Astroparticle Physics最新文献

{"title":"Universality of Cherenkov light in EAS","authors":"Isaac J. Buckland,&nbsp;D.R. Bergman","doi":"10.1016/j.astropartphys.2023.102832","DOIUrl":"10.1016/j.astropartphys.2023.102832","url":null,"abstract":"<div><p>The reconstruction of cosmic-ray-induced extensive air showers with a non-imaging Cherenkov detector array requires knowledge of the Cherenkov yield of any given air shower for a given set of shower parameters. Although air showers develop in a stochastic cascade, certain characteristics of the particles in the shower have been shown to come from universal probability distributions, a property known as shower universality. Both the energy and the angular distributions of charged particles within a shower have been parameterized. One can use these distributions to calculate the Cherenkov photon yield as an angular distribution from the Cherenkov cones of charged particles at various stages of shower development. This Cherenkov photon yield can then be tabulated for use in the reconstruction of air showers. In this work, we develop the calculation of both the Cherenkov angular distribution and Cherenkov yield per shower particle, and show how a look-up table was constructed to capture the relevant features of these distributions for general use. We compare the results of our calculations with the results of full, particle-stack, Monte Carlo simulation of the Cherenkov light produced in extensive air showers using CORSIKA-IACT. We make comparisons of both the lateral distribution of the Cherenkov photon flux amongst several detectors and of the arrival-time distribution of the Cherenkov photons in a single detector.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"150 ","pages":"Article 102832"},"PeriodicalIF":3.5,"publicationDate":"2023-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"45189681","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Searches for continuous gravitational waves from neutron stars: A twenty-year retrospective","authors":"Karl Wette","doi":"10.1016/j.astropartphys.2023.102880","DOIUrl":"https://doi.org/10.1016/j.astropartphys.2023.102880","url":null,"abstract":"<div><p>Seven years after the first direct detection of gravitational waves, from the collision of two black holes, the field of gravitational wave astronomy is firmly established. A first detection of continuous gravitational waves from rapidly-spinning neutron stars could be the field’s next big discovery. I review the last twenty years of efforts to detect continuous gravitational waves using the LIGO and Virgo gravitational wave detectors. I summarise the model of a continuous gravitational wave signal, the challenges to finding such signals in noisy data, and the data analysis algorithms that have been developed to address those challenges. I present a quantitative analysis of 297 continuous wave searches from 80 papers, published from 2003 to 2022, and compare their sensitivities and coverage of the signal model parameter space.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"153 ","pages":"Article 102880"},"PeriodicalIF":3.5,"publicationDate":"2023-07-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"49757193","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Ultra high energy cosmic rays The intersection of the Cosmic and Energy Frontiers","authors":"A. Coleman ,&nbsp;J. Eser ,&nbsp;E. Mayotte ,&nbsp;F. Sarazin ,&nbsp;F.G. Schröder ,&nbsp;D. Soldin ,&nbsp;T.M. Venters ,&nbsp;R. Aloisio ,&nbsp;J. Alvarez-Muñiz ,&nbsp;R. Alves Batista ,&nbsp;D. Bergman ,&nbsp;M. Bertaina ,&nbsp;L. Caccianiga ,&nbsp;O. Deligny ,&nbsp;H.P. Dembinski ,&nbsp;P.B. Denton ,&nbsp;A. di Matteo ,&nbsp;N. Globus ,&nbsp;J. Glombitza ,&nbsp;G. Golup ,&nbsp;M. Zotov","doi":"10.1016/j.astropartphys.2023.102819","DOIUrl":"10.1016/j.astropartphys.2023.102819","url":null,"abstract":"<div><p>The present white paper is submitted as part of the “Snowmass” process to help inform the long-term plans of the United States Department of Energy and the National Science Foundation for high-energy physics. It summarizes the science questions driving the Ultra-High-Energy Cosmic-Ray (UHECR) community and provides recommendations on the strategy to answer them in the next two decades.