A. Baktoraz, N. Saduyev, O. Kalikulov, D. Beznosko, Y. Mukhamejanov, S. Utey, S. Shinbulatov, N. Yerezhep, A. Zhumabayev, V. Zhukov, A. Shepetov
The extensive air showers (EAS) detector system consisting of timing detection is being built for the reconstruction of the EAS axis direction using chronotron timing information. This system consists of eight scintillator-based individual detectors (100 x 100 x 1 cm) using wavelength shifting fibers for light collection ("Chronotron" installation). The goal of the project is to supplement a complex of EAS installations that is located at the elevation of 3340 m above sea level at the (Tien Shan High-altitude Scientific Station) TSHSS near the city of Almaty, Kazakhstan, with the system of detectors with fast timing. This work presents the current design, the characteristics from the simulation and the performance of the prototype.
构建了由定时检测组成的广泛风淋探测系统，利用同步加速器定时信息重建风淋轴方向。该系统由八个基于闪烁体的独立探测器(100 x 100 x 1厘米)组成，使用波长移位光纤进行光收集(“Chronotron”安装)。该项目的目标是补充位于哈萨克斯坦阿拉木图市附近(天山高海拔科学站)TSHSS海拔3340米的EAS装置综合体，配备快速计时的探测器系统。本文介绍了该系统的设计现状、仿真特点和样机性能。
{"title":"\"Chronotron\" timing detectors for EAS studies","authors":"A. Baktoraz, N. Saduyev, O. Kalikulov, D. Beznosko, Y. Mukhamejanov, S. Utey, S. Shinbulatov, N. Yerezhep, A. Zhumabayev, V. Zhukov, A. Shepetov","doi":"10.22323/1.395.0259","DOIUrl":"https://doi.org/10.22323/1.395.0259","url":null,"abstract":"The extensive air showers (EAS) detector system consisting of timing detection is being built for the reconstruction of the EAS axis direction using chronotron timing information. This system consists of eight scintillator-based individual detectors (100 x 100 x 1 cm) using wavelength shifting fibers for light collection (\"Chronotron\" installation). The goal of the project is to supplement a complex of EAS installations that is located at the elevation of 3340 m above sea level at the (Tien Shan High-altitude Scientific Station) TSHSS near the city of Almaty, Kazakhstan, with the system of detectors with fast timing. This work presents the current design, the characteristics from the simulation and the performance of the prototype.","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"128 2 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"79590936","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}
V. Lenok, O. Kopylova, D. Wochele, F. Polgart, S. Golovachev, V. Sotnikov, E. Sotnikova, P. Bezyazeekov, N. Budnev, O. Fedorov, O. Gress, O. Grishin, A. Haungs, T. Huege, Y. Kazarina, M. Kleifges, E. Korosteleva, D. Kostunin, L. Kuzmichev, V. Lenok, N. Lubsandorzhiev, S. Malakhov, T. Marshalkina, R. Monkhoev, E. Osipova, A. Pakhorukov, L. Pankov, V. Prosin, F. Schröder, D. Shipilov, A. Zagorodnikov
V. Lenok,a,∗ D. Kostunin, O. Kopylova, P. Bezyazeekov, D. Wochele, F. Polgart, S. Golovachev, V. Sotnikov and E. Sotnikova for the Tunka-Rex Collaboration (a complete list of Tunka-Rex authors can be found at the end of the proceedings) Karlsruhe Institute of Technology, Institute for Astroparticle Physics, D-76021 Karlsruhe, Germany DESY, 15738 Zeuthen, Germany Applied Physics Institute, Irkutsk State University, 664020 Irkutsk, Russia JetBrains Research, 194100 St. Petersburg, Russia Sobolev Institute of Mathematics, 630090 Novosibirsk, Russia E-mail: contact@tunkarex.info
