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arXiv 2024年

作者： Aalbers, J. Abe, K. Adrover, M. Maouloud, S. Ahmed Akerib, D.S. Al Musalhi, A.K. Alder, F. Althueser, L. Amaral, D.W.P. Amarasinghe, C.S. Ames, A. Andrieu, B. Angelides, N. Angelino, E. Antunovic, B. Aprile, E. Araújo, H.M. Armstrong, J.E. Arthurs, M. Babicz, M. Bajpai, D. Baker, A. Balzer, M. Bang, J. Barberio, E. Bargemann, J.W. Barillier, E. Basharina-Freshville, A. Baudis, L. Bauer, D. Bazyk, M. Beattie, K. Beaupere, N. Bell, N.F. Bellagamba, L. Benson, T. Bhatti, A. Biesiadzinski, T.P. Biondi, R. Biondi, Y. Birch, H.J. Bishop, E. Bismark, A. Boehm, C. Boese, K. Bolotnikov, A. Brás, P. Braun, R. Breskin, A. Brew, C.A.J. Brommer, S. Brown, A. Bruni, G. Budnik, R. Burdin, S. Cai, C. Capelli, C. Carini, G. Carmona-Benitez, M.C. Carter, M. Chauvin, A. Chawla, A. Chen, H. Cherwinka, J.J. Chin, Y.T. Chott, N.I. Chavez, A.P. Cimental Clark, K. Colijn, A.P. Colling, D.J. Conrad, J. Converse, M.V. Coronel, R. Costanzo, D. Cottle, A. Cox, G. Cuenca-García, J.J. Curran, D. Cussans, D. D’Andrea, V. Garcia, L.C. Daniel Darlington, I. Dave, S. David, A. Davies, G.J. Decowski, M.P. Deisting, A. Delgaudio, J. Dey, S. Di Donato, C. Di Felice, L. Di Gangi, P. Diglio, S. Ding, C. Dobson, J.E.Y. Doerenkamp, M. Drexlin, G. Druszkiewicz, E. Dunbar, C.L. Eitel, K. Elykov, A. Engel, R. Eriksen, S.R. Fayer, S. Fearon, N.M. Ferella, A.D. Ferrari, C. Fieldhouse, N. Fischer, H. Flaecher, H. Flehmke, T. Flierman, M. Fraser, E.D. Fruth, T.M.A. Fujikawa, K. Fulgione, W. Fuselli, C. Gaemers, P. Gaior, R. Gaitskell, R.J. Gallice, N. Galloway, M. Gao, F. Garroum, N. Geffre, A. Genovesi, J. Ghag, C. Ghosh, S. Giacomobono, R. Gibbons, R. Girard, F. Glade-Beucke, R. Glück, F. Gokhale, S. Grandi, L. Green, J. Grigat, J. van der Grinten, M.G.D. Größle, R. Guan, H. Guida, M. Gyorgy, P. Haiston, J.J. Hall, C.R. Hall, T. Hammann, R. Hannen, V. Hansmann-Menzemer, S. Hargittai, N. Hartigan-O’Connor, E. Haselschwardt, S.J. Hernandez, M. Hertel, S.A. Higuera, A. Hils, C. Nikhef the University of Groningen Van Swinderen Institute Groningen9747AG Netherlands University of Tokyo Higashi-Mozumi Kamioka Hida Gifu506-1205 Japan Physik-Institut University of Zürich Zürich8057 Switzerland LPNHE Sorbonne Université CNRS IN2P3 Paris75005 France SLAC National Accelerator Laboratory Menlo ParkCA94025-7015 United States Kavli Institute for Particle Astrophysics and Cosmology Stanford University StanfordCA94305-4085 United States LondonWC1E 6BT United Kingdom Institute for Nuclear Physics University of Münster Münster48149 Germany Department of Physics and Astronomy Rice University HoustonTX77005 United States Department of Physics University of California Santa Barbara Santa BarbaraCA93106-9530 United States Department of Physics Imperial College London Blackett Laboratory LondonSW7 2AZ United Kingdom INAF-Astrophysical Observatory of Torino Department of Physics University of Torino INFN-Torino Torino10125 Italy INFN-Laboratori Nazionali del Gran Sasso Gran Sasso Science Institute L’Aquila67100 Italy Vinca Institute of Nuclear Science University of Belgrade Mihajla Petrovica Alasa 12-14 Belgrade Serbia Physics Department Columbia University New YorkNY10027 United States Department of Physics University of Maryland College ParkMD20742-4111 United States Department of Physics & Astronomy University of Alabama TuscaloosaAL34587-0324 United States Department of Physics King’s College London LondonWC2R 2LS United Kingdom Institute for Data Processing and Electronics Karlsruhe Institute of Technology Karlsruhe76021 Germany Department of Physics Brown University ProvidenceRI02912-9037 United States ARC Centre of Excellence for Dark Matter Particle Physics School of Physics The University of Melbourne VIC3010 Australia SUBATECH IMT Atlantique CNRS IN2P3 Nantes Université Nantes44307 France BerkeleyCA94720-8099 United States Department of Physics and Astronomy University of Bologna INF

