Astroparticle Physics最新文献

Through the heliospheric lens: Directional deflection of high-energy cosmic-ray electrons and positrons 通过日光层透镜：高能宇宙射线电子和正电子的定向偏转

IF 2.9 3区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Astroparticle Physics

Pub Date : 2025-12-13 DOI: 10.1016/j.astropartphys.2025.103202

Stefano Profumo , Aria Koul , Anika Malladi , Benjamin Schmitt

We investigate how the large-scale heliosphere alters the arrival directions of high-energy cosmic-ray electrons and positrons and ask if and when this “heliospheric lens” can be ignored for anisotropy and source — association studies — an especially timely topic given, for instance, the persistent cosmic-ray positron fraction and its unknown origin. Using a modular back-tracing framework, we explore a set of widely used magnetic-field descriptions—from a Parker spiral baseline to more structured configurations that include latitudinal wind contrasts, Smith–Bieber–type azimuthal strengthening, and tilted or wavy heliospheric current sheets. We model the deterministic deflections of high-energy cosmic-ray electrons and positrons (CREs) induced by large-scale heliospheric magnetic-field structures using a back-tracing approach. Our results apply to CREs above tens of GeV, where diffusion, convection, and adiabatic energy losses play a subdominant role; these processes are neglected in the present study and will be addressed in future work. Across these models the picture is consistent: most bending is accumulated within the inner tens of astronomical units and decreases rapidly with energy. Field choices and solar-cycle geometry set the overall normalization, with stronger spiral winding or a more highly tilted current sheet producing larger deflections at the same energy. Differences between electrons and positrons are most apparent at lower energies, where drift histories and current-sheet encounters diverge, and become increasingly small at multi-TeV energies. We summarize these trends with a practical threshold energy describing when heliospheric bending falls below an instrument’s angular resolution, and we verify that our conclusions are robust to numerical settings. For current instruments, heliospheric effects can usually be treated as a small correction at the highest energies, while sub-TeV analyses benefit from a calibrated envelope that accounts for plausible field configurations during the observing epoch.

我们研究了大规模的日球层如何改变高能宇宙射线电子和正电子的到达方向，并询问是否以及何时可以在各向异性和源关联研究中忽略这个“日球层透镜”-一个特别及时的主题，例如，持久的宇宙射线正电子分数及其未知的来源。使用模块化的反向追踪框架，我们探索了一组广泛使用的磁场描述-从帕克螺旋基线到更结构化的配置，包括纬向风对比，史密斯-比伯型方位增强，以及倾斜或波浪状的日球层电流片。我们用回溯法模拟了由大尺度日球磁场结构引起的高能宇宙射线电子和正电子（cre）的确定性偏转。我们的结果适用于数十GeV以上的CREs，其中扩散、对流和绝热能量损失占次要地位；这些过程在本研究中被忽略，将在今后的工作中加以解决。在这些模型中，情况是一致的：大多数弯曲是在内部几十个天文单位内积累的，并随着能量的增加而迅速减少。现场选择和太阳周期几何形状设定了整体的标准化，在相同的能量下，更强的螺旋绕组或更大的倾斜电流片产生更大的偏转。电子和正电子之间的差异在较低的能量下最为明显，在较低的能量下，漂移历史和电流片相遇是发散的，并且在多tev的能量下变得越来越小。我们用一个实际的阈值能量来描述当日球弯曲低于仪器的角度分辨率时，我们总结了这些趋势，并验证了我们的结论对数值设置是稳健的。对于目前的仪器，日球层效应通常可以被视为最高能量下的小修正，而亚tev分析则受益于校准的包络线，该包络线解释了观测时期可能的场结构。

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引用次数: 0

The mass of cosmic rays of ultra-high energy 超高能量宇宙射线的质量

IF 2.9 3区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Astroparticle Physics

Pub Date : 2025-11-29 DOI: 10.1016/j.astropartphys.2025.103200

A A Watson

A review of several analyses is presented that forces the conclusion that the mass composition of the highest-energy cosmic rays is not proton-dominated. This deduction, combined with the use of a modern hadronic interaction model, should lead to a re-evaluation of the energy spectrum reported by the Telescope Collaboration that may well bring that measurement, and the corresponding one from the Pierre Auger Observatory, into better agreement.