V. Lenok,a，∗D. Kostunin, O. Kopylova, P. Bezyazeekov, D. Wochele, F. Polgart, S. Golovachev, V. Sotnikov和E. Sotnikova为Tunka-Rex合作(Tunka-Rex的完整作者列表可在会议结尾处找到)卡尔斯鲁厄理工学院，天体粒子物理研究所，D-76021卡尔斯鲁厄，德国DESY, 15738 Zeuthen，德国应用物理研究所，伊尔库茨克国立大学，664020伊尔库茨克，俄罗斯JetBrains Research, 194100圣彼得堡，俄罗斯索博列夫数学研究所，俄罗斯新西伯利亚630090 E-mail: contact@tunkarex.info
{"title":"Tunka-Rex Virtual Observatory","authors":"V. Lenok, O. Kopylova, D. Wochele, F. Polgart, S. Golovachev, V. Sotnikov, E. Sotnikova, P. Bezyazeekov, N. Budnev, O. Fedorov, O. Gress, O. Grishin, A. Haungs, T. Huege, Y. Kazarina, M. Kleifges, E. Korosteleva, D. Kostunin, L. Kuzmichev, V. Lenok, N. Lubsandorzhiev, S. Malakhov, T. Marshalkina, R. Monkhoev, E. Osipova, A. Pakhorukov, L. Pankov, V. Prosin, F. Schröder, D. Shipilov, A. Zagorodnikov","doi":"10.22323/1.395.0421","DOIUrl":"https://doi.org/10.22323/1.395.0421","url":null,"abstract":"V. Lenok,a,∗ D. Kostunin, O. Kopylova, P. Bezyazeekov, D. Wochele, F. Polgart, S. Golovachev, V. Sotnikov and E. Sotnikova for the Tunka-Rex Collaboration (a complete list of Tunka-Rex authors can be found at the end of the proceedings) Karlsruhe Institute of Technology, Institute for Astroparticle Physics, D-76021 Karlsruhe, Germany DESY, 15738 Zeuthen, Germany Applied Physics Institute, Irkutsk State University, 664020 Irkutsk, Russia JetBrains Research, 194100 St. Petersburg, Russia Sobolev Institute of Mathematics, 630090 Novosibirsk, Russia E-mail: contact@tunkarex.info","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"19 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"79394121","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. Taylor, G. Giacinti, P. Desiati, J. C. Vélez, A. Chiavassa, G. Sciascio, J. Velazquez, S. Kunwar
DESY, Platanenallee 6, 15738 Zeuthen, Germany MPIK, Saupfercheckweg 1, 69117 Heidelberg, Germany WIPAC, University of Wisconsin Madison, 222 W. Washington Ave. Madison, WI 53703, U.S.A. Dipartimento di Fisica, Università degli Studi di Torino, Torino, Italy Istituto Nazionale di Fisica Nucleare, Sezione di Roma Tor Vergata, via della Ricerca Scientifica 1, 00133 Roma, Italy 5 Institute of Physics and Mathematics, Universidad Michoacana de San Nicol as de Hidalgo, Morelia, Mexico E-mail: andrew.taylor@desy.de, Gwenael.Giacinti@mpi-hd.mpg.de
DESY, Platanenallee 6, 15738 Zeuthen，德国MPIK, Saupfercheckweg 1, 69117 Heidelberg，德国威斯康星州麦迪逊大学，222 W。华盛顿Ave .麦迪逊,53703、U。S。A .物理系,universita degli Studi di,都灵,意大利国家核物理研究所,罗马Tor Vergata科、科学研究的道路上1、00133罗马,意大利5物理研究所和服装,大学Michoacana de Morelia Nicol as德伊达尔戈(aung San suu kyi)墨西哥电子邮件:安德鲁·taylor@desy . de Gwenael Giacinti@mpi-hd mpg。德。
{"title":"Composition Sensitivity for the Cosmic Ray Anisotropy with SWGO","authors":"A. Taylor, G. Giacinti, P. Desiati, J. C. Vélez, A. Chiavassa, G. Sciascio, J. Velazquez, S. Kunwar","doi":"10.22323/1.395.0198","DOIUrl":"https://doi.org/10.22323/1.395.0198","url":null,"abstract":"DESY, Platanenallee 6, 15738 Zeuthen, Germany MPIK, Saupfercheckweg 1, 69117 Heidelberg, Germany WIPAC, University of Wisconsin Madison, 222 W. Washington Ave. Madison, WI 53703, U.S.A. Dipartimento di Fisica, Università degli Studi di Torino, Torino, Italy Istituto Nazionale di Fisica Nucleare, Sezione di Roma Tor Vergata, via della Ricerca Scientifica 1, 00133 Roma, Italy 5 Institute of Physics and Mathematics, Universidad Michoacana de San Nicol as de Hidalgo, Morelia, Mexico E-mail: andrew.taylor@desy.de, Gwenael.Giacinti@mpi-hd.mpg.de","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"27 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"73605447","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}
