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Primary cosmic ray energy spectrum and mean mass composition using data from the TAIGA astrophysical complex

V. ProsinSkobeltsyn Institute of Nuclear PhysicsИ. И. АстаповMoscow Engineering Physics InstituteP. BezyazeekovIrkutsk State UniversityE. BonvechIrkutsk State UniversityА. БородинJoint Institute for Nuclear ResearchА. БуланSkobeltsyn Institute of Nuclear PhysicsA. ChiavassaINFN Sezione di TorinoД. В. ЧерновSkobeltsyn Institute of Nuclear PhysicsA. DyachokIrkutsk State UniversityА. Р. ГафаровIrkutsk State UniversityA. GarmashBudker Institute of Nuclear PhysicsV. GrebenyukDubna UniversityО. ГрессIrkutsk State UniversityE. GressIrkutsk State UniversityТ. И. ГрессIrkutsk State UniversityA. A. GrinyukJoint Institute for Nuclear ResearchО. ГришинIrkutsk State UniversityA. D. IvanovaBudker Institute of Nuclear PhysicsAnna L. IvanovaBudker Institute of Nuclear PhysicsН. Н. КалмыковSkobeltsyn Institute of Nuclear PhysicsВ. В. КиндинMoscow Engineering Physics InstituteS. KiryuhinIrkutsk State UniversityР. П. КокоулинMoscow Engineering Physics InstituteК. Г. КомпаниецMoscow Engineering Physics InstituteE. KorostelevaSkobeltsyn Institute of Nuclear PhysicsВ. А. КожинSkobeltsyn Institute of Nuclear PhysicsЕ. А. КравченкоBudker Institute of Nuclear PhysicsA. P. KryukovSkobeltsyn Institute of Nuclear PhysicsL. KuzmichevSkobeltsyn Institute of Nuclear PhysicsА. А. ЛагутинAltai State UniversityM. V. LavrovaJoint Institute for Nuclear ResearchYu. LemeshevIrkutsk State UniversityB. LubsandorzhievInstitute for Nuclear ResearchN. LubsandorzhievSkobeltsyn Institute of Nuclear PhysicsA. LukanovInstitute for Nuclear ResearchD. LukyantsevIrkutsk State UniversityS. MalakhovIrkutsk State UniversityР. Р. МиргазовIrkutsk State UniversityР. МонхоевIrkutsk State UniversityE. OkunevaMoscow Engineering Physics InstituteЭ. А. ОсиповаSkobeltsyn Institute of Nuclear PhysicsА. ПахоруковIrkutsk State UniversityА. ПанJoint Institute for Nuclear ResearchL. A. PanasenkoNovosibirsk State UniversityL. PankovIrkutsk State UniversityА. Д. ПановSkobeltsyn Institute of Nuclear PhysicsА. А. ПетрухинMoscow Engineering Physics InstituteI. PoddubnyIrkutsk State UniversityD. PodgrudkovSkobeltsyn Institute of Nuclear PhysicsV. PoleschukIrkutsk State UniversityV. PonomarevaIrkutsk State UniversityE. PopovaSkobeltsyn Institute of Nuclear PhysicsE. PostnikovSkobeltsyn Institute of Nuclear PhysicsВ. С. ПтускинInstitute of Terrestrial Magnetism Ionosphere and Radio Wave PropagationА. ПушнинIrkutsk State UniversityР. И. РайкинAltai State UniversityAlexander RazumovSkobeltsyn Institute of Nuclear PhysicsГ. И. РубцовInstitute for Nuclear ResearchE. V. RyabovIrkutsk State UniversityY. SaganDubna UniversityВ. СамолигаIrkutsk State UniversityA. A. SilaevSkobeltsyn Institute of Nuclear PhysicsAlexey A. SilaevSkobeltsyn Institute of Nuclear PhysicsA. SidorenkovInstitute for Nuclear ResearchA. SkurikhinSkobeltsyn Institute of Nuclear PhysicsA. SokolovBudker Institute of Nuclear PhysicsL. SveshnikovaSkobeltsyn Institute of Nuclear PhysicsВ. А. ТаболенкоIrkutsk State UniversityА. ТанаевIrkutsk State UniversityB. TarashchanskyIrkutsk State UniversityM. TernovoyIrkutsk State UniversityЛ. ТкачевJoint Institute for Nuclear ResearchR. TogooMongolian Academy of SciencesNikita UshakovA. VaidyanathanNovosibirsk State UniversityП. А. ВолчуговSkobeltsyn Institute of Nuclear PhysicsН. В. ВолковAltai State UniversityД. ВоронинA. ZagorodnikovIrkutsk State UniversityA. ZhaglovaIrkutsk State UniversityД. ЖуровIrkutsk State UniversityI. I. YashinMoscow Engineering Physics Institute

SciPost Physics Proceedingsjournal2023en

ABI

Annotatsiya

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.

Mavzular

Astrophysics and Cosmic Phenomena Dark Matter and Cosmic Phenomena Neutrino Physics Research

Identifikatorlar

DOI: 10.21468/scipostphysproc.13.037

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