This report describes the experimental strategy and technologies for a next-generation xenon observatory sensitive to dark matter and neutrino physics. The detector will have an active liquid xenon target mass of 60–80 tonnes and is proposed by the XENON-LUX-ZEPLIN-DARWIN (XLZD) collaboration. The design is based on the mature liquid xenon time projection chamber technology of the current-generation experiments, LZ and XENONnT. A baseline design and opportunities for further optimization of the individual detector components are discussed. The experiment envisaged here has the capability to explore parameter space for Weakly Interacting Massive Particle (WIMP) dark matter down to the neutrino fog, with a 3σ evidence potential for spin-independent WIMP-nucleon cross sections as low as 3 × 10−49 cm2 (at 40 GeV/c2 WIMP mass). The observatory is also projected to have a 3σ observation potential of neutrinoless double-beta decay of 136Xe at a half-life of up to 5.7 × 1027 years. Additionally, it is sensitive to astrophysical neutrinos from the atmosphere, sun, and galactic supernovae. Copyright © 2024, The Authors. All rights reserved.

关键词： Dark Matter

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Neutrinoless Double Beta Decay Sensitivity of the XLZD Rare Event Observatory

arXiv

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arXiv 2024年

作者： Aalbers, J. Abe, K. Adrover, M. Maouloud, S. Ahmed Akerib, D.S. Musalhi, A.K. Al Alder, F. Althueser, L. Amaral, D.W.P. Amarasinghe, C.S. Ames, A. Andrieu, B. Angelides, N. Angelino, E. Antunovic, B. Aprile, E. Araújo, H.M. Armstrong, J.E. Arthurs, M. Babicz, M. Bajpai, D. Baker, A. Balzer, M. Bang, J. Barberio, E. Bargemann, J.W. Barillier, E. Basharina-Freshville, A. Baudis, L. Bauer, D. Bazyk, M. Beattie, K. Beaupere, N. Bell, N.F. Bellagamba, L. Benson, T. Bhatti, A. Biesiadzinski, T.P. Biondi, R. Biondi, Y. Birch, H.J. Bishop, E. Bismark, A. Boehm, C. Boese, K. Bolotnikov, A. Brás, P. Braun, R. Breskin, A. Brew, C.A.J. Brommer, S. Brown, A. Bruni, G. Budnik, R. Burdin, S. Cai, C. Capelli, C. Carini, G. Carmona-Benitez, M.C. Carter, M. Chauvin, A. Chawla, A. Chen, H. Cherwinka, J.J. Chin, Y.T. Chott, N.I. Chavez, A.P. Cimental Clark, K. Colijn, A.P. Colling, D.J. Conrad, J. Converse, M.V. Coronel, R. Costanzo, D. Cottle, A. Cox, G. Cuenca-García, J.J. Curran, D. Cussans, D. D’Andrea, V. Garcia, L.C. Daniel Darlington, I. Dave, S. David, A. Davies, G.J. Decowski, M.P. Deisting, A. Delgaudio, J. Dey, S. Di Donato, C. Di Felice, L. Di Gangi, P. Diglio, S. Ding, C. Dobson, J.E.Y. Doerenkamp, M. Drexlin, G. Druszkiewicz, E. Dunbar, C.L. Eitel, K. Elykov, A. Engel, R. Eriksen, S.R. Fayer, S. Fearon, N.M. Ferella, A.D. Ferrari, C. Fieldhouse, N. Fischer, H. Flaecher, H. Flehmke, T. Flierman, M. Fraser, E.D. Fruth, T.M.A. Fujikawa, K. Fulgione, W. Fuselli, C. Gaemers, P. Gaior, R. Gaitskell, R.J. Gallice, N. Galloway, M. Gao, F. Garroum, N. Geffre, A. Genovesi, J. Ghag, C. Ghosh, S. Giacomobono, R. Gibbons, R. Girard, F. Glade-Beucke, R. Glück, F. Gokhale, S. Grandi, L. Green, J. Grigat, J. van der