P. Bezyazeekov, D. Shipilov, I. Plokhikh, A. Mikhaylenko, P. Turishcheva, S. Golovachev, V. Sotnikov, E. Sotnikova, N. Budnev, O. Fedorov, O. Gress, O. Grishin, A. Haungs, T. Huege, Y. Kazarina, M. Kleifges, E. Korosteleva, D. Kostunin, L. Kuzmichev, V. Lenok, N. Lubsandorzhiev, S. Malakhov, T. Marshalkina, R. Monkhoev, E. Osipova, A. Pakhorukov, L. Pankov, V. Prosin, F. Schroder, A. Zagorodnikov
P. Bezyazeekov,a,∗ D. Shipilov, D. Kostunin, I. Plokhikh, A. Mikhaylenko, P. Turishcheva, S. Golovachev, f V. Sotnikov f and E. Sotnikova for the Tunka-Rex Collaboration (a complete list of Tunka-Rex authors can be found at the end of the proceedings) Applied Physics Institute, Irkutsk State University, 664020 Irkutsk, Russia X5 Retail Group, Moscow, 119049 Russia DESY, 15738 Zeuthen, Germany Novosibirsk State University, 630090 Novosibirsk, Russia Innopolis University, 420500 Innopolis, Russia f JetBrains Research, 194100 St. Petersburg, Russia Sobolev Institute of Mathematics, 630090 Novosibirsk, Russia E-mail: contact@tunkarex.info
P. Bezyazeekov,a .∗D. Shipilov, D. Kostunin, I. Plokhikh, a . Mikhaylenko, P. Turishcheva, S. Golovachev, f . V. Sotnikov和E. Sotnikova为Tunka-Rex合作(Tunka-Rex作者的完整列表可在会议结尾处找到)应用物理研究所，伊尔库茨克国立大学，664020伊尔库茨克，俄罗斯X5零售集团，莫斯科，119049俄罗斯DESY, 15738 zeeuthen，德国新西伯利亚国立大学，630090新西伯利亚，俄罗斯Innopolis大学，420500 Innopolis，俄罗斯JetBrains研究中心，194100圣彼得堡，俄罗斯索博列夫数学研究所，630090新西伯利亚，俄罗斯E-mail: contact@tunkarex.info
{"title":"Reconstruction of sub-threshold events of cosmic-ray radio detectors using an autoencoder","authors":"P. Bezyazeekov, D. Shipilov, I. Plokhikh, A. Mikhaylenko, P. Turishcheva, S. Golovachev, V. Sotnikov, E. Sotnikova, N. Budnev, O. Fedorov, O. Gress, O. Grishin, A. Haungs, T. Huege, Y. Kazarina, M. Kleifges, E. Korosteleva, D. Kostunin, L. Kuzmichev, V. Lenok, N. Lubsandorzhiev, S. Malakhov, T. Marshalkina, R. Monkhoev, E. Osipova, A. Pakhorukov, L. Pankov, V. Prosin, F. Schroder, A. Zagorodnikov","doi":"10.22323/1.395.0223","DOIUrl":"https://doi.org/10.22323/1.395.0223","url":null,"abstract":"P. Bezyazeekov,a,∗ D. Shipilov, D. Kostunin, I. Plokhikh, A. Mikhaylenko, P. Turishcheva, S. Golovachev, f V. Sotnikov f and E. Sotnikova for the Tunka-Rex Collaboration (a complete list of Tunka-Rex authors can be found at the end of the proceedings) Applied Physics Institute, Irkutsk State University, 664020 Irkutsk, Russia X5 Retail Group, Moscow, 119049 Russia DESY, 15738 Zeuthen, Germany Novosibirsk State University, 630090 Novosibirsk, Russia Innopolis University, 420500 Innopolis, Russia f JetBrains Research, 194100 St. Petersburg, Russia Sobolev Institute of Mathematics, 630090 Novosibirsk, Russia E-mail: contact@tunkarex.info","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"85 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"79973727","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}
