{"title":"Properties of Cosmic Beryllium Isotopes","authors":"Francesco Dimiccoli","doi":"10.22323/1.423.0068","DOIUrl":"https://doi.org/10.22323/1.423.0068","url":null,"abstract":"","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"23 6","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139271511","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
B. Pont, P. Abreu, M. Aglietta, I. Allekotte, K. Almeida Cheminant, A. Almela, J. Alvarez-Muñiz, J. Ammerman Yebra, G. A. Anastasi, L. Anchordoqui, B. Andrada, S. Andringa, C. Aramo, P. R. Araújo Ferreira, E. Arnone, J. C. Arteaga Velázquez, Hernán Asorey, P. Assis, G. Avila, E. Avocone, A. Badescu, A. Bakalová, A. Bălăceanu, F. Barbato, J. Bellido, C. Bérat, M. Bertaina, G. Bhatta, P. Biermann, V. Binet, K. Bismark, T. Bister, J. Biteau, J. Blažek, C. Bleve, J. Blümer, M. Boháčová, D. Boncioli, C. Bonifazi, L. Bonneau Arbeletche, N. Borodai, J. Brack, T. Bretz, P. G. Brichetto Orchera, F. Briechle, P. Buchholz, A. Bueno, S. Buitink, M. Buscemi, M. Büsken, A. Bwembya, K. Caballero-Mora, L. Caccianiga, I. Caracas, R. Caruso, A. Castellina, F. Catalani, G. Cataldi, L. Cazon, M. Cerda, J. Chinellato, J. Chudoba, L. Chytka, R. Clay, A. Cobos Cerutti, R. Colalillo, Alan Coleman, M. Coluccia, R. Conceição, A. Condorelli, G. Consolati, F. Contreras, F. Convenga, D. Correia dos Santos, C. Covault, M. Cristinziani
The Auger Engineering Radio Array (AERA), as part of the Pierre Auger Observatory, is an array of 153 radio antennas spanning an area of 17 km 2 , currently the largest of its kind, that probes the nature of ultra-high-energy cosmic rays at energies around the transition from Galactic to extra-galactic origin. It measures the MHz radio emission of extensive air showers produced by cosmic rays hitting our atmosphere. We show the recent work by AERA, such as the measurement of the muon content of inclined air showers and the stability of the measured radio signal over almost a decade, as measured with the Galactic radio background. In particular, we highlight the measurements of the depths of the shower maxima 𝑋 max , which we use to make inferences about the mass composition of cosmic rays. We reconstruct 𝑋 max by comparing the measured radio footprint on the ground to an ensemble of footprints from Monte-Carlo CORSIKA/CoREAS air shower simulations. We compare our 𝑋 max reconstruction with fluorescence 𝑋 max measurements on a per-event basis, a setup unique to the Pierre Auger Observatory, and show the methods to be fully compatible. We determine the resolution of our method as a function of energy and reach a precision better than 15 g cm − 2 at the highest energies. With a bias-free set of around 600 showers, we find agreement with the Auger fluorescence measurements at energies between 10 17 . 5 to 10 18 . 8 eV.
作为皮埃尔·奥格天文台的一部分，奥格工程无线电阵列(AERA)是一个由153个无线电天线组成的阵列，横跨17平方公里的面积，是目前最大的无线电天线阵列，用于探测从银河系到星系外起源过渡能量的超高能宇宙射线的本质。它测量宇宙射线撞击大气层产生的大量空气阵雨的兆赫无线电发射。我们展示了AERA最近的工作，例如测量倾斜空气阵雨的介子含量和近十年来测量的无线电信号的稳定性，正如用银河系射电背景测量的那样。特别地，我们强调了淋浴的深度测量最大值𝑋max，我们用它来推断宇宙射线的质量组成。我们通过将地面上测量的无线电足迹与蒙特卡洛CORSIKA/CoREAS空气淋点模拟的足迹集合进行比较来重建𝑋max。我们比较了我们的𝑋最大重建与荧光𝑋最大测量在每个事件的基础上，一个独特的设置皮埃尔·奥格天文台，并显示方法是完全兼容的。我们将方法的分辨率确定为能量的函数，并在最高能量下达到优于15 g cm−2的精度。在无偏置的大约600个阵雨中，我们发现在10 - 17之间的能量与俄歇荧光测量值一致。5 ~ 10 18。8 eV。
{"title":"Mass Composition and More: Results from the Auger Engineering Radio Array","authors":"B. Pont, P. Abreu, M. Aglietta, I. Allekotte, K. Almeida Cheminant, A. Almela, J. Alvarez-Muñiz, J. Ammerman Yebra, G. A. Anastasi, L. Anchordoqui, B. Andrada, S. Andringa, C. Aramo, P. R. Araújo Ferreira, E. Arnone, J. C. Arteaga Velázquez, Hernán Asorey, P. Assis, G. Avila, E. Avocone, A. Badescu, A. Bakalová, A. Bălăceanu, F. Barbato, J. Bellido, C. Bérat, M. Bertaina, G. Bhatta, P. Biermann, V. Binet, K. Bismark, T. Bister, J. Biteau, J. Blažek, C. Bleve, J. Blümer, M. Boháčová, D. Boncioli, C. Bonifazi, L. Bonneau Arbeletche, N. Borodai, J. Brack, T. Bretz, P. G. Brichetto Orchera, F. Briechle, P. Buchholz, A. Bueno, S. Buitink, M. Buscemi, M. Büsken, A. Bwembya, K. Caballero-Mora, L. Caccianiga, I. Caracas, R. Caruso, A. Castellina, F. Catalani, G. Cataldi, L. Cazon, M. Cerda, J. Chinellato, J. Chudoba, L. Chytka, R. Clay, A. Cobos