对几个分析的回顾提出了一个结论，即最高能量宇宙射线的质量组成不是质子主导的。这一推断，结合现代强子相互作用模型的使用，应该会导致望远镜合作组织报告的能谱的重新评估，这很可能会使测量结果与皮埃尔·奥格天文台的相应测量结果更加一致。

引用次数: 0

Investigation of a muon burst coincident with KM3-230213A 与KM3-230213A重合的μ子爆发的研究

IF 2.9 3区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Astroparticle Physics

Pub Date : 2025-11-28 DOI: 10.1016/j.astropartphys.2025.103201

Francesco Nozzoli

On February 13, 2023, the KM3NeT/ARCA neutrino telescope detected the high-energy neutrino candidate KM3-230213A, characterized by a

\sim

120 PeV through-going muon with a nearly horizontal trajectory. Independently, the Yangbajing muon telescope in Tibet recorded a burst of events starting at the same UTC time, showing a

5.7 σ

excess in a direction compatible with KM3-230213A. The burst exhibits a statistically significant exponential time structure with a decay constant

τ = 7.0 \pm 1.5

min and a peak flux of

55 \pm 10

Hz/m

^{2}

, resulting in

2300 \pm 400

excess events over 30 min. The analysis of the time series of the event rate recorded by the Yangbajing telescope shows that the probability of a chance coincidence of this muon burst with the KM3-230213A event is less than

1 0^{- 3}

. The agreement between the muon burst and the KM3-230213A event in both timing and direction, together with the non-detection by IceCube and the Pierre Auger Observatory, supports the hypothesis of a rapidly flaring source and highlights the relevance of combining surface muon data with neutrino telescope observations.

2023年2月13日，KM3NeT/ARCA中微子望远镜探测到高能中微子候选粒子KM3-230213A，其特征是具有接近水平轨迹的~ 120 PeV穿过μ子。在与KM3-230213A相匹配的方向上有7σ过剩。该脉冲具有统计学上显著的指数时间结构，衰减常数τ=7.0±1.5 min，峰值通量为55±10 Hz/m2，在30 min内产生2300±400个过剩事件。对羊八井望远镜记录的事件速率时间序列的分析表明，此次μ子爆发与KM3-230213A事件的偶合概率小于10−3。这次μ子爆发与KM3-230213A事件在时间和方向上的一致，以及冰立方和皮埃尔·奥格天文台的未探测到，支持了一个快速燃烧源的假设，并强调了将表面μ子数据与中微子望远镜观测相结合的相关性。

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引用次数: 0

Gamma rays as leptonic portals to energetic neutrinos: A new Monte Carlo approach 伽马射线作为高能中微子的轻子入口：一种新的蒙特卡罗方法

IF 2.9 3区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Astroparticle Physics

Pub Date : 2025-11-22 DOI: 10.1016/j.astropartphys.2025.103192

Gaetano Di Marco , Rafael Alves Batista , Miguel A. Sánchez-Conde

High center-of-mass electromagnetic (EM) interactions could produce decaying heavy leptons and hadrons, leading to neutrino generation. These processes might occur in the most extreme astrophysical scenarios, potentially altering the expected gamma-ray and neutrino fluxes in both the hadronic and the leptonic pictures. For instance, neutrinos could arise from high-redshift EM cascades, triggered by gamma rays beyond

1 0^{18} eV

scattering background photons, from radio to ultraviolet energy bands. Such energetic gamma rays are predicted in cosmogenic models and in scenarios involving non-standard physics. On astrophysical scales, leptonic production of neutrinos could take place in active galactic nuclei cores, where several-TeV gamma rays interact with the X-ray photons from the hot corona. We explore these scenarios within the CRPropa Monte Carlo code framework, developing dedicated tools to account for leptonic production and decay of heavy leptons and hadrons. In particular, the latter are performed by interfacing with the PYTHIA event generator. With these novel tools, we characterise the spectrum and flavour composition of neutrinos emerging from cosmological EM cascades and from leptonic processes in the core of active galactic nuclei. Finally, we investigate the leptonic production of neutrinos in the context of the IceCube detection of NGC 1068.

