Pub Date : 2023-09-28DOI: 10.21468/scipostphysproc.13.001
S. Miyake, T. Koi, Yasushi Muraki, Y. Matsubara, S. Masuda, P. Miranda, T. Naito, E. Ortiz, A. Oshima, T. Sakai, T. Sako, S. Shibata, H. Takamaru, M. Tokumaru, J. F. Valdés-Galicia
In association with a large solar flare on November 7, 2004, the solar neutron detectors located at Mt. Chacaltaya (5,250 m) in Bolivia and Mt. Sierra Negra (4,600 m) in Mexico recorded very interesting events. In order to explain these events, we have performed a calculation solving the equation of motion of anti-protons inside the magnetosphere. Based on these results, the Mt. Chacaltaya event may be explained by the detection of solar neutrons, while the Mt. Sierra Negra event may be explained by the first detection of very high energy solar neutron decay protons (SNDPs) around 6 GeV.
{"title":"Proton penetration efficiency over a high altitude observatory in Mexico","authors":"S. Miyake, T. Koi, Yasushi Muraki, Y. Matsubara, S. Masuda, P. Miranda, T. Naito, E. Ortiz, A. Oshima, T. Sakai, T. Sako, S. Shibata, H. Takamaru, M. Tokumaru, J. F. Valdés-Galicia","doi":"10.21468/scipostphysproc.13.001","DOIUrl":"https://doi.org/10.21468/scipostphysproc.13.001","url":null,"abstract":"In association with a large solar flare on November 7, 2004, the solar neutron detectors located at Mt. Chacaltaya (5,250 m) in Bolivia and Mt. Sierra Negra (4,600 m) in Mexico recorded very interesting events. In order to explain these events, we have performed a calculation solving the equation of motion of anti-protons inside the magnetosphere. Based on these results, the Mt. Chacaltaya event may be explained by the detection of solar neutrons, while the Mt. Sierra Negra event may be explained by the first detection of very high energy solar neutron decay protons (SNDPs) around 6 GeV.","PeriodicalId":355998,"journal":{"name":"SciPost Physics Proceedings","volume":"17 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135345062","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}
Pub Date : 2023-09-28DOI: 10.21468/scipostphysproc.13.018
Ken Ohashi, Hiroaki Menjo, Takashi Sako, Yoshitaka Itow
Mass composition is important for understanding the origin of ultra-high-energy cosmic rays. However, interpretation of mass composition from air shower experiments is challenging, owing to significant uncertainty in hadronic interaction models adopted in air shower simulation. A particular source of uncertainty is diffractive dissociation, as its measurements in accelerator experiments demonstrated significant systematic uncertainty. In this research, we estimate the uncertainty in langle X_{max}rangle 〈Xmax⟩ from the uncertainty of the measurement of diffractive dissociation by the ALICE experiment. The maximum uncertainty size of the entire air shower was estimated to be ^{+4.0}_{-5.6} mathrm{g/cm^2} −5.6+4.0g/cm2 for air showers induced by 10^{17} 1017 ~eV proton, which is not negligible in the uncertainty of langle X_{max}rangle 〈Xmax⟩ predictions.