Cerutti, R. Colalillo, Alan Coleman, M. Coluccia, R. Conceição, A. Condorelli, G. Consolati, F. Contreras, F. Convenga, D. Correia dos Santos, C. Covault, M. Cristinziani","doi":"10.22323/1.423.0093","DOIUrl":"https://doi.org/10.22323/1.423.0093","url":null,"abstract":"The Auger Engineering Radio Array (AERA), as part of the Pierre Auger Observatory, is an array of 153 radio antennas spanning an area of 17 km 2 , currently the largest of its kind, that probes the nature of ultra-high-energy cosmic rays at energies around the transition from Galactic to extra-galactic origin. It measures the MHz radio emission of extensive air showers produced by cosmic rays hitting our atmosphere. We show the recent work by AERA, such as the measurement of the muon content of inclined air showers and the stability of the measured radio signal over almost a decade, as measured with the Galactic radio background. In particular, we highlight the measurements of the depths of the shower maxima 𝑋 max , which we use to make inferences about the mass composition of cosmic rays. We reconstruct 𝑋 max by comparing the measured radio footprint on the ground to an ensemble of footprints from Monte-Carlo CORSIKA/CoREAS air shower simulations. We compare our 𝑋 max reconstruction with fluorescence 𝑋 max measurements on a per-event basis, a setup unique to the Pierre Auger Observatory, and show the methods to be fully compatible. We determine the resolution of our method as a function of energy and reach a precision better than 15 g cm − 2 at the highest energies. With a bias-free set of around 600 showers, we find agreement with the Auger fluorescence measurements at energies between 10 17 . 5 to 10 18 . 8 eV.","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"336 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"121249987","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Status and prospects of the Auger Radio Detector","authors":"J. Hörandel","doi":"10.22323/1.423.0095","DOIUrl":"https://doi.org/10.22323/1.423.0095","url":null,"abstract":"","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"15 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-07-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"124350805","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"The 27th European Cosmic Ray Symposium – General remarks","authors":"J. Hörandel","doi":"10.22323/1.423.0001","DOIUrl":"https://doi.org/10.22323/1.423.0001","url":null,"abstract":"","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"10 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-06-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"134107833","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
We report the properties of cosmic ray nuclei from protons to nickel (Z=1–14, 16, 26, and 28) in the rigidity range from 2 GV to 3 TV collected by the Alpha Magnetic Spectrometer on the International Space Station from May 19, 2011 to May 6, 2021. We found that the primary cosmic rays He-C-O-Fe-Ni, and Ne-Mg-Si-S belong to two different classes of cosmic rays. We also found that the secondary cosmic rays Li-Be-B and F belong to another two different classes of cosmic rays.The rigidity dependences of the secondary cosmic rays and the primary cosmic rays are distinctly different. In particular, above ∼ 200 GV the secondary cosmic rays harden twice as much as the primary cosmic rays. The third group of cosmic rays N, Na, and Al can be described as linear combinations of primary (O, Si) and secondary (B, F) cosmic rays. Compared with O and Si, the primary cosmic rays C, Ne, Mg, and S were found to have secondary component, similar to N, Na, and Al. As a result, the C/O, N/O, Ne/Si, Na/Si, Al/Si, Mg/Si, and S/Si abundance ratios at the source are directly determined independent of cosmic ray propagation. Finally, we found that the lightest and most abundant primary proton cosmic rays have two components, the first being with the same rigidity dependence as He-C-O-Fe-Ni and the second with rigidity spectral index softer than the first one by Δ 𝑝 / 𝐻𝑒 = 0 . 30 ± 0 . 01.
