Yakutsk Cherenkov) [20]. Energy was estimated with the use of a similar quasi-calorimetric technique that utilizes a flux of Cherenkov photons at a certain core distance Q(r) as an energy estimator: E = (9.12 ± 2.28) × 10 On lower panels of Fig.…”

Section: Cosmic Ray Energy Spectrummentioning

confidence: 99%

See 1 more Smart Citation

Status of the Yakutsk air shower array and future plans

Alekseev,

Atlasov,

Bolotnikov

et al. 2021

Preprint

View full text Add to dashboard Cite

The Yakutsk Extensive Air Shower Array has been continuously operating for more than 50 years (since 1970) and up until recently it has been one of world's largest ground-based instruments aimed at studying the properties of cosmic rays in the ultra-high energy domain. In this report we discuss results recently obtained at the array -on cosmic rays energy spectrum, mass composition and directional anisotropy -and how they fit into the world data. Special attention is paid to the measurements of muonic component of extensive air showers. Theoretical results of particle acceleration at shocks are also briefly reviewed. Future scientific and engineering plans on the array modernization are discussed. I. INTRODUCTIONThe only way to study the properties of cosmic rays (CR) with energies above ∼ 10 15 eV is by registering extensive air showers (EAS) -cascades of secondary particles produced by high-energy CRs hitting Earth's atmosphere. On one hand by studying the EAS properties one can investigate hadron interactions at energies unreachable for terrestrial particle acceleration technology. On the other hand -EAS method provides the basis for obtaining crucial information on primary CR properties: their energy spectrum, mass composition and distribution of arrival directions on the celestial sphere. Hence, EAS study is a dedicated area of CR physics at the intersection of astrophysics and nuclear physics.

show abstract

Section: Cosmic Ray Energy Spectrummentioning

confidence: 99%

“…2(c) is shown a comparison of ln A estimations obtained with two methods described above. Black circles denote results obtained with Main ChA [21]; with black triangles -results obtained with Small ChA [20];…”

Section: Cosmic Ray Mass Compositionmentioning

confidence: 99%

Status of the Yakutsk air shower array and future plans

Alekseev,

Atlasov,

Bolotnikov

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

“…Since in a first approximation a shower produced by a nucleus of energy E and mass number A can be considered as the superposition of A showers of energy E/A (which being less energetic are also less penetrating), the average values of X max at a given energy provide an indication of the average CR mass composition. We use measurements of X max obtained with telescopes in different experiments, in particular those of Yakutsk [22,23] and Tunka-133 [8,9] or Auger [24]. We normalize the relative abundances at PeV energies with representative values comparable to those determined by direct measurements at ∼ 10 TeV and, through a global fit, we determine the spectral features of the different Galactic components as well as the properties of the transition towards a dominant extragalactic component.…”

Section: Jcap03(2019)017mentioning

confidence: 99%

“…The fluxes are multiplied by E 3 in order to make them flatter. Right panel: average X max vs. E measured by Yakutsk [22,23], Tunka-133 [8,9] and Auger [24]. Also shown are the predictions from simulations based on the hadronic models Sibyll 2.3, EPOS-LHC and QGSJet II-04 for pure H and Fe compositions.…”

Section: Jcap03(2019)017mentioning

confidence: 99%

A scenario for the Galactic cosmic rays between the knee and the second-knee

Mollerach¹,

Roulet

2019

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

We perform a fit to measurements of the cosmic ray spectrum in the energy range between 10 15 eV and 10 18 eV using data from the TALE, Tunka and Auger experiments. We also fit the data on the depth of shower maximum, Xmax, from Tunka and Yakutsk or from Auger to constrain the cosmic ray composition. We consider a Galactic component that is a mixture of five representative nuclear species (H, He, N, Si and Fe), for which we adopt rigidity dependent broken power-law spectra, and we allow for an extragalactic component which becomes strongly suppressed for decreasing energies. The relative abundances of the Galactic components at 10 15 eV are taken to be comparable to those determined by direct measurements at 10 13 eV. The main features of the spectrum and of the composition are reproduced in these scenarios. The spectral knee results from the break of the H spectrum at E k ≃ 3 × 10 15 eV, although it is broadened by the comparable contribution from He which has a break at about 6×10 15 eV. The low-energy ankle at E la ≃ 2×10 16 eV coincides with the strong suppression of the H and He Galactic components and the increasing relative contribution of the heavier ones, but the observed hardening of the spectrum at this energy turns out to result from the growing contribution of the extragalactic component. The second-knee at E sk ≃ 26E k ≃ 8 × 10 16 eV is associated with the steepening of the Galactic Fe component. The transition to the regime in which the total cosmic ray flux is dominated by the extragalactic component takes place at an energy of about 10 17 eV. The parameters of the fit depend on the specific Xmax dataset that is considered, with the Yakutsk and Tunka data leading to a suppression of the light components being steeper beyond the knee so as to allow a faster growth of the average mass around the low-energy ankle. The results also depend on the hadronic model that is used to interpret Xmax measurements and we compare the parameters obtained with Sibyll 2.3, EPOS-LHC and QGSJET II-04. The impact of the possible existence of a maximum rigidity cutoff in the Galactic components is also discussed.

show abstract

“…4 with dark circles. Light circles represent spectrum from [26] obtained from measurements of Cherenkov light emission. Other symbols represent the data from Akeno (1984,1992) [27,28], AGASA [29], Tunka-133 [30], IceTop [31], HiRes I [6], HiRes II [32], Telescope Array (TA) [7] and from The Pierre Auger Observatory (PAO) [8].…”

Section: Primary Energy Spectrummentioning

confidence: 99%

Energy spectrum of ultra-high energy cosmic rays according to surface detectors of Yakutsk EAS array

Sabourov¹,

Glushkov²,

Pravdin³

et al. 2017

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

View full text Add to dashboard Cite

Spectrum and mass composition of cosmic rays in the energy range 10¹⁵–10¹⁸eV derived from the Yakutsk array data

Cited by 8 publications

References 7 publications

Status of the Yakutsk air shower array and future plans

Status of the Yakutsk air shower array and future plans

A scenario for the Galactic cosmic rays between the knee and the second-knee

Energy spectrum of ultra-high energy cosmic rays according to surface detectors of Yakutsk EAS array

Contact Info

Product

Resources

About

Spectrum and mass composition of cosmic rays in the energy range 1015–1018eV derived from the Yakutsk array data

Cited by 8 publications

References 7 publications

Status of the Yakutsk air shower array and future plans

Status of the Yakutsk air shower array and future plans

A scenario for the Galactic cosmic rays between the knee and the second-knee

Energy spectrum of ultra-high energy cosmic rays according to surface detectors of Yakutsk EAS array

Contact Info

Product

Resources

About

Spectrum and mass composition of cosmic rays in the energy range 10¹⁵–10¹⁸eV derived from the Yakutsk array data