{"title":"Uncertainty in mean $X_{rm max}$ from diffractive dissociation estimated using measurements of accelerator experiments","authors":"Ken Ohashi, Hiroaki Menjo, Takashi Sako, Yoshitaka Itow","doi":"10.21468/scipostphysproc.13.018","DOIUrl":"https://doi.org/10.21468/scipostphysproc.13.018","url":null,"abstract":"Mass composition is important for understanding the origin of ultra-high-energy cosmic rays. However, interpretation of mass composition from air shower experiments is challenging, owing to significant uncertainty in hadronic interaction models adopted in air shower simulation. A particular source of uncertainty is diffractive dissociation, as its measurements in accelerator experiments demonstrated significant systematic uncertainty. In this research, we estimate the uncertainty in langle X_{max}rangle <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:mrow><mml:mo stretchy=\"false\" form=\"prefix\">〈</mml:mo><mml:msub><mml:mi>X</mml:mi><mml:mrow><mml:mi>m</mml:mi><mml:mi>a</mml:mi><mml:mi>x</mml:mi></mml:mrow></mml:msub><mml:mo stretchy=\"false\" form=\"postfix\">⟩</mml:mo></mml:mrow></mml:math> from the uncertainty of the measurement of diffractive dissociation by the ALICE experiment. The maximum uncertainty size of the entire air shower was estimated to be ^{+4.0}_{-5.6} mathrm{g/cm^2} <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:mrow><mml:msubsup><mml:mi /><mml:mrow><mml:mo>−</mml:mo><mml:mn>5.6</mml:mn></mml:mrow><mml:mrow><mml:mo>+</mml:mo><mml:mn>4.0</mml:mn></mml:mrow></mml:msubsup><mml:mspace width=\"0.222em\" /><mml:mstyle mathvariant=\"normal\"><mml:mi>g</mml:mi><mml:mi>/</mml:mi><mml:mi>c</mml:mi><mml:msup><mml:mi>m</mml:mi><mml:mn>2</mml:mn></mml:msup></mml:mstyle></mml:mrow></mml:math> for air showers induced by 10^{17} <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:msup><mml:mn>10</mml:mn><mml:mn>17</mml:mn></mml:msup></mml:math> ~eV proton, which is not negligible in the uncertainty of langle X_{max}rangle <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:mrow><mml:mo stretchy=\"false\" form=\"prefix\">〈</mml:mo><mml:msub><mml:mi>X</mml:mi><mml:mrow><mml:mi>m</mml:mi><mml:mi>a</mml:mi><mml:mi>x</mml:mi></mml:mrow></mml:msub><mml:mo stretchy=\"false\" form=\"postfix\">⟩</mml:mo></mml:mrow></mml:math> predictions.","PeriodicalId":355998,"journal":{"name":"SciPost Physics Proceedings","volume":"18 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135385502","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}
Pub Date : 2023-09-28DOI: 10.21468/scipostphysproc.13.003
Aleksei Bogdanov, N. S. Barbashina, S. S. Khokhlov, V. V. Kindin, R. P. Kokoulin, K. G. Kompaniets, A. Y. Konovalova, G. Mannocchi, A. A. Petrukhin, V. V. Shutenko, G. Trinchero, V. S. Vorobev, I. I. Yashin, E. A. Yurina, E. A. Zadeba
The data of cosmic ray NEVOD-DECOR experiment on the investigation of inclined muon bundles for a long time period (May 2012 - March 2021) are presented. The analysis showed that the observed intensity of muon bundles at primary cosmic ray energies of about 1 EeV and higher can be compatible with the expectation in frame of widely used hadron interaction models only under the assumption of an extremely heavy mass composition. This conclusion is consistent with data of several experiments on investigations of muon content in air showers, but contradicts the available fluorescence data on X_{max} Xmax which favor a light mass composition at these energies. In order to clarify the nature of the "muon puzzle", investigations of the muon bundle energy deposit in the detector material were carried out. For the first time, experimental estimates of the average energy of muons in the bundles of inclined air showers initiated by primary particles with energies from 10 to 1000 PeV have been obtained.