P. Bezyazeekov, O. Fedorov, Y. Kazarina, O. Kopylova, D. Kostunin, V. Lenok, S. Malakhov
Air-shower radio arrays operate in low signal-to-noise ratio conditions, which complicates the autonomous measurement of air-shower signals without using an external trigger from optical or scintillator detectors. A simple threshold trigger for radio detector can be efficiently applied onlyin radio-quiet conditions, because for other cases this trigger detects a high fraction of noise pulses. In the present work, we study aspects of independent air-shower detection by dense antenna clusters with a complex real-time trigger system. For choosing the optimal procedures for the real-time analysis, we study the dependence between trigger efficiency, count rate, detector hardware and geometry. For this study, we develop a framework for testing various methods of signal detection and noise filtration for arrays with various specifications and the hardware implementation of these methods based on field programmable gate arrays. The framework provides flexible settings for the management of station-level and cluster-level steps of detecting the signal, optimized for the hardware implementation for real-time processing. It includes data-processing tools for the initialconfiguration and tests on pre-recorded data, tools for configuring the trigger architecture andtools for preliminary estimates of the trigger efficiency at given thresholds of cosmic-ray energyand air-shower pulse amplitude. We show examples of the trigger pipeline developed with this framework and discuss the results of tests on simulated data.
{"title":"Efficiency estimation of self-triggered antenna clusters for air-shower detection","authors":"P. Bezyazeekov, O. Fedorov, Y. Kazarina, O. Kopylova, D. Kostunin, V. Lenok, S. Malakhov","doi":"10.22323/1.395.0273","DOIUrl":"https://doi.org/10.22323/1.395.0273","url":null,"abstract":"Air-shower radio arrays operate in low signal-to-noise ratio conditions, which complicates the autonomous measurement of air-shower signals without using an external trigger from optical or scintillator detectors. A simple threshold trigger for radio detector can be efficiently applied onlyin radio-quiet conditions, because for other cases this trigger detects a high fraction of noise pulses. In the present work, we study aspects of independent air-shower detection by dense antenna clusters with a complex real-time trigger system. For choosing the optimal procedures for the real-time analysis, we study the dependence between trigger efficiency, count rate, detector hardware and geometry. For this study, we develop a framework for testing various methods of signal detection and noise filtration for arrays with various specifications and the hardware implementation of these methods based on field programmable gate arrays. The framework provides flexible settings for the management of station-level and cluster-level steps of detecting the signal, optimized for the hardware implementation for real-time processing. It includes data-processing tools for the initialconfiguration and tests on pre-recorded data, tools for configuring the trigger architecture andtools for preliminary estimates of the trigger efficiency at given thresholds of cosmic-ray energyand air-shower pulse amplitude. We show examples of the trigger pipeline developed with this framework and discuss the results of tests on simulated data.","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"11 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"81998712","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}