Grinten, M.G.D. Größle, R. Guan, H. Guida, M. Gyorgy, P. Haiston, J.J. Hall, C.R. Hall, T. Hammann, R. Hannen, V. Hansmann-Menzemer, S. Hargittai, N. Hartigan-O’Connor, E. Haselschwardt, S.J. Hernandez, M. Hertel, S.A. Higuera, A. Hils, C. Nikhef The University of Groningen Van Swinderen Institute Groningen9747AG Netherlands University of Tokyo Higashi-Mozumi Kamioka Gifu Hida506-1205 Japan Physik-Institut University of Zürich Zürich8057 Switzerland LPNHE Sorbonne Université CNRS IN2P3 Paris75005 France SLAC National Accelerator Laboratory Menlo ParkCA94025-7015 United States Kavli Institute for Particle Astrophysics and Cosmology Stanford University StanfordCA94305-4085 United States LondonWC1E 6BT United Kingdom Institute for Nuclear Physics University of Münster Münster48149 Germany Department of Physics and Astronomy Rice University HoustonTX77005 United States Department of Physics University of California Santa Barbara Santa BarbaraCA93106-9530 United States Department of Physics Imperial College London Blackett Laboratory LondonSW7 2AZ United Kingdom INAF-Astrophysical Observatory of Torino Department of Physics University of Torino INFN-Torino Torino10125 Italy INFN-Laboratori Nazionali del Gran Sasso Gran Sasso Science Institute L’Aquila67100 Italy Vinca Institute of Nuclear Science University of Belgrade Mihajla Petrovica Alasa 12-14 Belgrade Serbia Physics Department Columbia University New YorkNY10027 United States Department of Physics University of Maryland College ParkMD20742-4111 United States Department of Physics & Astronomy University of Alabama TuscaloosaAL34587-0324 United States Department of Physics King’s College London LondonWC2R 2LS United Kingdom Institute for Data Processing and Electronics Karlsruhe Institute of Technology Karlsruhe76021 Germany Department of Physics Brown University ProvidenceRI02912-9037 United States ARC Centre of Excellence for Dark Matter Particle Physics School of Physics The University ofMelbourne VIC3010 Australia SUBATECH IMT Atlantique CNRS IN2P3 Nantes Université Nantes44307 France BerkeleyCA94720-8099 United States Department of Physics and Astronomy University of Bologna INFN

The XLZD collaboration is developing a two-phase xenon time projection chamber with an active mass of 60 to 80 t capable of probing the remaining WIMP-nucleon interaction parameter space down to the so-called neutrino fog. In this work we show that, based on the performance of currently operating detectors using the same technology and a realistic reduction of radioactivity in detector materials, such an experiment will also be able to competitively search for neutrinoless double beta decay in 136Xe using a natural-abundance xenon target. XLZD can reach a 3σ discovery potential half-life of 5.7×1027 yr (and a 90% CL exclusion of 1.3×1028 yr) with 10 years of data taking, corresponding to a Majorana mass range of 7.3–31.3 meV (4.8–20.5 meV). XLZD will thus exclude the inverted neutrino mass ordering parameter space and will start to probe the normal ordering region for most of the nuclear matrix elements commonly considered by the community. © 2024, CC BY-NC-SA.