{"title":"Muon puzzle in inclined muon bundles detected by NEVOD-DECOR","authors":"Aleksei Bogdanov, N. S. Barbashina, S. S. Khokhlov, V. V. Kindin, R. P. Kokoulin, K. G. Kompaniets, A. Y. Konovalova, G. Mannocchi, A. A. Petrukhin, V. V. Shutenko, G. Trinchero, V. S. Vorobev, I. I. Yashin, E. A. Yurina, E. A. Zadeba","doi":"10.21468/scipostphysproc.13.003","DOIUrl":"https://doi.org/10.21468/scipostphysproc.13.003","url":null,"abstract":"The data of cosmic ray NEVOD-DECOR experiment on the investigation of inclined muon bundles for a long time period (May 2012 - March 2021) are presented. The analysis showed that the observed intensity of muon bundles at primary cosmic ray energies of about 1 EeV and higher can be compatible with the expectation in frame of widely used hadron interaction models only under the assumption of an extremely heavy mass composition. This conclusion is consistent with data of several experiments on investigations of muon content in air showers, but contradicts the available fluorescence data on X_{max} <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:msub><mml:mi>X</mml:mi><mml:mrow><mml:mi>m</mml:mi><mml:mi>a</mml:mi><mml:mi>x</mml:mi></mml:mrow></mml:msub></mml:math> which favor a light mass composition at these energies. In order to clarify the nature of the \"muon puzzle\", investigations of the muon bundle energy deposit in the detector material were carried out. For the first time, experimental estimates of the average energy of muons in the bundles of inclined air showers initiated by primary particles with energies from 10 to 1000 PeV have been obtained.","PeriodicalId":355998,"journal":{"name":"SciPost Physics Proceedings","volume":"76 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135344388","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}
Pub Date : 2023-09-28DOI: 10.21468/scipostphysproc.13.006
Luca Orusa, Mattia Di Mauro, Fiorenza Donato, Michael Korsmeier
The cosmic-ray fluxes of electrons and positrons ( e^{±} e± ) are measured with high precision by the space-borne particle spectrometer AMS-02. To infer a precise interpretation of the production processes for e^{±} e± in our Galaxy, it is necessary to have an accurate description of the secondary component, produced by the interaction of cosmic-ray proton and helium with the interstellar medium atoms. We determine new analytical functions of the Lorentz invariant cross section for the production of e^± e± by fitting data from collider experiments. The total differential cross section dsigma/dT_{e^±}(p+p→ e^±+X) dσ/dTe±(p+p→e±+X) is predicted with an uncertainty of about 5-7% in the energies relevant for AMS-02 positron flux. For further information about this work refer to [Phys. Rev. D 105, 123021 (2022)].
{"title":"New determination of the production cross section for secondary positrons and electrons in the Galaxy","authors":"Luca Orusa, Mattia Di Mauro, Fiorenza Donato, Michael Korsmeier","doi":"10.21468/scipostphysproc.13.006","DOIUrl":"https://doi.org/10.21468/scipostphysproc.13.006","url":null,"abstract":"The cosmic-ray fluxes of electrons and positrons ( e^{&#177;} <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:msup><mml:mi>e</mml:mi><mml:mo>±</mml:mo></mml:msup></mml:math> ) are measured with high precision by the space-borne particle spectrometer AMS-02. To infer a precise interpretation of the production processes for e^{&#177;} <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:msup><mml:mi>e</mml:mi><mml:mo>±</mml:mo></mml:msup></mml:math> in our Galaxy, it is necessary to have an accurate description of the secondary component, produced by the interaction of cosmic-ray proton and helium with the interstellar medium atoms. We determine new analytical functions of the Lorentz invariant cross section for the production of e^&#177; <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:msup><mml:mi>e</mml:mi><mml:mo>±</mml:mo></mml:msup></mml:math> by fitting data from collider experiments. The total differential cross section