高质心电磁（EM）相互作用可以产生衰变的重轻子和强子，从而产生中微子。这些过程可能发生在最极端的天体物理场景中，可能会改变强子和轻子图像中预期的伽马射线和中微子通量。例如，中微子可能产生于高红移的电磁级联，由超过1018eV的伽马射线散射背景光子引发，从无线电到紫外线能带。在宇宙形成模型和涉及非标准物理的场景中，可以预测到这种高能伽马射线。在天体物理学的尺度上，中微子的轻子产生可能发生在活跃的星系核中，在那里，几tev的伽马射线与来自热日冕的x射线光子相互作用。我们在CRPropa蒙特卡罗代码框架中探索这些场景，开发专用工具来解释轻子的产生和重轻子和强子的衰变。特别是，后者是通过与PYTHIA事件生成器接口来执行的。利用这些新工具，我们描述了宇宙电磁级联和活动星系核核心轻子过程中出现的中微子的光谱和风味组成。最后，我们在冰立方探测ngc1068的背景下研究了中微子的轻子产生。

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引用次数: 0

The source of the cosmic-ray excess in the Centaurus region—Constraints on possible candidates, mass composition and cosmic magnetic fields 半人马座区域宇宙射线过剩的来源——对可能的候选者、质量组成和宇宙磁场的限制

IF 2.9 3区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Astroparticle Physics

Pub Date : 2025-11-19 DOI: 10.1016/j.astropartphys.2025.103190

Teresa Bister

<div><div>The most significant excess in the arrival directions of ultra-high-energy cosmic rays with energies <span><math><mrow><mo>≳</mo><mn>40</mn><mspace></mspace><mi>EeV</mi></mrow></math></span> is found in the direction of several interesting source candidates, most prominently the nearby radio galaxy Centaurus A. Naturally, Centaurus A has been suspected to create the anisotropy — but very different scenarios have been proposed. This includes a subdominant source contribution in combination with isotropic background sources, as well as a scenario where Centaurus A supplies the whole cosmic-ray flux above the ankle. Recently, it was suggested that the overdensity could instead consist of strongly deflected events from the Sombrero galaxy. Thanks to the recent development of several models of the Galactic magnetic field, it is now possible to test these proposed scenarios explicitly. We find that both sources inside the overdensity region (Centaurus A, NGC 4945, or M83), as well as outside of it (Sombrero galaxy) can in principle reproduce the excess. Leveraging the measured overdensity direction, significance, angular scale, and energy evolution, we place limits on the allowed signal fraction, the possible ejected charge number and the strength of the extragalactic magnetic field between the respective source and Earth. We find that the scenario of a subdominant source in the overdensity region requires the charge number to be <span><math><mrow><mi>Z</mi><mo>≲</mo><mn>6</mn></mrow></math></span> and the extragalactic magnetic field quantity <span><math><mrow><mi>B</mi><mo>/</mo><mi>nG</mi><msqrt><mrow><msub><mrow><mi>L</mi></mrow><mrow><mi>c</mi></mrow></msub><mo>/</mo><mi>Mpc</mi></mrow></msqrt></mrow></math></span> to be between <span><math><mrow><mspace></mspace><mn>1</mn></mrow></math></span> and <span><math><mrow><mspace></mspace><mn>100</mn></mrow></math></span> (depending on the charge and signal fraction). For the Sombrero galaxy to be the source, the dominant charge number has to be around <span><math><mrow><mi>Z</mi><mo>=</mo><mn>6</mn></mrow></math></span> with <span><math><mrow><mn>1</mn><mo>≲</mo><mi>B</mi><mo>/</mo><mi>nG</mi><msqrt><mrow><msub><mrow><mi>L</mi></mrow><mrow><mi>c</mi></mrow></msub><mo>/</mo><mi>Mpc</mi></mrow></msqrt><mo>≲</mo><mn>20</mn></mrow></math></span>. We find that a scenario where all the flux above <span><math><mrow><mn>30</mn><mspace></mspace><mi>EeV</mi></mrow></math></span> is supplied by Cen A or M83 is possible for <span><math><mrow><mn>20</mn><mo>≲</mo><mi>B</mi><mo>/</mo><mi>nG</mi><msqrt><mrow><msub><mrow><mi>L</mi></mrow><mrow><mi>c</mi></mrow></msub><mo>/</mo><mi>Mpc</mi></mrow></msqrt><mo>≲</mo><mn>30</mn></mrow></math></span> and a mixed composition – explaining both the Centaurus region excess and the distribution of the highest-energy events – however, another contributing source is possibly required in the energy range <span><math><mrow><mo><</mo><mn>30</mn><mspace></mspace><mi>EeV<

