Astroparticle Physics最新文献

{"title":"Characterizing interplanetary magnetic field fluctuations at arctic using cosmic ray secondaries–An approach with machine learning","authors":"Sandipan Dawn ,&nbsp;A.K. Bakshi ,&nbsp;P.K. Mohanty ,&nbsp;Sujoy Chatterjee ,&nbsp;B.K. Sahoo ,&nbsp;B.K. Sapra","doi":"10.1016/j.astropartphys.2025.103087","DOIUrl":"10.1016/j.astropartphys.2025.103087","url":null,"abstract":"<div><div>This study explores the potential of ground-based cosmic ray measurements to quantify solar weather parameters, specifically the total interplanetary magnetic field (B_t). A compact Tissue Equivalent Proportional Counter (TEPC), meant for measuring radiation doses in human tissue, was set up at Ny-Ålesund near the North Pole, a region with zero geomagnetic cut-off, which allows for detailed measurements of the different components of cosmic rays. The TEPC continuously monitored low Linear Energy Transfer (LET) cosmic ray components, mainly electrons, and photons during two different seasons: January to March (winter) and September (summer) in 2024. Monte Carlo simulations using PHITS and EXPACS were carried out to understand the changes in cosmic ray flux related to solar weather. To model the relationship between cosmic ray flux and B_t, two machine learning algorithms were used: Gaussian Process Regression (GPR) and Artificial Neural Networks (ANN). Cosmic ray neutron data from the Oulu neutron monitor, which is part of the global neutron monitor network for studying solar weather, were included in the model. Adding the low LET data increased the R² value in the GPR model from 0.81 to 0.90 on the training data, and in the ANN model from 0.76 to 0.88 in comparison to only neutron data, showing a significant improvement in predictive ability. The results show a significant correlation between cosmic ray variations and B_t, suggesting that ground based cosmic ray data collected at low geomagnetic cut-offs—as captured by the TEPC in Ny-Ålesund, can be a reliable way to estimate B_t, especially when satellite data is unavailable. This approach offers a promising, cost-effective method for continuous solar weather monitoring, providing valuable insights into the effect of solar activity on cosmic rays, in turn, helping to make space-based technological systems more resilient.</div></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"167 ","pages":"Article 103087"},"PeriodicalIF":4.2,"publicationDate":"2025-01-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143182016","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":"Many body gravity and the bullet cluster","authors":"S. Ganesh","doi":"10.1016/j.astropartphys.2025.103080","DOIUrl":"10.1016/j.astropartphys.2025.103080","url":null,"abstract":"<div><div>Many body gravity (MBG) is an alternate theory of gravity, which has been able to explain the galaxy rotation curves, the radial acceleration relation (RAR) and the wide binary stars (WBS). The genesis of MBG is a novel theory, which models systems with thermal gradients, by recasting the variation in the temperature as a variation in the metric. Merging the above concept with Einstein’s gravity, leads to the theory of thermal gravity in 5-D space–time–temperature. Thermal gravity when generalized for partially thermalized systems, results in the theory of MBG. The bullet cluster is supposed to be a smoking gun evidence for the presence of dark matter. However, this work demonstrates that the MBG theory can naturally explain the weak gravitational lensing effect of the bullet cluster, without the need for yet undiscovered baryonic matter or dark matter.</div></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"167 ","pages":"Article 103080"},"PeriodicalIF":4.2,"publicationDate":"2025-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143182013","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":"Test results of the optical calibration system for the Large Sized Telescope camera","authors":"M. Iori,&nbsp;F. Ferrarotto,&nbsp;L. Recchia,&nbsp;A. Girardi,&nbsp;R. Lunadei","doi":"10.1016/j.astropartphys.2025.103079","DOIUrl":"10.1016/j.astropartphys.2025.103079","url":null,"abstract":"<div><div>In 2018 the Large Sized Telescope (LST-1) prototype, designed to be the lowest energy detector for the Cherenkov Telescope Array Observatory, was inaugurated at the Observatorio de Roque de Los Muchachos