{"title":"Unique Properties of Cosmic Rays: Results from the Alpha Magnetic spectrometer","authors":"V. Choutko, Qi Yan","doi":"10.22323/1.423.0012","DOIUrl":"https://doi.org/10.22323/1.423.0012","url":null,"abstract":"We report the properties of cosmic ray nuclei from protons to nickel (Z=1–14, 16, 26, and 28) in the rigidity range from 2 GV to 3 TV collected by the Alpha Magnetic Spectrometer on the International Space Station from May 19, 2011 to May 6, 2021. We found that the primary cosmic rays He-C-O-Fe-Ni, and Ne-Mg-Si-S belong to two different classes of cosmic rays. We also found that the secondary cosmic rays Li-Be-B and F belong to another two different classes of cosmic rays.The rigidity dependences of the secondary cosmic rays and the primary cosmic rays are distinctly different. In particular, above ∼ 200 GV the secondary cosmic rays harden twice as much as the primary cosmic rays. The third group of cosmic rays N, Na, and Al can be described as linear combinations of primary (O, Si) and secondary (B, F) cosmic rays. Compared with O and Si, the primary cosmic rays C, Ne, Mg, and S were found to have secondary component, similar to N, Na, and Al. As a result, the C/O, N/O, Ne/Si, Na/Si, Al/Si, Mg/Si, and S/Si abundance ratios at the source are directly determined independent of cosmic ray propagation. Finally, we found that the lightest and most abundant primary proton cosmic rays have two components, the first being with the same rigidity dependence as He-C-O-Fe-Ni and the second with rigidity spectral index softer than the first one by Δ 𝑝 / 𝐻𝑒 = 0 . 30 ± 0 . 01.","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"149 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-06-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"116426610","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
A. Lenni, M. Boezio, R. Munini, N. Marcelli, M. Potgieter, D. Ngobeni, O. Adriani, G. Barbarino, G. Bazilevskaya, R. Bellotti, É. Bogomolov, M. Bongi, V. Bonvicini, A. Bruno, F. Cafagna, D. Campana, P. Carlson, M. Casolino, G. Castellini, C. De Santis, A. M. Galper, S. Koldashov, S. Koldobskiy, A. Kvashnin, A. Leonov, V. Malakhov, L. Marcelli, M. Martucci, A. Mayorov, W. Menn, M. Mergé, Vladimir V. Mikhailov, E. Mocchiutti, A. Monaco, N. Mori, G. Osteria, B. Panico, P. Papini, M. Pearce, P. Picozza, M. Ricci, S. Ricciarini, M. Simon, A. Sotgiu, R. Sparvoli, P. Spillantini, Y. Stozhkov, A. Vacchi, E. Vannuccini, G. I. Vasilyev, S. Voronov, Y. Yurkin, G. Zampa, N. Zampa
{"title":"Studies of cosmic-ray solar modulation with the PAMELA experiment","authors":"A. Lenni, M. Boezio, R. Munini, N. Marcelli, M. Potgieter, D. Ngobeni, O. Adriani, G. Barbarino, G. Bazilevskaya, R. Bellotti, É. Bogomolov, M. Bongi, V. Bonvicini, A. Bruno, F. Cafagna, D. Campana, P. Carlson, M. Casolino, G. Castellini, C. De Santis, A. M. Galper, S. Koldashov, S. Koldobskiy, A. Kvashnin, A. Leonov, V. Malakhov, L. Marcelli, M. Martucci, A. Mayorov, W. Menn, M. Mergé, Vladimir V. Mikhailov, E. Mocchiutti, A. Monaco, N. Mori, G. Osteria, B. Panico, P. Papini, M. Pearce, P. Picozza, M. Ricci, S. Ricciarini, M. Simon, A. Sotgiu, R. Sparvoli, P. Spillantini, Y. Stozhkov, A. Vacchi, E. Vannuccini, G. I. Vasilyev, S. Voronov, Y. Yurkin, G. Zampa, N. Zampa","doi":"10.22323/1.423.0044","DOIUrl":"https://doi.org/10.22323/1.423.0044","url":null,"abstract":"","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"15 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-03-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"125793090","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Extreme Solar Energetic Proton Events","authors":"E. Cliver","doi":"10.22323/1.423.0004","DOIUrl":"https://doi.org/10.22323/1.423.0004","url":null,"abstract":"","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"1 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-03-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"129616589","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Mateusz A. Ogrodnik, M. Hanasz, D. Wóltański, A. Gawryszczak
Galactic outflows and extended non-thermal emission due to Comic Ray (CR) electrons have been observed in many edge-on galaxies in the radio range of electromagnetic radiation, allowing us to estimate the strength and vertical structure of the galactic magnetic field. We construct a global model of NGC891 based on the observational characteristics of this galaxy. We assume that on large scales, the dynamics of the magnetized ISM is driven by Cosmic Rays. We apply the coarse-grained momentum finite volume (CGMV), for solving the Fokker–Planck CR transport equation for CR electrons in ”Cosmic Ray Energy SPectrum” (CRESP) module of PIERNIK MHD code to model CR propagation in this galaxy. The overall propagation of cosmic rays is described by the Fokker-Planck equation. The numerical model exhibits magnetic field amplification by CR-driven dynamo. We perform a parameter study of the system by varying the injection spectrum slope, the magnitude and momentum dependence of the CR electron diffusion coefficients and SFR. We take into account the advection, diffusion, and adiabatic changes as well as synchrotron and inverse-Compton losses. The spectrum of synchrotron radiation, polarization maps and spectral index maps reproduce the observed structures of the real edge-on galaxy very well. Comparison of different models suggests harder CR 𝑒 − injection spectra, higher conversion ratios of SN → CR energies (of 10–20%) and diffusion coefficients ∼ 9 × 10 28 cm 2 s − 1 .