能量在40EeV以上的超高能宇宙射线的到达方向上最显著的过剩是在几个有趣的候选源的方向上发现的，最突出的是附近的射电星系半人马座A。自然地，半人马座A被怀疑是各向异性的产生者，但提出了非常不同的设想。这包括亚主导源与各向同性背景源的结合，以及半人马座a提供脚踝以上的整个宇宙射线通量的情况。最近，有人提出，过度密度可能是由来自草帽星系的强烈偏转事件组成的。由于最近几个银河系磁场模型的发展，现在有可能明确地测试这些提出的场景。我们发现，在密度过大的区域内（半人马座A、NGC 4945或M83）以及在密度过大区域外（Sombrero星系）的两个源原则上都可以复制过量的辐射。利用测量的过密度方向、重要性、角尺度和能量演化，我们对允许的信号分数、可能的喷射电荷数和各自源与地球之间的河外磁场强度进行了限制。我们发现，在过密度区存在亚优势源的情况下，需要电荷数Z > 6，河外磁场量B/nGLc/Mpc在1 ~ 100之间（取决于电荷和信号分数）。如果Sombrero星系是源星系，则主导电荷数必须在Z=6附近，且1 > B/nGLc/Mpc > 20。我们发现，在20≤B/nGLc/Mpc≤30的范围内，所有30EeV以上的通量都可能由半人马座a或M83提供，并且可能是一种混合成分——解释了半人马座区域的过剩和最高能量事件的分布——然而，在能量范围<；30EeV内可能需要另一个贡献源。

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引用次数: 0

Camera calibration of the first Large-Sized Telescope of the Cherenkov Telescope Array Observatory 切伦科夫望远镜阵列天文台首台大型望远镜的相机标定

IF 2.9 3区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Astroparticle Physics

Pub Date : 2025-11-17 DOI: 10.1016/j.astropartphys.2025.103189

Franca Cassol , Maximilian Linhoff , Yukiho Kobayashi , Julian Sitarek , Pawel Gliwny , Shunsuke Sakurai , Maurizio Iori , Michele Palatiello , Seiya Nozaki , Takayuki Saito

The Cherenkov Telescope Array Observatory (CTAO), a forthcoming very-high-energy gamma-ray facility, will use the Imaging Atmospheric Cherenkov Technique (IACT) to achieve unprecedented energy and angular resolution from 20 GeV to 300 TeV. Large-Sized Telescopes (LSTs) are crucial for the low-energy range. This paper details the calibration tools and methods developed for the first LST (LST-1) to ensure the precise conversion of photomultiplier tube signals and accurate photon timing, vital for the reconstruction of extensive air showers. This framework supports LST-1’s early science and will be applied to future LSTs.

切伦科夫望远镜阵列天文台（CTAO）是一个即将到来的高能伽玛射线设施，将使用成像大气切伦科夫技术（IACT）来实现从20 GeV到300 TeV的前所未有的能量和角分辨率。大型望远镜（large - size telescope, LSTs）是低能观测的关键。本文详细介绍了为第一个LST （LST-1）开发的校准工具和方法，以确保光电倍增管信号的精确转换和准确的光子定时，这对重建广泛的空气阵雨至关重要。该框架支持LST-1的早期科学研究，并将应用于未来的lst。

引用次数: 0

TXS 0506+056-like blazar sources and their role as possible neutrino emitters TXS 0506+056类耀变体源及其作为可能的中微子发射器的作用