K. Sakai, K. Abe, H. Fuke, S. Haino, T. Hams, M. Hasegawa, K. Kim, M. Lee, Y. Makida, J. Mitchell, J. Nishimura, M. Nozaki, R. Orito, J. Ormes, N. Picot-Clemente, M. Sasaki, E. Seo, R.E. Streltmatter, N. Thakur, A. Yamamoto, T. Yoshida, K. Yoshimura
High precision cosmic-ray low energy antiproton fluxes reported by BESS-Polar, PAMELA and AMS-02 are consistent with secondary production from interactions of primary cosmic rays with the interstellar medium. This severely constrains the possibility of antiprotons of primary origin such as annihilation or decay of supersymmetric dark matter or evaporation of primordial
{"title":"New result of Antideuteron search in BESS-Polar II","authors":"K. Sakai, K. Abe, H. Fuke, S. Haino, T. Hams, M. Hasegawa, K. Kim, M. Lee, Y. Makida, J. Mitchell, J. Nishimura, M. Nozaki, R. Orito, J. Ormes, N. Picot-Clemente, M. Sasaki, E. Seo, R.E. Streltmatter, N. Thakur, A. Yamamoto, T. Yoshida, K. Yoshimura","doi":"10.22323/1.395.0123","DOIUrl":"https://doi.org/10.22323/1.395.0123","url":null,"abstract":"High precision cosmic-ray low energy antiproton fluxes reported by BESS-Polar, PAMELA and AMS-02 are consistent with secondary production from interactions of primary cosmic rays with the interstellar medium. This severely constrains the possibility of antiprotons of primary origin such as annihilation or decay of supersymmetric dark matter or evaporation of primordial","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"8 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"85964207","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}
TIGERISS is an Ultra-Heavy Galactic Cosmic Ray (UHGCR) detector to be proposed to the NASA Astrophysics Pioneers Program capable of measuring the abundance relative to 26Fe of every element from 5B to 82Pb. It is evolved from the LDB TIGER and SuperTIGER balloon instruments and the Heavy-Nuclei Explorer SMEX, and compared to its predecessors, TIGERISS will have a greatly improved capability to definitively identify UHGCR nuclei. This has been demonstrated in component accelerator tests at CERN, including silicon strip detectors in place of scintillators. The geometry factor for TIGERISS is estimated to be from 1.1 to 1.7 m2 sr depending on the ISS attachment point, compared to 0.6 m2 sr for TIGER. Within one-year TIGERISS would observe ∼27 56Ba nuclei, a 20% statistically significant result comparable to the current SuperTIGER data set. Not requiring corrections for atmospheric interactions and scintillator saturation effects the TIGERISS results would be cleaner, and they would also make preliminary measurements to higher charges that will test models for cosmic-ray origins and acceleration. TIGERISS will measure UHGCR nuclei resulting from neutron-capture nucleosynthesis in heavy stars, supernovae, and binary neutron-star mergers and will probe the relative contribution of r-process elements to the cosmic rays.