在电磁辐射的射电范围内，在许多边缘星系中观测到由Comic Ray (CR)电子引起的星系外流和扩展的非热辐射，使我们能够估计星系磁场的强度和垂直结构。基于NGC891的观测特征，我们构建了该星系的全球模型。我们假设在大尺度上，被磁化的ISM的动力学是由宇宙射线驱动的。我们应用粗粒度动量有限体积(CGMV)来求解PIERNIK MHD代码“宇宙射线能谱”(CRESP)模块中CR电子的Fokker-Planck CR输运方程，以模拟CR在该星系中的传播。宇宙射线的整体传播由福克-普朗克方程描述。数值模型显示了cr驱动发电机对磁场的放大。我们通过改变注入光谱斜率，CR电子扩散系数和SFR的大小和动量依赖性来对系统进行参数研究。我们考虑了平流、扩散和绝热变化以及同步加速器和逆康普顿损失。同步辐射光谱、极化图和光谱指数图很好地再现了观测到的真实边缘星系的结构。不同模型的比较表明，CR𝑒−注入光谱较硬，SN→CR能量的转化率较高(10 - 20%)，扩散系数为~ 9 × 10 28 cm 2 s−1。
{"title":"Modeling CR electron propagation with PIERNIK & CRESP: simulations vs. observational data of NGC891","authors":"Mateusz A. Ogrodnik, M. Hanasz, D. Wóltański, A. Gawryszczak","doi":"10.22323/1.423.0131","DOIUrl":"https://doi.org/10.22323/1.423.0131","url":null,"abstract":"Galactic outflows and extended non-thermal emission due to Comic Ray (CR) electrons have been observed in many edge-on galaxies in the radio range of electromagnetic radiation, allowing us to estimate the strength and vertical structure of the galactic magnetic field. We construct a global model of NGC891 based on the observational characteristics of this galaxy. We assume that on large scales, the dynamics of the magnetized ISM is driven by Cosmic Rays. We apply the coarse-grained momentum finite volume (CGMV), for solving the Fokker–Planck CR transport equation for CR electrons in ”Cosmic Ray Energy SPectrum” (CRESP) module of PIERNIK MHD code to model CR propagation in this galaxy. The overall propagation of cosmic rays is described by the Fokker-Planck equation. The numerical model exhibits magnetic field amplification by CR-driven dynamo. We perform a parameter study of the system by varying the injection spectrum slope, the magnitude and momentum dependence of the CR electron diffusion coefficients and SFR. We take into account the advection, diffusion, and adiabatic changes as well as synchrotron and inverse-Compton losses. The spectrum of synchrotron radiation, polarization maps and spectral index maps reproduce the observed structures of the real edge-on galaxy very well. Comparison of different models suggests harder CR 𝑒 − injection spectra, higher conversion ratios of SN → CR energies (of 10–20%) and diffusion coefficients ∼ 9 × 10 28 cm 2 s − 1 .","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"20 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-03-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"132411013","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Hadronic Interactions at Ultra-High Energies with Extensive Air Showers","authors":"L. Cazon","doi":"10.22323/1.423.0011","DOIUrl":"https://doi.org/10.22323/1.423.0011","url":null,"abstract":"","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"1 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-03-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"128584994","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"R&D and production of the scintillation detectors for the IceCube Surface Array Enhancement","authors":"S. Shefali","doi":"10.22323/1.423.0141","DOIUrl":"https://doi.org/10.22323/1.423.0141","url":null,"abstract":"","PeriodicalId":375543,"journal":{"name":"Proceedings of 27th European Cosmic Ray Symposium — PoS(ECRS)","volume":"49 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-03-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"132935732","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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