IF 2.9 3区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Astroparticle Physics

Pub Date : 2025-11-17 DOI: 10.1016/j.astropartphys.2025.103191

I. Viale , G. Principe , C. Righi , M. Cerruti , F. Tavecchio , E. Bernardini

The interest in blazars as candidate neutrino emitters grew after the 3

σ

evidence for a contemporaneous joint photon and neutrino emission from the flaring blazar TXS 0506+056 in 2017. Blazars, a class of extragalactic sources with relativistic jets pointing toward Earth, present a broadband emission interpretable via leptonic and hadronic processes, the latter relevant for proton acceleration and neutrino production. Several emission models have been developed to explain this multi-messenger observation, but the details of the neutrino production and the nature of TXS 0506+056 are not yet fully understood. In this work we investigate the properties of sources similar to TXS 0506+056. We select a sample of blazars from the Fermi 4LAC-DR2 catalog by constraining a number of key parameters in ranges centered on TXS 0506+056 values. We estimate their disk accretion efficiency and model their spectral energy distribution (SED) in terms of lepto-hadronic emission, gaining information respectively on the potential similarity of their environment with that of TXS 0506+056 and on their neutrino flux and detectability prospects at TeV energies. Our study shows the candidates’ high energy emission to be dominated by leptonic processes. Part of them also show a high accretion rate, characteristic of FSRQs. For these sources, the very high energy (VHE) and neutrino fluxes appear undetectable by current and future instruments in an average emission state.

2017年，从燃烧的耀变体TXS 0506+056获得同时光子和中微子联合发射的3σ证据后，人们对耀变体作为候选中微子发射器的兴趣增加了。Blazars是一类具有指向地球的相对论性喷流的河外源，它呈现出一种宽带发射，可以通过轻子和强子过程来解释，后者与质子加速和中微子产生有关。已经开发了几种发射模型来解释这种多信使观测，但是中微子产生的细节和TXS 0506+056的性质尚未完全了解。在这项工作中，我们研究了类似于txs0506 +056的源的性质。我们通过限制以TXS 0506+056值为中心的一系列关键参数，从费米4LAC-DR2星表中选择了一个blazar样本。我们估计了它们的盘吸积效率，并根据轻强子发射建立了它们的光谱能量分布（SED）模型，分别获得了它们与TXS 0506+056环境的潜在相似性以及它们在TeV能量下的中微子通量和可探测性前景的信息。我们的研究表明候选粒子的高能量发射是由轻子过程主导的。其中一部分还表现出高吸积速率，这是FSRQs的特征。对于这些源，在平均发射状态下，目前和未来的仪器似乎无法检测到极高能量（VHE）和中微子通量。

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引用次数: 0

Multi-wavelength variability of Mrk 501 during the observations with MACE in June–July, 2022 2022年6 - 7月MACE观测期间Mrk 501的多波长变化

IF 2.9 3区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Astroparticle Physics

Pub Date : 2025-10-28 DOI: 10.1016/j.astropartphys.2025.103188

P. Pandey , B. Ghosal , C. Borwankar , A. Tolamatti , Z.A. Dar , S. Godiyal , S. Godambe , J. Hariharan , Keshvanand , N. Mankuzhyil , S. Norlha , D. Sakar , R. Thubstan , K. Venugopal , A. Pathania , K.K. Singh , M. Khurana , P. Chandra , M.K. Koul , S.V. Kotwal , K.K. Yadav

Mrk 501, a high synchrotron peak blazar (HBL), located at a redshift of z

=

0.034, is known for its frequent flaring episodes across various energy bands. Very high energy (VHE)

γ

-ray emission in the energy range from 80 GeV to 3.2 TeV from Mrk 501 was detected by MACE telescope during of June–July, 2022. It is found that the VHE emission from the source remained steady during that period with an average flux value of