dsigma/dT_{e^&#177;}(p+p&#8594; e^&#177;+X) <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:mrow><mml:mi>d</mml:mi><mml:mi>σ</mml:mi><mml:mi>/</mml:mi><mml:mi>d</mml:mi><mml:msub><mml:mi>T</mml:mi><mml:msup><mml:mi>e</mml:mi><mml:mo>±</mml:mo></mml:msup></mml:msub><mml:mrow><mml:mo stretchy=\"true\" form=\"prefix\">(</mml:mo><mml:mi>p</mml:mi><mml:mo>+</mml:mo><mml:mi>p</mml:mi><mml:mo>→</mml:mo><mml:msup><mml:mi>e</mml:mi><mml:mo>±</mml:mo></mml:msup><mml:mo>+</mml:mo><mml:mi>X</mml:mi><mml:mo stretchy=\"true\" form=\"postfix\">)</mml:mo></mml:mrow></mml:mrow></mml:math> is predicted with an uncertainty of about 5-7% in the energies relevant for AMS-02 positron flux. For further information about this work refer to [Phys. Rev. D 105, 123021 (2022)].","PeriodicalId":355998,"journal":{"name":"SciPost Physics Proceedings","volume":"19 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135387098","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}
Pub Date : 2023-09-28DOI: 10.21468/scipostphysproc.13.021
Hari Haran Balakrishnan, S. Ahmad, M. Chakraborty, S. R. Dugad, Umananda Dev Goswami, S. K. Gupta, Y. Hayashi, P. Jagadeesan, A. Jain, P. Jain, S. Kawakami, H. Kojima, S. Mahapatra, P. K. Mohanty, R. Moharana, Yasushi Muraki, P. K. Nayak, T. Nonaka, A. Oshima, Diptiranjan Pattanaik, B. P. Pant, Mohamed Rameez, K. Ramesh, L. V. Reddy, S. Shibata, Fahim Varsi, M. Zuberi
The GRAPES-3 experiment is a unique, extensive air shower experiment consisting of 400 scintillator detectors spread over 25000 m ^2 2 and a 560 m ^2 2 muon telescope. The experiment located at Ooty, India, has been collecting data for the past two decades. The unique capabilities of GRAPES-3 have allowed the study of cosmic rays over energies from a few TeV to tens of PeV and beyond. The measurement of the directional flux of muons (E _mu μ ≥1 GeV) by the large muon telescope permits an excellent gamma-hadron separation, which then becomes a powerful tool in the study of multi-TeV gamma-ray sources and the composition of primary cosmic rays. However, the high precision measurements also enable studies of transient atmospheric and interplanetary phenomena such as those produced by thunderstorms and geomagnetic storms. This paper presents some exciting new and recent results, including updates on various ongoing analyses.
GRAPES-3实验是一个独特的、广泛的气淋实验，由400个闪烁体探测器组成，分布在25000 m ^2和一个560 m ^2的μ子望远镜。这个位于印度乌蒂的实验在过去的二十年里一直在收集数据。GRAPES-3的独特功能使得研究能量从几TeV到几十PeV甚至更高的宇宙射线成为可能。大型μ子望远镜测量μ子的定向通量(e_ mu μ≥1 GeV)，实现了良好的伽玛-强子分离，从而成为研究多tev伽玛射线源和初级宇宙射线组成的有力工具。然而，高精度的测量也使研究瞬态大气和行星际现象成为可能，例如由雷暴和地磁风暴产生的现象。本文介绍了一些令人兴奋的最新结果，包括各种正在进行的分析的更新。
{"title":"Highlights of the results from the GRAPES-3 experiment","authors":"Hari Haran Balakrishnan, S. Ahmad, M. Chakraborty, S. R. Dugad, Umananda Dev Goswami, S. K. Gupta, Y. Hayashi, P. Jagadeesan, A. Jain, P. Jain, S. Kawakami, H. Kojima, S. Mahapatra, P. K. Mohanty, R. Moharana, Yasushi Muraki, P. K. Nayak, T. Nonaka, A. Oshima, Diptiranjan Pattanaik, B. P. Pant, Mohamed Rameez, K. Ramesh, L. V. Reddy, S. Shibata, Fahim Varsi, M. Zuberi","doi":"10.21468/scipostphysproc.13.021","DOIUrl":"https://doi.org/10.21468/scipostphysproc.13.021","url":null,"abstract":"The GRAPES-3 experiment is a unique, extensive air shower experiment consisting of 400 scintillator detectors spread over 25000 m ^2 <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:msup><mml:mi /><mml:mn>2</mml:mn></mml:msup></mml:math> and a 560 m ^2 <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:msup><mml:mi /><mml:mn>2</mml:mn></mml:msup></mml:math> muon telescope. The experiment located at Ooty, India, has been collecting data for the past two decades. The unique capabilities of GRAPES-3 have allowed the study of cosmic rays over energies from a few TeV to tens of PeV and beyond. The measurement of the directional flux of muons (E _mu <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:msub><mml:mi /><mml:mi>μ</mml:mi></mml:msub></mml:math> ≥1 GeV) by the large muon telescope permits an excellent gamma-hadron separation, which then becomes a powerful tool in the study of multi-TeV gamma-ray sources and the composition of primary cosmic rays. However, the high precision measurements also enable studies of transient atmospheric and interplanetary phenomena such as those produced by thunderstorms and geomagnetic storms. This paper presents some exciting new and recent results, including updates on various ongoing analyses.","PeriodicalId":355998,"journal":{"name":"SciPost Physics Proceedings","volume":"98 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135420581","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}