in La Palma, Canary Island and today three more are under construction, LST2-4. The LST camera, with 1855 photomultipliers (PMTs), requires precise and regular calibration. The camera calibration system (hereafter CaliBox), installed at the center of the telescope mirror dish, is equipped with a Q-switching 355 nm UV laser corresponding to the wavelength at which the maximum camera PMT quantum efficiency is achieved, a set of filters to guarantee a large dynamic range of photons on each camera pixel, and a Ulbricht sphere to spread uniformly the laser light over the camera plane 28 m away. The system is managed by an ODROID-C1+ single board computer that communicates through an Open Platform Communication Unified Architecture (OPCUA) protocol to the camera. The CaliBox is designed to fulfill the requirements needed for the calibration of the camera including the monitor of the photon flux to guarantee the quality of the CaliBox system of laser stability, uniform illumination and intensity range. In this paper, we present in detail the optical system, the monitor of the photon flux, the relevant electronic to monitor the device. The performance of the device, the photon flux monitoring, the evaluation of the photon flux sent to the camera obtained during tests performed in laboratory are shown.</div></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"167 ","pages":"Article 103079"},"PeriodicalIF":4.2,"publicationDate":"2025-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143182014","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"A systematic assessment of Data Volume Reduction for IACTs","authors":"Clara Escañuela Nieves,&nbsp;Felix Werner,&nbsp;Jim Hinton","doi":"10.1016/j.astropartphys.2025.103078","DOIUrl":"10.1016/j.astropartphys.2025.103078","url":null,"abstract":"<div><div>High-energy cosmic rays generate air showers of secondary particles when they enter the Earth’s atmosphere. These highly energetic particles emit Cherenkov light that can be detected by Imaging Air Cherenkov Telescopes (IACTs) or Water-Cherenkov Detectors at mountain altitudes. Advances in the technique and larger collection areas have increased the rate at which air shower events can be captured, and the amount of data produced by modern high-time-resolution Cherenkov cameras. Therefore, <em>Data Volume Reduction</em> (DVR) has become critical for such telescope arrays, ensuring that only relevant information regarding the air shower is stored long-term. Given the vast amount of raw data, owing to the highest resolution and sensitivity, the upcoming Cherenkov Telescope Array Observatory (CTAO) will need robust data reduction strategies to ensure efficient data handling and a sustainable data analysis. The CTAO data rates needs to be reduced from hundreds of Petabytes (PB) per year to a few PB/year.</div><div>This paper presents DVR algorithms tailored for CTAO but also applicable for other existing IACT arrays, focusing on the selection of pixels likely to contain Cherenkov light from the air shower. It describes and evaluates multiple algorithms based on their signal efficiency, noise rejection, and shower reconstruction. With a focus on a time-based clustering algorithm which demonstrates a notable enhancement in the retention of low level signal pixels. Moreover, the robustness is assessed under different observing conditions, including detector defects. Through testing and analysis, it is shown that these algorithms offer promising solutions for efficient volume reduction in CTAO. They effectively address the challenges posed by the array’s very large data volume and ensure reliable data storage amidst varying observational conditions and hardware issues.</div></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"167 ","pages":"Article 103078"},"PeriodicalIF":4.2,"publicationDate":"2025-01-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143182012","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"A measurement of the all-particle energy spectrum of cosmic rays from 1013 to 1015eV using HAWC","authors":"R. Alfaro ,&nbsp;C. Alvarez ,&nbsp;J.C. Arteaga-Velázquez ,&nbsp;D. Avila Rojas ,&nbsp;H.A. Ayala Solares ,&nbsp;E. Belmont-Moreno ,&nbsp;A. Bernal ,&nbsp;K.S. Caballero-Mora ,&nbsp;T. Capistrán ,&nbsp;A. Carramiñana ,&nbsp;S. Casanova ,&nbsp;J. Cotzomi ,&nbsp;S. Coutiño de León ,&nbsp;E. De la Fuente ,&nbsp;D. Depaoli ,&nbsp;P. Desiati ,&nbsp;N. Di Lalla ,&nbsp;R. Diaz Hernandez ,&nbsp;M.A. DuVernois ,&nbsp;J.C. Díaz-Vélez ,&nbsp;C. de León","doi":"10.1016/j.astropartphys.2024.103077","DOIUrl":"10.1016/j.astropartphys.2024.103077","url":null,"abstract":"<div><div>We report the total energy spectrum of cosmic rays in the energy interval from <span><math><mrow><mn>10</mn><mspace></mspace><mtext>TeV</mtext></mrow></math></span> to <span><math><mrow><mn>1</mn><mspace></mspace><mtext>PeV</mtext></mrow></math></span>, which lies in the energy region where both direct and indirect cosmic ray experiments overlap. The all-particle spectrum was obtained from an unfolding analysis of 5.3 years of data collected with the High Altitude Water Cherenkov (HAWC) observatory for zenith angles smaller than or equal to 35°. The study was carried out in the framework of the QGSJET-II-04 hadronic interaction model. The measured spectrum confirms the presence of a knee-like feature at tens of TeV. In our analysis, the position of this softening is found at <span><math><mrow><mn>40</mn><mo>.</mo><mn>2</mn><mo>±</mo><mn>1</mn><mo>.</mo><mn>0</mn></mrow></math></span>(stat.)<span><math><msubsup><mrow></mrow><mrow><mo>−</mo><mn>6</mn><mo>.</mo><mn>4</mn></mrow><mrow><mo>+</mo><mn>6</mn><mo>.</mo><mn>2</mn></mrow></msubsup></math></span>(sys.)<span><math><mrow><mspace></mspace><mspace></mspace><mi>TeV</mi></mrow></math></span>. The measured spectral indices before and after the break are <span><math><mrow><msub><mrow><mi>γ</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>=</mo><mo>−</mo><mn>2</mn><mo>.</mo><mn>53</mn><mspace></mspace><mo>±</mo><mspace></mspace><mn>0</mn><mo>.</mo><mn>01</mn></mrow></math></span>(stat.)<span><math><msubsup><mrow></mrow><mrow><mo>−</mo><mn>0</mn><mo>.</mo><mn>05</mn></mrow><mrow><mo>+</mo><mn>0</mn><mo>.</mo><mn>04</mn></mrow></msubsup></math></span>(sys.) and <span><math><mrow><msub><mrow><mi>γ</mi></mrow><mrow><mn>2</mn></mrow></msub><mo>=</mo><mo>−</mo><mn>2</mn><mo>.</mo><mn>71</mn><mspace></mspace><mo>±</mo><mspace></mspace><mn>0</mn><mo>.</mo><mn>01</mn></mrow></math></span>(stat.)<span><math><msubsup><mrow></mrow><mrow><mo>−</mo><mn>0</mn><mo>.</mo><mn>04</mn></mrow><mrow><mo>+</mo><mn>0</mn><mo>.</mo><mn>03</mn></mrow></msubsup></math></span>(sys.), respectively.</div></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"167 ","pages":"Article 103077"},"PeriodicalIF":4.2,"publicationDate":"2024-12-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143181561","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":"On the accretion flow and mass accretion rates/fluctuations in black hole candidate; MAXI J1535–571","authors":"Ambrose C. Eze ,&nbsp;Romanus N.C. Eze ,&nbsp;Augustine E. Chukwude ,&nbsp;Fidelis O. Madu","doi":"10.1016/j.astropartphys.2024.103076","DOIUrl":"10.1016/j.astropartphys.2024.103076","url":null,"abstract":"<div><div>MAXI J1535–571 underwent dramatic and transient outbursts accompanied by accretion flow. Hard X-radiations are produced due to thermal–and inverse–comptonization of soft photons by high-temperature electrons. The variations/fluctuations of components of the accretion flow rates and their fractional X-ray emissions/flux variability contributions at different epochs infer the spectral states. In this study, we utilized MAXI J1535–571 data observed by the three X-ray missions/detectors (<em>MAXI/GSC, NuSTAR</em>, and <em>SWIFT/BAT</em>) on the same and/or close-in epochs. Each detector's data were separately reduced and analyzed using HEASoft v6.28 and its software packages alongside the standard pipeline product software of each detector. Thereafter, the MAXI J1535–571 data were simultaneously fitted in <em>XSPEC</em> version 12.10.1f and modelled using selected analytical and phenomenological models (AP-model) to examine the photon index–N_BMC saturation effect and variations of components of the accretion flow rates. Moreover, the <em>TCAF</em> model was used on MAXI J1535–571 data to determine the correlation of components of the accretion flow rates. The <em>AP</em>– and <em>TCAF</em>–models gave a statistically acceptable fit with a reduced Chi-squared value of ≤ 1.2, and their spectral results were compared. The best-fit photon index of ∼ 2.0–2.20 affirms that MAXI J1535–571 is in its rising phase; the hard-intermediate state. The correlation of mass accretion rates suggests that their variations/fluctuations could be responsible for the dynamics and geometry of the accretion flow.