{"title":"The Trans-Iron Galactic Element Recorder for the International Space Station (TIGERISS)","authors":"B. Rauch, N. Walsh, W. Zober","doi":"10.22323/1.395.0087","DOIUrl":"https://doi.org/10.22323/1.395.0087","url":null,"abstract":"TIGERISS is an Ultra-Heavy Galactic Cosmic Ray (UHGCR) detector to be proposed to the NASA Astrophysics Pioneers Program capable of measuring the abundance relative to 26Fe of every element from 5B to 82Pb. It is evolved from the LDB TIGER and SuperTIGER balloon instruments and the Heavy-Nuclei Explorer SMEX, and compared to its predecessors, TIGERISS will have a greatly improved capability to definitively identify UHGCR nuclei. This has been demonstrated in component accelerator tests at CERN, including silicon strip detectors in place of scintillators. The geometry factor for TIGERISS is estimated to be from 1.1 to 1.7 m2 sr depending on the ISS attachment point, compared to 0.6 m2 sr for TIGER. Within one-year TIGERISS would observe ∼27 56Ba nuclei, a 20% statistically significant result comparable to the current SuperTIGER data set. Not requiring corrections for atmospheric interactions and scintillator saturation effects the TIGERISS results would be cleaner, and they would also make preliminary measurements to higher charges that will test models for cosmic-ray origins and acceleration. TIGERISS will measure UHGCR nuclei resulting from neutron-capture nucleosynthesis in heavy stars, supernovae, and binary neutron-star mergers and will probe the relative contribution of r-process elements to the cosmic rays.","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"20 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"75031091","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}
ã Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). https://pos.sissa.it/ Bursty betatron acceleration of electrons at nonstationary quasi-perpendicular shocks Fumiko Otsukaa*, Shuichi Matsukiyoa, Mitsuo Oka b a Kyushu University, 6-1 Kasuga-Koen, Kasuga, Fukuoka, Japan b Space Sciences Laboratory, University of California, Berkeley, USA E-mail: otsuka@esst.kyushu-u.ac.jp
ã根据知识共享署名-非商业-非衍生品4.0国际许可协议(CC by - nc - nd 4.0)的条款，版权归作者所有。https://pos.sissa.it/非平稳准垂直冲击下电子的瞬态电子加速器加速Fumiko Otsukaa*， Shuichi Matsukiyoa, Mitsuo Oka b a九州大学，日本福冈Kasuga- koen 6-1 b美国加州大学伯克利分校空间科学实验室E-mail: otsuka@esst.kyushu-u.ac.jp
{"title":"Bursty betatron acceleration of electrons at nonstationary quasi-perpendicular shocks","authors":"F. Otsuka, S. Matsukiyo, M. Oka","doi":"10.22323/1.395.1344","DOIUrl":"https://doi.org/10.22323/1.395.1344","url":null,"abstract":"ã Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). https://pos.sissa.it/ Bursty betatron acceleration of electrons at nonstationary quasi-perpendicular shocks Fumiko Otsukaa*, Shuichi Matsukiyoa, Mitsuo Oka b a Kyushu University, 6-1 Kasuga-Koen, Kasuga, Fukuoka, Japan b Space Sciences Laboratory, University of California, Berkeley, USA E-mail: otsuka@esst.kyushu-u.ac.jp","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"25 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"82844094","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. Shiomi, Hiroki Nakada, Y. Katayose, M. Ohnishi, T. Sako, K. Hibino
Several spread TeV gamma-ray sources have been observed in the galaxy by several experimental groups. Experiments with high angular resolution that can detect gamma rays in the 100 TeV region will help study acceleration mechanisms of those gamma-ray sources. In recent years, three groups using extensive air shower arrays have reported detecting gamma rays in the 100 TeV region from astronomical objects in the galaxy. In extensive air shower experiments, an arrival direction of a cosmic ray is determined by estimating a shape of a front surface of an air shower based on a detected secondary particle density distribution and detection time. The density of secondary gamma rays of an air shower is several times that of secondary electrons and positrons in an air shower and the difference increases as the distance from the shower axis increases. Therefore, secondary gamma-ray measurements are key to determining the arrival direction of the shower. We report the results of investigating the effect of secondary gamma rays on the time determination accuracy of an air shower front using a Monte Carlo simulation. We also report the results of examining different detector structures to improve the time resolution using a water Cherenkov detector, which has high detection efficiency for secondary gamma rays.
