Vasily Prosin, I. Astapov, P. Bezyazeekov, E. Bonvech, A. Borodin, A. Bulan, Andrea Chiavassa, D. Chernov, A. Dyachok, A. Gafarov, A. Garmash, V. Grebenyuk, O. Gress, E. Gress, T. Gress, A. Grinyuk, O. Grishin, A. D. Ivanova, Anna L. Ivanova, N. Kalmykov, V. V. Kindin, S. Kiryuhin, R. Kokoulin, K. Kompaniets, 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. Panov, A. A. Petrukhin, I. Poddubny, D. Podgrudkov, V. Poleschuk, V. Ponomareva, E. Popova, E. Postnikov, V. Ptuskin, A. Pushnin, R. Raikin, Alexander Razumov, G. Rubtsov, E. Ryabov, Y. Sagan, V. Samoliga, Alexander A. Silaev, Alexey A. Silaev, A. Sidorenkov, A. Skurikhin, A. Sokolov, L. Sveshnikova, V. Tabolenko, A. Tanaev, B. Tarashchansky, M. Ternovoy, L. Tkachev, R. Togoo, N. Ushakov, A. Vaidyanathan, P. Volchugov, N. Volkov, D. Voronin, A. Zagorodnikov, A. Zhaglova, D. Zhurov, I. I. Yashin
{"title":"Primary cosmic ray energy spectrum and mean mass composition using data from the TAIGA astrophysical complex","authors":"Vasily Prosin, I. Astapov, P. Bezyazeekov, E. Bonvech, A. Borodin, A. Bulan, Andrea Chiavassa, D. Chernov, A. Dyachok, A. Gafarov, A. Garmash, V. Grebenyuk, O. Gress, E. Gress, T. Gress, A. Grinyuk, O. Grishin, A. D. Ivanova, Anna L. Ivanova, N. Kalmykov, V. V. Kindin, S. Kiryuhin, R. Kokoulin, K. Kompaniets, 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. Panov, A. A. Petrukhin, I. Poddubny, D. Podgrudkov, V. Poleschuk, V. Ponomareva, E. Popova, E. Postnikov, V. Ptuskin, A. Pushnin, R. Raikin, Alexander Razumov, G. Rubtsov, E. Ryabov, Y. Sagan, V. Samoliga, Alexander A. Silaev, Alexey A. Silaev, A. Sidorenkov, A. Skurikhin, A. Sokolov, L. Sveshnikova, V. Tabolenko, A. Tanaev, B. Tarashchansky, M. Ternovoy, L. Tkachev, R. Togoo, N. Ushakov, A. Vaidyanathan, P. Volchugov, N. Volkov, D. Voronin, A. Zagorodnikov, A. Zhaglova, D. Zhurov, I. I. Yashin","doi":"10.21468/scipostphysproc.13.037","DOIUrl":null,"url":null,"abstract":"The corrected dependence of the mean depth of the EAS maximum X_{max} <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:msub><mml:mi>X</mml:mi><mml:mrow><mml:mi>m</mml:mi><mml:mi>a</mml:mi><mml:mi>x</mml:mi></mml:mrow></mml:msub></mml:math> on the energy was obtained from the data of the Tunka-133 array for 7 years and the TAIGA-HiSCORE array for 2 years. The parameter \\langle\\ln A\\rangle <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:mrow><mml:mo stretchy=\"false\" form=\"prefix\">⟩</mml:mo><mml:mo>ln</mml:mo><mml:mi>A</mml:mi><mml:mo stretchy=\"false\" form=\"postfix\">⟪</mml:mo></mml:mrow></mml:math> , 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} <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:mrow><mml:mn>2</mml:mn><mml:mo>⋅</mml:mo><mml:msup><mml:mn>10</mml:mn><mml:mn>14</mml:mn></mml:msup></mml:mrow></mml:math> – 2\\cdot 10^{16} <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:mrow><mml:mn>2</mml:mn><mml:mo>⋅</mml:mo><mml:msup><mml:mn>10</mml:mn><mml:mn>16</mml:mn></mml:msup></mml:mrow></mml:math> eV was reconstructed using the new parameter Q_{100} <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:msub><mml:mi>Q</mml:mi><mml:mn>100</mml:mn></mml:msub></mml:math> 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} <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:msub><mml:mi>Q</mml:mi><mml:mn>200</mml:mn></mml:msub></mml:math> to Q_{100} <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:msub><mml:mi>Q</mml:mi><mml:mn>100</mml:mn></mml:msub></mml:math> provides a decreasing energy threshold for the spectrum to about 200 TeV.","PeriodicalId":355998,"journal":{"name":"SciPost Physics Proceedings","volume":"40 1","pages":"0"},"PeriodicalIF":0.0000,"publicationDate":"2023-09-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"1","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"SciPost Physics Proceedings","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.21468/scipostphysproc.13.037","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
引用次数: 1
Abstract
The corrected dependence of the mean depth of the EAS maximum X_{max} Xmax on the energy was obtained from the data of the Tunka-133 array for 7 years and the TAIGA-HiSCORE array for 2 years. The parameter \langle\ln A\rangle ⟩lnA⟪ , 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⋅1014 – 2\cdot 10^{16} 2⋅1016 eV was reconstructed using the new parameter Q_{100} Q100 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} Q200 to Q_{100} Q100 provides a decreasing energy threshold for the spectrum to about 200 TeV.
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