</div></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"166 ","pages":"Article 103076"},"PeriodicalIF":4.2,"publicationDate":"2024-12-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143145494","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":"Towards searching for photons with energies beyond the PeV range from galactic PeVatrons","authors":"M. Niechciol,&nbsp;C. Papior,&nbsp;M. Risse","doi":"10.1016/j.astropartphys.2024.103074","DOIUrl":"10.1016/j.astropartphys.2024.103074","url":null,"abstract":"<div><div>Several gamma-ray observatories have discovered photons of cosmic origin with energies in the PeV (<span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>15</mn></mrow></msup><mspace></mspace><mi>eV</mi></mrow></math></span>) range. Photons at these energies might be produced as by-products from particle acceleration in so-called PeVatrons, which are widely assumed to be the sources of a large part of galactic cosmic rays. Based on recent measurements of these PeV <span><math><mi>γ</mi></math></span>-sources by LHAASO and HAWC, we extrapolate the energy spectra of selected sources up to the ultra-high-energy (UHE, <span><math><mrow><mo>≥</mo><mn>10</mn><mspace></mspace><mi>PeV</mi></mrow></math></span>) regime. The goal of this study is to evaluate if (and under what conditions) giant air-shower observatories, for example the Pierre Auger Observatory, could contribute to testing the UHE luminosity of PeV <span><math><mi>γ</mi></math></span>-sources. Possible propagation effects are investigated as well as the required discrimination power to distinguish photon- and hadron-initiated air showers. For present detector setups, it turns out to be challenging to achieve the required sensitivity due to the energy threshold being too high or the detection area too small. Dedicated detector concepts appear to be needed to explore the UHE frontier. Ultimately, this could provide complementary information on the sources of cosmic rays beyond the PeV regime—a key objective of current efforts in multimessenger astronomy.</div></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"166 ","pages":"Article 103074"},"PeriodicalIF":4.2,"publicationDate":"2024-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143145498","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Thin accretion disk and shadow of Kerr–Sen black hole in Einstein–Maxwell-dilaton–axion gravity","authors":"Haiyuan Feng ,&nbsp;Rong-Jia Yang ,&nbsp;Wei-Qiang Chen","doi":"10.1016/j.astropartphys.2024.103075","DOIUrl":"10.1016/j.astropartphys.2024.103075","url":null,"abstract":"<div><div>We investigate the thin disk and shadow of Kerr–Sen black hole in Einstein–Maxwell-dilaton–axion gravity. The results reveal that as the dilaton parameter <span><math><msub><mrow><mi>r</mi></mrow><mrow><mn>2</mn></mrow></msub></math></span> increase, the energy flux, the radiation temperature, the spectra luminosity, and the radiative efficiency of the disk all increase. By narrowing down the dilaton parameter range to <span><math><mrow><mn>0</mn><mo>⩽</mo><mfrac><mrow><msub><mrow><mi>r</mi></mrow><mrow><mn>2</mn></mrow></msub></mrow><mrow><mi>M</mi></mrow></mfrac><mo>⩽</mo><mn>0</mn><mo>.</mo><mn>4</mn></mrow></math></span>, we discover that in the high-frequency region, the Kerr–Sen black hole demonstrates higher energy output compared to the Kerr black hole. We also investigated the shadow of Kerr–Sen black hole in a uniform plasma environment. For fixed inclination angle, dilaton, and spin parameters, the shadow increases as the homogeneous plasma parameter <span><math><mi>k</mi></math></span> increases. Conversely, when <span><math><mi>k</mi></math></span> and <span><math><mi>a</mi></math></span> are fixed, an increase in <span><math><msub><mrow><mi>r</mi></mrow><mrow><mn>2</mn></mrow></msub></math></span> leads to a decrease in the shadow. Finally, we constrain the model parameters with observational data from M87* and Sgr A*.