Pub Date : 2023-09-28DOI: 10.21468/scipostphysproc.13.013
Olivier Deligny
Assuming that the energy density of super-heavy particles matches that of dark matter observed today, tight constraints on the couplings governing the decay process are presented as a function of the particle mass. These constraints are obtained from the lack of signatures that would be suggestive of decaying super-heavy X X particles in the data of the Pierre Auger Observatory. In particular, instanton-induced decay processes allow us to derive a bound on the reduced coupling constant of gauge interactions in the dark sector: alpha_X lesssim 0.09 αX≲0.09 , for 10^{9} lesssim M_X/mathrm{GeV} < 10^{19} 109≲MX/GeV<1019 . Cosmological aspects for super-heavy dark matter production during the reheating epoch are discussed.
{"title":"Limits to gauge coupling in the dark sector of super-heavy dark matter particles from the Pierre Auger Observatory data","authors":"Olivier Deligny","doi":"10.21468/scipostphysproc.13.013","DOIUrl":"https://doi.org/10.21468/scipostphysproc.13.013","url":null,"abstract":"Assuming that the energy density of super-heavy particles matches that of dark matter observed today, tight constraints on the couplings governing the decay process are presented as a function of the particle mass. These constraints are obtained from the lack of signatures that would be suggestive of decaying super-heavy X <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:mi>X</mml:mi></mml:math> particles in the data of the Pierre Auger Observatory. In particular, instanton-induced decay processes allow us to derive a bound on the reduced coupling constant of gauge interactions in the dark sector: alpha_X lesssim 0.09 <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:mrow><mml:msub><mml:mi>α</mml:mi><mml:mi>X</mml:mi></mml:msub><mml:mo>≲</mml:mo><mml:mn>0.09</mml:mn></mml:mrow></mml:math> , for 10^{9} lesssim M_X/mathrm{GeV} &lt; 10^{19} <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:mrow><mml:msup><mml:mn>10</mml:mn><mml:mn>9</mml:mn></mml:msup><mml:mo>≲</mml:mo><mml:msub><mml:mi>M</mml:mi><mml:mi>X</mml:mi></mml:msub><mml:mi>/</mml:mi><mml:mstyle mathvariant=\"normal\"><mml:mi>G</mml:mi><mml:mi>e</mml:mi><mml:mi>V</mml:mi></mml:mstyle><mml:mo><</mml:mo><mml:msup><mml:mn>10</mml:mn><mml:mn>19</mml:mn></mml:msup></mml:mrow></mml:math> . Cosmological aspects for super-heavy dark matter production during the reheating epoch are discussed.","PeriodicalId":355998,"journal":{"name":"SciPost Physics Proceedings","volume":"64 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135386404","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}
Pub Date : 2023-09-28DOI: 10.21468/scipostphysproc.13.010
Tianlu Yuan
Instrumenting a gigaton of ice at the geographic South Pole, the IceCube Neutrino Observatory has been at the forefront of groundbreaking scientific discoveries over the past decade. These include the observation of a flux of TeV-PeV astrophysical neutrinos, detection of the first astrophysical neutrino on the Glashow resonance and evidence of the blazar TXS 0506+056 as the first known astronomical source of high-energy neutrinos. Several questions, however, remain, pertaining to the precise origins of astrophysical neutrinos, their production mechanisms at the source and in Earth’s atmosphere and in the context of physics beyond the Standard Model. This proceeding highlights some of our latest results, from new constraints on neutrino interactions and oscillations to the latest measurements of the astrophysical neutrino flux and searches for their origins to future prospects with IceCube-Gen2.