{"title":"Study of water Cherenkov detector to determine air shower arrival directions with accuracy","authors":"A. Shiomi, Hiroki Nakada, Y. Katayose, M. Ohnishi, T. Sako, K. Hibino","doi":"10.22323/1.395.0732","DOIUrl":"https://doi.org/10.22323/1.395.0732","url":null,"abstract":"Several spread TeV gamma-ray sources have been observed in the galaxy by several experimental groups. Experiments with high angular resolution that can detect gamma rays in the 100 TeV region will help study acceleration mechanisms of those gamma-ray sources. In recent years, three groups using extensive air shower arrays have reported detecting gamma rays in the 100 TeV region from astronomical objects in the galaxy. In extensive air shower experiments, an arrival direction of a cosmic ray is determined by estimating a shape of a front surface of an air shower based on a detected secondary particle density distribution and detection time. The density of secondary gamma rays of an air shower is several times that of secondary electrons and positrons in an air shower and the difference increases as the distance from the shower axis increases. Therefore, secondary gamma-ray measurements are key to determining the arrival direction of the shower. We report the results of investigating the effect of secondary gamma rays on the time determination accuracy of an air shower front using a Monte Carlo simulation. We also report the results of examining different detector structures to improve the time resolution using a water Cherenkov detector, which has high detection efficiency for secondary gamma rays.","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"74 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"73536057","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}
The SuperTIGER (Super Trans-Iron Galactic Element Recorder) balloon-borne ultra-heavy galactic cosmic-ray (UHGCR) detector has flown twice in the stratosphere over Antarctica at altitudes up to ∼ 130,000 ft. Corrections for propagating through the last ∼ 0.5% of the atmosphere are based on those developed for the preceding TIGER instrument. Changes due to nuclear interactions are determined by finding top of the atmosphere (TOA) elemental abundances that yield those measured in the instrument after solving networks of equations for all elements with partial and total charge changing cross sections stepping through fine slabs of material. Varying rates of energy loss in the atmosphere for different elements yield different TOA minimum energies for the acrylic Cherenkov detector threshold ( ∼ 350 MeV/nuc). TOA abundances corrected for nuclear interactions for each element are scaled with the fraction of the integral energy spectrum for its TOA minimum energy, using the iron spectrum for the UHGCR. Statistical uncertainties are derived at the TOA by shifting the abundance of each element individually up and down by the measured uncertainty in the instrument and calculating the TOA abundance of that element. Systematic uncertainties previously were estimated by simultaneously shifting the partial and then the total cross sections for all elements up and down by their uncertainties and finding TOA abundances compared to the nominal values. Here we present a Monte Carlo study of the systematic impact of simultaneously randomly varying atmospheric propagation parameters over many trials to find the normal range of variation in the resulting TOA element abundances. Total
{"title":"SuperTIGER Ultra-Heavy Galactic Cosmic Ray Atmospheric Propagation Corrections and Uncertainty Analysis","authors":"B. Rauch, N. Walsh, W. Zober","doi":"10.22323/1.395.0089","DOIUrl":"https://doi.org/10.22323/1.395.0089","url":null,"abstract":"The SuperTIGER (Super Trans-Iron Galactic Element Recorder) balloon-borne ultra-heavy galactic cosmic-ray (UHGCR) detector has flown twice in the stratosphere over Antarctica at altitudes up to ∼ 130,000 ft. Corrections for propagating through the last ∼ 0.5% of the atmosphere are based on those developed for the preceding TIGER instrument. Changes due to nuclear interactions are determined by finding top of the atmosphere (TOA) elemental abundances that yield those measured in the instrument after solving networks of equations for all elements with partial and total charge changing cross sections stepping through fine slabs of material. Varying rates of energy loss in the atmosphere for different elements yield different TOA minimum energies for the acrylic Cherenkov detector threshold ( ∼ 350 MeV/nuc). TOA abundances corrected for nuclear interactions for each element are scaled with the fraction of the integral energy spectrum for its TOA minimum energy, using the iron spectrum for the UHGCR. Statistical uncertainties are derived at the TOA by shifting the abundance of each element individually up and down by the measured uncertainty in the instrument and calculating the TOA abundance of that element. Systematic uncertainties previously were estimated by simultaneously shifting the partial and then the total cross sections for all elements up and down by their uncertainties and finding TOA abundances compared to the nominal values. Here we present a Monte Carlo study of the systematic impact of simultaneously randomly varying atmospheric propagation parameters over many trials to find the normal range of variation in the resulting TOA element abundances. Total","PeriodicalId":20473,"journal":{"name":"Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)","volume":"39 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2021-08-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"82546387","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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