SciPost Submission Page
Primary Cosmic Ray Energy Spectrum and Mean Mass Composition Using Data from the TAIGA Astrophysical Complex
by V. Prosin, I. Astapov, P. Bezyazeekov, E. Bonvech, A. Borodin, A. Bulan, A. Chiavassa, D. Chernov, A. Dyachok, A. Gafarov, A. Garmash, V. Grebenyuk, O. Gress, E. Gress, T. Gress, A. Grinyuk, O. Grishin, A. D. Ivanova, A. L. Ivanova, N. Kalmykov, V. Kindin, S. Kiryuhin, R. Kokoulin, K. Komponiets, E. Korosteleva, V. Kozhin, E. Kravchenko, A. Kryukov, L. Kuzmichev, A. Lagutin, M. Lavrova, Y. Lemeshev, B. Lubsandorzhiev, N. Lubsandorzhiev, A. Lukanov, D. Lukyantsev, S. Malakhov, R. Mirgazov, R. Monkhoev, E. Okuneva, E. Osipova, A. Pakhorukov, A. Pan, L. Panasenko, L. Pankov, A. D. Panov, A. Petrukhin, I. Poddubny, D. Podgrudkov, V. Poleschuk, V. Ponomareva, E. Popova, E. Postnikov, V. Ptuskin, A. Pushnin, R. Raikin, A. Razumov, G. Rubtsov, E. Ryabov, Y. Sagan, V. Samoliga, A. Silaev, A. Silaev Jr, A. Sidorenkov, A. Skurikhin, A. Sokolov, L. Sveshnikova, V. Tabolenko, A. Tanaev, B. Tarashchansky, M. Y. Ternovoy, L. Tkachev, R. Togoo, N. Ushakov, A. Vaidyanathan, P. Volchugov, N. Volkov, D. Voronin, A. Zagorodnikov, A. Zhaglova, D. Zhurov, I. Yashin
This is not the latest submitted version.
This Submission thread is now published as
Submission summary
| Authors (as registered SciPost users): | Anna Ivanova · Vasily Prosin |
| Submission information | |
|---|---|
| Preprint Link: | https://arxiv.org/abs/2208.01689v2 (pdf) |
| Date submitted: | 2022-12-20 18:05 |
| Submitted by: | Prosin, Vasily |
| Submitted to: | SciPost Physics Proceedings |
| Proceedings issue: | 21st International Symposium on Very High Energy Cosmic Ray Interactions (ISVHECRI2022) |
| Ontological classification | |
|---|---|
| Academic field: | Physics |
| Specialties: |
|
Abstract
The corrected dependence of the mean depth of the EAS maximum $X_{max}$ on the energy was obtained from the data of the Tunka-133 array for 7 years and the TAIGA-HiSCORE array for 2 year. The parameter $\langle\ln A\rangle$, characterizing the mean mass compositon was derived from these results. The differential energy spectrum of primary cosmic rays in the energy range of $2\cdot 10^{14}$ – $2\cdot 10^{16}$\,eV was reconstructed using the new parameter $Q_{100}$ the Cherenkov light flux at the core distance 100 m. Change of the parameter for the energy reconstuction for the TAIGA-HiSCORE from $Q_{200}$ to $Q_{100}$ provides a decreasing energy threshold for the spectrum to about 200 TeV.
List of changes
1. Title: Primary Cosmic Ray Energy Spectrum and Mean Mass Composition Using Data from the TAIGA Astrophysical Complex
2. Abstract: +Change of the parameter for the energy reconstuction for the TAIGA-HiSCORE from Q200 to Q100 provides a decreasing energy threshold for the spectrum to about 200 TeV.
3. Introduction: +The main aim of the present work is to achieve the lower energy threshold by the new method of energy reconstruction, descibed below.
4. Section 3: ...One has to control that there are the measurements of light flux at core distances Rc ≥ 200m and Rc ≥ 80m. The first of these conditions is applied to the events for the primary energy E0 ≥ 1016 eV for Tunka-133 and E0 ≥ 1015 eV for the TAIGA-HiSCORE. CORSIKA simulation [5] confirmed that the Cherenkov light LDF steepness is determined solely by the thickness of the atmosphere between the array and the depth of the EAS maximum (Xmax = X0/secθ −Xmax).
5. Section 5: ...One has to control that there are the measurements of light flux at core distances Rc ≥ 200m and Rc ≥ 80m. The first of these conditions is applied to the events for the primary energy E0 ≥ 1016 eV for Tunka-133 and E0 ≥ 1015 eV for the TAIGA-HiSCORE. CORSIKA simulation [5] confirmed that the Cherenkov light LDF steepness is determined solely by the thickness of the atmosphere between the array and the depth of the EAS maximum (Xmax = X0/secθ −Xmax).
6. Conclusions: The new estimations of Xmax , derived from the steepness parameter P = Q(80)/Q(200) provides good agreement between both the results of our arrays Tunka-133, TAIGA-HiSCORE and Tunka-133 and the direct measurements of Xmax at the Pierre Auger Observatory (PAO).
The primary composition, derived from Xmax is lighter than it seemed in our previous publications. It is mostly light (p+He) over the whole energy range. The observed increase of 〈lnA〉 in the energy range 1016 - 1017 eV demands a new theoretical explanation.
Change of the parameter for the energy reconstruction for the TAIGA-HiSCORE from Q200to Q100 provides a decreasing energy threshold for the spectrum to about 200 TeV.
The all particle energy spectrum over the energy range 200 TeV - 3 PeV follows a pure
power law with index 2.71±0.01.