{"title":"Neutrinos from near and far: Results from the IceCube Neutrino Observatory","authors":"Tianlu Yuan","doi":"10.21468/scipostphysproc.13.010","DOIUrl":"https://doi.org/10.21468/scipostphysproc.13.010","url":null,"abstract":"Instrumenting a gigaton of ice at the geographic South Pole, the IceCube Neutrino Observatory has been at the forefront of groundbreaking scientific discoveries over the past decade. These include the observation of a flux of TeV-PeV astrophysical neutrinos, detection of the first astrophysical neutrino on the Glashow resonance and evidence of the blazar TXS 0506+056 as the first known astronomical source of high-energy neutrinos. Several questions, however, remain, pertaining to the precise origins of astrophysical neutrinos, their production mechanisms at the source and in Earth’s atmosphere and in the context of physics beyond the Standard Model. This proceeding highlights some of our latest results, from new constraints on neutrino interactions and oscillations to the latest measurements of the astrophysical neutrino flux and searches for their origins to future prospects with IceCube-Gen2.","PeriodicalId":355998,"journal":{"name":"SciPost Physics Proceedings","volume":"69 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135388260","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}
Pub Date : 2023-09-28DOI: 10.21468/scipostphysproc.13.002
Dennis Soldin
IceCube is a cubic-kilometer Cherenkov detector in the deep ice at the geographic South Pole. The dominant event yield in the deep ice detector consists of penetrating atmospheric muons with energies above approximately 300 GeV, produced in cosmic ray air showers. In addition, the surface array, IceTop, measures the electromagnetic component and GeV muons of air showers. Hence, IceCube and IceTop yield unique opportunities to study cosmic rays with unprecedented statistics in great detail. We will present recent results of comic ray measurements from IceCube and IceTop. In this overview, we will highlight measurements of the energy spectrum of cosmic rays from 250 TeV up to the EeV range and their mass composition above 3 PeV. We will also report recent results from measurements of the muon content in air showers and discuss their consistency with predictions from current hadronic interaction models.
{"title":"Cosmic ray measurements with IceCube and IceTop","authors":"Dennis Soldin","doi":"10.21468/scipostphysproc.13.002","DOIUrl":"https://doi.org/10.21468/scipostphysproc.13.002","url":null,"abstract":"IceCube is a cubic-kilometer Cherenkov detector in the deep ice at the geographic South Pole. The dominant event yield in the deep ice detector consists of penetrating atmospheric muons with energies above approximately 300 GeV, produced in cosmic ray air showers. In addition, the surface array, IceTop, measures the electromagnetic component and GeV muons of air showers. Hence, IceCube and IceTop yield unique opportunities to study cosmic rays with unprecedented statistics in great detail. We will present recent results of comic ray measurements from IceCube and IceTop. In this overview, we will highlight measurements of the energy spectrum of cosmic rays from 250 TeV up to the EeV range and their mass composition above 3 PeV. We will also report recent results from measurements of the muon content in air showers and discuss their consistency with predictions from current hadronic interaction models.","PeriodicalId":355998,"journal":{"name":"SciPost Physics Proceedings","volume":"60 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135344961","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}
Pub Date : 2023-09-28DOI: 10.21468/scipostphysproc.13.007
Hushnud Hushnud
ALICE is a general purpose experiment designed to investigate nucleus-nucleus collisions at the Large Hadron Collider (LHC), located at CERN. The ALICE detector is optimized for the reconstruction of quarkonia through the dimuon decay channel at foward rapidity as well as the dielectron decay channel at midrapidity. In this contribution, quarkonium measurements performed by the ALICE collaboration at both midrapidity and forward rapidity for various energies and colliding systems (pp, p-Pb and Pb-Pb), will be discussed and compared to theory.