</div></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"166 ","pages":"Article 103075"},"PeriodicalIF":4.2,"publicationDate":"2024-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143145493","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":"Isotropization and complexity based extended Krori–Barua and Tolman IV Rastall models under the effect of electromagnetic field","authors":"Tayyab Naseer","doi":"10.1016/j.astropartphys.2024.103073","DOIUrl":"10.1016/j.astropartphys.2024.103073","url":null,"abstract":"<div><div>Three different exact solutions to the gravitational equations are formulated in this paper in the context of Rastall theory using the gravitational decoupling strategy. For doing so, the anisotropic spherical interior fluid distribution is assumed as a seed source characterized by the corresponding Lagrangian. I then modify the field equations by introducing an additional source which is gravitationally coupled with the former fluid setup. Since this approach makes the Rastall equations more complex, I use the MGD scheme to tackle this, dividing these equations into two systems. The Krori–Barua and Tolman IV spacetimes are taken into account to solve the first system, describing an initial anisotropic fluid. The metric potentials associated with these solutions contain multiple constants which are determined with the help of boundary conditions. Furthermore, I work out the solution for the second system through different well-known constraints. Afterwards, the estimated data of a compact star <span><math><mrow><mi>L</mi><mi>M</mi><mi>C</mi><mspace></mspace><mi>X</mi><mo>−</mo><mn>4</mn></mrow></math></span> is considered to explore the feasibility of the developed solutions through graphical interpretation. It is concluded that all the resulting models show physically existing profiles under the variation of certain parameters.</div></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"166 ","pages":"Article 103073"},"PeriodicalIF":4.2,"publicationDate":"2024-12-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143145496","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":"Simulating radio emission from particle cascades with CORSIKA 8","authors":"J.M. Alameddine ,&nbsp;J. Albrecht ,&nbsp;J. Ammerman-Yebra ,&nbsp;L. Arrabito ,&nbsp;A.A. Alves Jr. ,&nbsp;D. Baack ,&nbsp;A. Coleman ,&nbsp;H. Dembinski ,&nbsp;D. Elsässer ,&nbsp;R. Engel ,&nbsp;A. Faure ,&nbsp;A. Ferrari ,&nbsp;C. Gaudu ,&nbsp;C. Glaser ,&nbsp;M. Gottowik ,&nbsp;D. Heck ,&nbsp;T. Huege ,&nbsp;K.H. Kampert ,&nbsp;N. Karastathis ,&nbsp;L. Nellen ,&nbsp;R. Ulrich","doi":"10.1016/j.astropartphys.2024.103072","DOIUrl":"10.1016/j.astropartphys.2024.103072","url":null,"abstract":"<div><div>CORSIKA 8 is a new framework for simulations of particle cascades in air and dense media implemented in modern C++17, based on past experience with existing codes, in particular CORSIKA 7. The flexible and modular structure of the project allows the development of independent modules that can produce a fully customizable particle shower simulation. The radio module in particular is designed to treat the electric field calculation and its propagation through complex media to each observer location in an autonomous and flexible way. It already allows for the simultaneous simulation of the radio emission calculated with two independent time-domain formalisms, the “Endpoint formalism” as previously implemented in CoREAS and the “ZHS” algorithm as ported from ZHAireS. The design acts as the baseline interface for current and future development for the simulation of radio emission from particle showers in standard and complex scenarios, such as cross-media showers penetrating from air into ice. In this work, we present the design and implementation of the radio module in CORSIKA 8, along with validation studies and a direct comparison of the radio emission from air showers simulated with CORSIKA 8, CORSIKA 7, and ZHAireS. We also present the impact of simulation details such as the step size of simulated particle tracks on radio-emission simulations and perform a direct comparison of the “Endpoints” and “ZHS” formalisms for the same underlying air showers. Finally, we present an in-depth comparison of CORSIKA 8 and CORSIKA 7 for optimum simulation settings and discuss the relevance of observed differences in light of reconstruction efforts for the energy and mass of cosmic rays.</div></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"166 ","pages":"Article 103072"},"PeriodicalIF":4.2,"publicationDate":"2024-12-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143145499","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}