(1.62 \pm 0.13) \times 1 0^{- 10} {ph cm}^{- 2} s^{- 1}

. An X-ray flare was detected by Swift-XRT in the energy range of 0.3–10 keV during the observation period. In this work, a comprehensive multi-wavelength analysis of the Mrk 501 is presented using the observations from MACE, Fermi-LAT, Swift-BAT, Swift-XRT and Swift-UVOT. The analysis is focused on characterising the X-ray variability during the observation period. Significant X-ray spectral variations were found in the source, showing spectral hardening during the X-ray flaring activity. Spectral energy distributions (SEDs) were obtained using quasi-simultaneous multi-wavelength data during both the high and low X-ray flux states. Theoretical modelling of the SEDs was done using a leptonic model. It is found that both the SEDs corresponding to the high and low X-ray flux states could be explained within the framework of a one-zone leptonic model. The study provides insights into the emission mechanisms of Mrk 501 and its role in understanding the underlying particle distribution in the source.

Mrk 501是一个高同步峰耀变体（HBL），位于红移z = 0.034处，以其频繁的在不同能带上的耀斑事件而闻名。MACE望远镜于2022年6 - 7月探测到Mrk 501发射的高能γ射线（VHE），能量范围为80gev ~ 3.2 TeV。在此期间，源的VHE辐射保持稳定，平均通量值为（1.62±0.13）×10−10ph cm−2s−1。在观测期间，Swift-XRT探测到一个能量在0.3 ~ 10 keV的x射线耀斑。本文利用MACE、Fermi-LAT、Swift-BAT、Swift-XRT和Swift-UVOT的观测数据，对Mrk 501进行了全面的多波长分析。分析的重点是表征观测期间的x射线变异性。在源中发现了显著的x射线光谱变化，表明在x射线耀斑活动期间光谱硬化。利用准同步多波长数据获得了高、低x射线通量状态下的光谱能量分布。用轻子模型建立了SEDs的理论模型。发现对应于高和低x射线通量态的SEDs都可以在单区轻子模型的框架内解释。该研究为了解Mrk 501的排放机制及其在了解源中潜在颗粒分布方面的作用提供了见解。

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引用次数: 0

Time structure variation of extensive air shower particles initiated by vertical protons during thunderstorms at LHAASO site LHAASO站点雷暴中垂直质子引发的大范围空气阵雨粒子的时间结构变化

IF 2.9 3区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Astroparticle Physics

Pub Date : 2025-10-14 DOI: 10.1016/j.astropartphys.2025.103187

X.J. Chen , X.X. Zhou , H.H. He , R.M. Wei , C. Yang , K.J. Guo , T. Zhou , S.Y. Ji

Crossing kilometer-sized thunderclouds, the characteristic parameters, such as the temporal structure and spatial distribution of extensive air shower (EAS) induced by cosmic ray, will be changed. To study the time structure variations of secondary electromagnetic particles (i.e., electrons, positrons, and photons) in EAS produced by vertical primary proton at LHAASO observatory level during thunderstorms, detailed Monte Carlo simulations are performed with CORSIKA. The results indicate that the temporal variations of EAS particles are highly dependent on the polarity and strength of the atmospheric electric field (AEF), the AEF layer thickness, the core distance, and the types of secondary particles. For secondary electrons and positrons, the opposite temporal variations occur, depending on the polarity of the electric field in thundercloud. For secondary photons, the time distributions are broadening in positive or negative fields. With the increasing of AEF strength and layer thickness, the temporal variations increase. In a field of -1000 V/cm with a layer thickness of 1000 m, the average arrival time and the time width increase by 12.2 ns and 20.8 ns for electrons, 0.9 ns and 8.3 ns for photons, while decrease by -5.2 ns and -8.0 ns for positrons. As the core distance grows, the temporal variations are larger. In this work, the primary energy dependence of the time structure variations during thunderstorms are also simulated. These simulations not only enhance our understanding of the acceleration/deceleration mechanism of EAS particles caused by AEF, but also offer predictions for observed data with ground-based experiments during thunderstorms.