{"title":"Overview of quarkonium production with ALICE at the LHC","authors":"Hushnud Hushnud","doi":"10.21468/scipostphysproc.13.007","DOIUrl":"https://doi.org/10.21468/scipostphysproc.13.007","url":null,"abstract":"ALICE is a general purpose experiment designed to investigate nucleus-nucleus collisions at the Large Hadron Collider (LHC), located at CERN. The ALICE detector is optimized for the reconstruction of quarkonia through the dimuon decay channel at foward rapidity as well as the dielectron decay channel at midrapidity. In this contribution, quarkonium measurements performed by the ALICE collaboration at both midrapidity and forward rapidity for various energies and colliding systems (pp, p-Pb and Pb-Pb), will be discussed and compared to theory.","PeriodicalId":355998,"journal":{"name":"SciPost Physics Proceedings","volume":"11 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135387261","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}
Pub Date : 2023-09-28DOI: 10.21468/scipostphysproc.13.020
Stanislav P. Knurenko, Igor S. Petrov
Existing small, medium and large arrays for the study of cosmic rays of ultra-high energies are aimed for obtaining information about our galaxy and extragalactic space, namely to search and study astronomical objects that produce the flux of relativistic particles. The drift and interaction of such particles with magnetic fields and shock waves taking place in interstellar space causes the same interest. The shape of the energy spectrum of cosmic rays in the energy range 10^{15}-10^{18} 1015−1018 eV, where the "knee" and the "second knee’’ are observed, can be formed as a superposition of the partial spectra of various chemical elements. Verification of galactic models, using recent experimental spectral data, makes it possible to study the nature of the galactic and extragalactic components of cosmic rays. The paper presents the result of the energy spectrum of cosmic rays in the range 10^{16}-10^{18} 1016−1018 eV of measurements obtained with the Small Cherenkov array - a part of the Yakutsk array.
{"title":"On irregularities in the cosmic ray spectrum of (10^{16}-10^{18}) eV range","authors":"Stanislav P. Knurenko, Igor S. Petrov","doi":"10.21468/scipostphysproc.13.020","DOIUrl":"https://doi.org/10.21468/scipostphysproc.13.020","url":null,"abstract":"Existing small, medium and large arrays for the study of cosmic rays of ultra-high energies are aimed for obtaining information about our galaxy and extragalactic space, namely to search and study astronomical objects that produce the flux of relativistic particles. The drift and interaction of such particles with magnetic fields and shock waves taking place in interstellar space causes the same interest. The shape of the energy spectrum of cosmic rays in the energy range 10^{15}-10^{18} <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:mrow><mml:msup><mml:mn>10</mml:mn><mml:mn>15</mml:mn></mml:msup><mml:mo>−</mml:mo><mml:msup><mml:mn>10</mml:mn><mml:mn>18</mml:mn></mml:msup></mml:mrow></mml:math> eV, where the \"knee\" and the \"second knee’’ are observed, can be formed as a superposition of the partial spectra of various chemical elements. Verification of galactic models, using recent experimental spectral data, makes it possible to study the nature of the galactic and extragalactic components of cosmic rays. The paper presents the result of the energy spectrum of cosmic rays in the range 10^{16}-10^{18} <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><mml:mrow><mml:msup><mml:mn>10</mml:mn><mml:mn>16</mml:mn></mml:msup><mml:mo>−</mml:mo><mml:msup><mml:mn>10</mml:mn><mml:mn>18</mml:mn></mml:msup></mml:mrow></mml:math> eV of measurements obtained with the Small Cherenkov array - a part of the Yakutsk array.","PeriodicalId":355998,"journal":{"name":"SciPost Physics Proceedings","volume":"47 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135385774","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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