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"149 ","pages":"Article 102819"},"PeriodicalIF":3.5,"publicationDate":"2023-07-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"49327732","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"A new ultra low-level HPGe activity counting setup in the Felsenkeller shallow-underground laboratory","authors":"S. Turkat ,&nbsp;D. Bemmerer ,&nbsp;A. Boeltzig ,&nbsp;A.R. Domula ,&nbsp;J. Koch ,&nbsp;T. Lossin ,&nbsp;M. Osswald ,&nbsp;K. Schmidt ,&nbsp;K. Zuber","doi":"10.1016/j.astropartphys.2023.102816","DOIUrl":"10.1016/j.astropartphys.2023.102816","url":null,"abstract":"<div><p>A new ultra low-level counting setup has been installed in the shallow-underground laboratory Felsenkeller in Dresden, Germany. It includes a high-purity germanium detector (HPGe) of 163% relative efficiency within passive and active shields. The passive shield consists of 45 m rock overburden (140 meters water equivalent), 40 cm of low-activity concrete, and a lead and copper castle enclosed by an anti-radon box. The passive shielding alone is found to reduce the background rate to rates comparable to other shallow-underground laboratories. An additional active veto is given by five large plastic scintillation panels surrounding the setup. It further reduces the background rate by more than one order of magnitude down to 116(1) kg⁻¹d⁻¹ in an energy interval of [40 keV;2700 keV]. This low background rate is unprecedented for shallow-underground laboratories and close to deep underground laboratories.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"148 ","pages":"Article 102816"},"PeriodicalIF":3.5,"publicationDate":"2023-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"49118151","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Analytic fluid approximation for warm dark matter","authors":"Jorge Mastache ,&nbsp;Axel de la Macorra","doi":"10.1016/j.astropartphys.2023.102818","DOIUrl":"10.1016/j.astropartphys.2023.102818","url":null,"abstract":"&lt;div&gt;&lt;p&gt;&lt;span&gt;We present the cosmological evolution&lt;span&gt; of the velocity of a massive particle, along with its equation of state. Both quantities are expressed in terms of &lt;/span&gt;&lt;/span&gt;&lt;span&gt;&lt;math&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;a&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;mi&gt;r&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/math&gt;&lt;/span&gt;&lt;span&gt;, the moment when a massive particle becomes nonrelativistic. The expressions for the energy density and pressure for the background evolution are also in terms of &lt;/span&gt;&lt;span&gt;&lt;math&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;a&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;mi&gt;r&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/math&gt;&lt;/span&gt;&lt;span&gt;; therefore, the perturbation equations for any massively decoupled particle, i.e., warm dark matter (WDM) or neutrinos, can be computed in the fluid approximation. A relation between the mass of the WDM particle, &lt;/span&gt;&lt;span&gt;&lt;math&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;m&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;wdm&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/math&gt;&lt;/span&gt;, with the moment of the nonrelativistic transition, &lt;span&gt;&lt;math&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;a&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;mi&gt;r&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/math&gt;&lt;/span&gt;, and the temperature ratio with the neutrinos, &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;T&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;wdm&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;mo&gt;/&lt;/mo&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;T&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;ν&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;, are obtained and compared to results from Boltzmann solvers as CLASS with a non-cold relic as WDM. We found that using the analytic fluid approximation, the value of &lt;span&gt;&lt;math&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;a&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;n&lt;/mi&gt;&lt;mi&gt;r&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/math&gt;&lt;/span&gt; is 2.1% different on average in a wide range of WDM masses, and the temperature ratio is 7.1% lower than previous parametrizations. A smooth velocity dispersion for the WDM allows us to compute the cut-off scale in structure formation due to the free-streaming (&lt;span&gt;&lt;math&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;λ&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;f&lt;/mi&gt;&lt;mi&gt;s&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;/math&gt;&lt;/span&gt;&lt;span&gt;), which is a feature for a WDM particle to explain the satellite problem. The cut-off in the matter power spectrum and halo mass function using the analytic fluid approximation is similar to the Boltzmann solvers with a non-cold relic and the transfer function from numerical simulations. This approach provides a more detailed description and a deeper understanding of the WDM cosmological evolution by understanding the velocity dispersion of a WDM particle. Comprehensive numerical modeling can