穿越千米级雷雨云时，宇宙射线诱发的大范围空气阵雨（EAS）的时间结构和空间分布等特征参数将发生改变。为了研究雷暴期间LHAASO天文台水平垂直初级质子产生的EAS中二次电磁粒子（即电子、正电子和光子）的时间结构变化，利用CORSIKA进行了详细的蒙特卡罗模拟。结果表明：大气电场的极性和强度、电场层厚度、磁芯距离和二次粒子的类型与东亚地区大气电场粒子的时间变化密切相关。对于次级电子和正电子，则发生相反的时间变化，这取决于雷云中电场的极性。对于二次光子，时间分布在正场或负场中展宽。随着电场强度和层厚的增加，时间变化幅度增大。在-1000 V/cm、层厚为1000 m的电场中，电子的平均到达时间和时间宽度分别增加12.2 ns和20.8 ns，光子的平均到达时间和时间宽度分别增加0.9 ns和8.3 ns，而正电子的平均到达时间和时间宽度分别减少-5.2 ns和-8.0 ns。随着地核距离的增加，时间变化越大。本文还模拟了雷暴期间时间结构变化的一次能量依赖性。这些模拟不仅加深了我们对AEF引起的EAS粒子加速/减速机制的理解，而且为雷暴期间地面实验观测数据的预测提供了依据。

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引用次数: 0

Uncertainties in the estimation of air shower observables from Monte Carlo simulation of radio emission 无线电发射蒙特卡罗模拟估算风淋观测值的不确定性

IF 2.9 3区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Astroparticle Physics

Pub Date : 2025-10-09 DOI: 10.1016/j.astropartphys.2025.103183

Carlo S. Cruz Sanchez , Patricia M. Hansen , Matias Tueros , Jaime Alvarez-Muñiz , Diego G. Melo

The detection of extensive air showers (EAS) induced by cosmic rays via radio signals has undergone significant advancements in the last two decades. Numerous ultra-high energy cosmic ray experiments routinely capture radio pulses in the MHz to GHz frequency range emitted by EAS. The Monte Carlo simulation of these radio pulses is crucial to enable an accurate reconstruction of the primary cosmic ray energy and to infer the composition of the primary particles. In this work, a comprehensive comparison of the predicted electric field in EAS simulated with CoREAS and ZHAireS was conducted to estimate the systematic uncertainties arising from the use of different simulation packages in the determination of two key shower observables namely, the electromagnetic energy of the EAS and the depth of maximum development (

X_{max}

). For this comparison, input parameters and settings as similar as possible were used in both simulations, along with the same realistic atmospheric refractive index depending on altitude, which is crucial for the prediction of radio emission properties of EAS. In addition, simulated EAS with very similar values of depth of maximum development were selected. Good agreement was found between CoREAS and ZHAireS, with discrepancies in the dominant electric field components generally remaining below 10% across the frequency range of a few MHz to hundreds of MHz, relevant for most radio detection experiments, translating into uncertainties in the determination of energy below 5% and

≃ 10 {g/cm}^{2}

in

X_{max}

. Our work underscores the need for further studies to clarify their origin and impact on

X_{max}

inference in composition analyses.

在过去的二十年里，通过无线电信号探测宇宙射线引起的大范围空气阵雨（EAS）取得了重大进展。许多超高能量宇宙射线实验经常捕获由EAS发射的MHz到GHz频率范围内的无线电脉冲。这些射电脉冲的蒙特卡罗模拟对于精确重建主要宇宙射线能量和推断主要粒子的组成至关重要。在这项工作中，对CoREAS和ZHAireS模拟的EAS预测电场进行了全面比较，以估计在确定EAS的电磁能和最大发展深度（Xmax）这两个关键观测值时，使用不同的模拟软件包所产生的系统不确定性。为了进行比较，在两个模拟中都使用了尽可能相似的输入参数和设置，以及相同的实际大气折射率，这对于预测EAS的射电发射特性至关重要。此外，还选择了具有非常相似的最大发育深度值的模拟EAS。CoREAS和ZHAireS的结果一致，在几MHz到几百MHz的频率范围内，主要电场分量的差异通常保持在10%以下，这与大多数无线电探测实验相关，这导致在Xmax中能量低于5%和10g/cm2的不确定性。我们的工作强调需要进一步的研究来澄清它们的起源和对成分分析中Xmax推断的影响。

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引用次数: 0