incorporate the analytical fluid formulation, potentially improving calculation performance, for instance, running MCMC for a &lt;/span&gt;&lt;span&gt;&lt;math&gt;&lt;mi&gt;Λ&lt;/mi&gt;&lt;/math&gt;&lt;/span&gt;&lt;span&gt;WDM scenario using CMB Planck and WiggleZ data, we obtained a lower bound for the WDM mass &lt;/span&gt;&lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;msub&gt;&lt;mrow&gt;&lt;mi&gt;m&lt;/mi&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mi&gt;wdm&lt;/mi&gt;&lt;/mrow&gt;&lt;/msub&gt;&lt;mo&gt;&gt;&lt;/mo&gt;&lt;mn&gt;70&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;mn&gt;3&lt;/mn&gt;&lt;mspace&gt;&lt;/mspace&gt;&lt;mi&gt;eV&lt;/mi&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; at &lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mn&gt;1&lt;/mn&gt;&lt;mi&gt;σ&lt;/mi&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt; confidence. Still, more data at small scales or a combination with other observations are needed to constrain the mass value of the ","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"148 ","pages":"Article 102818"},"PeriodicalIF":3.5,"publicationDate":"2023-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"46878127","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Connecting multi-lepton anomalies at the LHC and in Astrophysics with MeerKAT/SKA","authors":"Geoff Beck ,&nbsp;Ralekete Temo ,&nbsp;Elias Malwa ,&nbsp;Mukesh Kumar ,&nbsp;Bruce Mellado","doi":"10.1016/j.astropartphys.2023.102821","DOIUrl":"10.1016/j.astropartphys.2023.102821","url":null,"abstract":"<div><p><span><span>Multi-lepton anomalies at the Large Hadron Collider (LHC) are reasonably well described by a two Higgs doublet model with an additional singlet scalar. Here we demonstrate that using this model, with parameters set by the LHC, we are also able to describe the excesses in gamma-ray flux from the </span>galactic centre and the cosmic-ray spectra from AMS-02. This is achieved through Dark Matter (DM) annihilation via the singlet scalar. Of great interest is the flux of </span>synchrotron emissions<span> which results from annihilation of DM in Milky-Way satellites. We make predictions for MeerKAT/SKA observations of the nearby dwarf galaxy Reticulum II and we demonstrate the power of this instrument as a new frontier in indirect dark matter searches. Since the dark matter sector of the aforementioned two Higgs doublet model is unconstrained by current LHC data, we also demonstrate a synergy between particle and astrophysical searches in order to motivate further exploration of this promising model.</span></p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"148 ","pages":"Article 102821"},"PeriodicalIF":3.5,"publicationDate":"2023-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"47080541","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Criticality and phase transition of Kerr–anti-de Sitter black hole with quintessence and cloud of strings","authors":"Qanitah Ama-Tul-Mughani ,&nbsp;Rabia Saleem ,&nbsp;Wardat Us Salam ,&nbsp;Sobia Sadiq","doi":"10.1016/j.astropartphys.2023.102820","DOIUrl":"10.1016/j.astropartphys.2023.102820","url":null,"abstract":"<div><p><span>In this paper, a thermodynamical study of the Kerr–anti-de Sitter (KAdS) black hole (BH) encircled by quintessence matter and the cloud of strings is presented. We check the effects of the cloud parameter on the thermodynamical variables including Hawking temperature, entropy, Helmholtz free energy (HFE), Gibbs free energy (GFE), and specific heat capacity. These thermodynamic variables hold the Smarr–Gibbs–Dehum (SGD) relation in the appearance of quintessence and the cloud of the string parameter. Then we calculate the critical expressions of the developed variables in two different ways that are “Van-der-Waals (vdW)-type equation of state” (EoS) and the “Maxwell equal-area law” (MEAL). The latter technique is found to be more reasonable to examine the criticality of the complex BHs. Using MEAL, we plot the </span>phase diagram in a temperature–entropy plane and obtain an isobar, which represents the co-existence region of liquid–gas phases. It is concluded that the uncharged BHs exhibit the same phase transition (PT) to vdW fluid as the temperature drops down its critical value. Also, we discuss the influence of thermal fluctuations (TF) on the stability of KAdS BH.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"148 ","pages":"Article 102820"},"PeriodicalIF":3.5,"publicationDate":"2023-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"46030996","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Lorentz invariance violation induced threshold anomaly versus very-high energy cosmic photon emission from GRB 221009A","authors":"Hao Li ,&nbsp;Bo-Qiang Ma","doi":"10.1016/j.astropartphys.2023.102831","DOIUrl":"10.1016/j.astropartphys.2023.102831","url":null,"abstract":"<div><p><span>It has been reported that the Large High Altitude Air Shower<span> Observatory (LHAASO) observed very high energy photons from GRB 221009A, with the highest energy reaching 18 TeV. We find that observation of such high energy photons is quite nontrivial since extragalactic background light could absorb these photons severely and the flux is too weak to be observed. Therefore we discuss a potential mechanism for us to observe these photons, and suggest that Lorentz invariance violation induced threshold anomaly of the process </span></span><span><math><mrow><mi>γ</mi><mi>γ</mi><mo>→</mo><msup><mrow><mi>e</mi></mrow><mrow><mo>−</mo></mrow></msup><msup><mrow><mi>e</mi></mrow><mrow><mo>+</mo></mrow></msup></mrow></math></span> provides a candidate to explain this phenomenon.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"148 ","pages":"Article 102831"},"PeriodicalIF":3.5,"publicationDate":"2023-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"41392872","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"An improved method of estimating the uncertainty of air-shower size at ultra-high energies","authors":"A. Coleman ,&nbsp;P. Billoir ,&nbsp;O. Deligny","doi":"10.1016/j.astropartphys.2023.102815","DOIUrl":"10.1016/j.astropartphys.2023.102815","url":null,"abstract":"<div><p>The collection of a statistically significant number detected of cosmic rays with energy above <span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>17</mn></mrow></msup></mrow></math></span> to <span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>18</mn></mrow></msup></mrow></math></span><span> eV requires widely-spaced particle detectors at the ground level to detect the extensive air showers<span> induced in the atmosphere. The air-shower sizes, proxies of the primary energies, are then estimated by fitting the observed signals to a functional form for expectations so as to interpolate the signal at a reference distance. The functional form describes the rapid falloff of the expected signal with the distance from the shower core, using typically two logarithmic slopes to account for the short-range and long-range decreases of signals. The uncertainties associated to the air-shower sizes are determined under the assumption of a quadratic dependence of the log-likelihood on the fitted parameters around the minimum, so that a meaningful variance–covariance matrix is provided. In this paper, we show that for an event topology where one signal is much larger than the others, the quadratic dependence of the fitted function around the minimum is a poor approximation that leads to an inaccurate estimate of the uncertainties. To restore a quadratic shape, we propose to use the polar coordinates around the detector recording the largest signal, projected onto the plane of the shower front, to define the likelihood function in terms of logarithmic polar distances, polar angles and logarithmic shower sizes as free parameters. We show that a meaningful variance–covariance matrix is then recovered in the new coordinate system, as the dependence of the fitted function on the modified parameters is properly approximated by a quadratic function. The use of the uncertainties in the new coordinate system for subsequent high-level analyses is illustrated.</span></span></p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"148 ","pages":"Article 102815"},"PeriodicalIF":3.5,"publicationDate":"2023-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"46453837","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Cosmic-ray measurements with an array of Cherenkov telescopes using reconstruction of longitudinal profiles of air showers","authors":"Andrés G. Delgado Giler,&nbsp;Vitor de Souza","doi":"10.1016/j.astropartphys.2023.102817","DOIUrl":"10.1016/j.astropartphys.2023.102817","url":null,"abstract":"<div><p><span>We present a method to reconstruct the longitudinal profile of electrons in showers using Cherenkov telescopes. We show how the Cherenkov light collected by an array of telescopes can be transformed into the number of electrons as a function of atmospheric depth. This method is validated using air shower and simplified telescope simulations. The reconstruction of the depth in which the shower has the maximum number of electrons (X</span><span><math><msub><mrow></mrow><mrow><mi>max</mi></mrow></msub></math></span>) opens the possibility of cosmic ray composition studies with Cherenkov telescopes in the energy range from 10 to 100 TeV.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"148 ","pages":"Article 102817"},"PeriodicalIF":3.5,"publicationDate":"2023-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"48059253","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}