关键词： Neutrons

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Beam-Plasma Dynamics in Finite-Length, Collisionless Inhomogeneous Systems

arXiv

引用

arXiv 2021年

作者： Mishra, R. Moulick, R. Adhikari, S. Marholm, S. Eklund, A.J. Miloch, W.J. Department of Physics University of Oslo PO Box 1048 Blindern OsloNO-0316 Norway Centre of Plasma Physics Institute for Plasma Research Nazirakhat Assam Sonapur782402 India Homi Bhaba National Institute Training School Complex Anushaktinagar Mumbai400094 India Department of Computational Materials Processing Institute for Energy Technology Instituttveien 8 Kjeller2007 Norway Materials Physics Oslo SINTEF Industry Forskningsveien 1 OsloNO-0373 Norway

This study investigates the streaming instability triggered by ion motion in a plasma system that is finite in length, collisionless, and inhomogeneous. Employing numerical simulations using Particle-In-Cell (PIC) techniques and kinetic equations, the study examines how inhomogeneity emerges from integrating a cold ion beam with a background plasma within a confined system. The findings suggest that steady ion flow can modify ion sound waves through acoustic reflections from system boundaries, leading to instability. Such phenomena are known to be a hydrodynamic effect. However, there are also signatures of the beam-driven ion sound instability where kinetic resonances play a pivotal role. The main objective is to understand the impact of a finite-length system on beam-plasma instability and to identify the wave modes supported in such *** Codes 76X05, 76E20, 85-10, 82D10 Copyright © 2021, The Authors. All rights reserved.

关键词： Plasma stability

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Searching for asymmetric and heavily precessing Binary Black Holes in the gravitational wave data from the LIGO third Observing Run

arXiv

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arXiv 2024年

作者： Schmidt, Stefano Caudill, Sarah Creighton, Jolien D.E. Tsukada, Leo Doke, Anushka Jain, Manvi Ray, Anarya Adhicary, Shomik Baral, Pratyusava Baylor, Amanda Cannon, Kipp Cousins, Bryce Ewing, Becca Fong, Heather George, Richard N. Godwin, Patrick Hanna, Chad Harada, Reiko Huang, Yun-Jing Huxford, Rachael Joshi, Prathamesh Kennington, James Kuwahara, Soichiro Li, Alvin K.Y. Magee, Ryan Meacher, Duncan Messick, Cody Morisaki, Soichiro Mukherjee, Debnandini Niu, Wanting Pace, Alex Posnansky, Cort Sachdev, Surabhi Sakon, Shio Singh, Divya Shah, Urja Tapia, Ron Tsutsui, Takuya Ueno, Koh Viets, Aaron Wade, Leslie Wade, Madeline Nikhef Science Park 105 Amsterdam1098 XG Netherlands Utrecht University Princetonplein 1 Utrecht3584 CC Netherlands Department of Physics University of Massachusetts DartmouthMA02747 United States Center for Scientific Computing and Data Science Research University of Massachusetts DartmouthMA02747 United States Leonard E. Parker Center for Gravitation Cosmology and Astrophysics University of Wisconsin-Milwaukee MilwaukeeWI53201 United States Department of Physics The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States International Centre for Theoretical Sciences Tata Institute of Fundamental Research Bengaluru560089 India RESCEU The University of Tokyo Tokyo113-0033 Japan Department of Physics University of Illinois UrbanaIL61801 United States Department of Physics and Astronomy University of British Columbia VancouverBCV6T 1Z4 Canada Graduate School of Science The University of Tokyo Tokyo113-0033 Japan Center for Gravitational Physics University of Texas at Austin AustinTX78712 United States LIGO Laboratory California Institute of Technology MS 100-36 PasadenaCA91125 United States Department of Astronomy and Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational and Data Sciences The Pennsylvania State University University ParkPA16802 United States LIGO Laboratory California Institute of Technology PasadenaCA91125 United States MIT Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Institute for Cosmic Ray Research The University of Tokyo 5-1-5 Kashiwanoha Chiba Kashiwa277-8582 Japan NASA Marshall Space Flight Center HuntsvilleAL35811 United States Center for Space Plasma and Aeronomic Research University of Alabama in Huntsville HuntsvilleAL35899 United S

Leveraging the features of the GstLAL pipeline, we present the results of a matched filtering search for asymmetric binary black hole systems with heavily misaligned spins in LIGO and Virgo data taken during the third observing run. Our target systems show strong imprints of precession whereas current searches have non-optimal sensitivity in detecting them. After measuring the sensitivity improvement brought by our search over standard spin-aligned searches, we report the detection of 30 gravitational wave events already discovered in the latest version of the Gravitational Wave Transient Catalog. However, we do not find any additional significant gravitational wave candidates. Our results allow us to place an upper limit of R90% = 0.28+0−0.3304 Gpc−3yr−1 on the merger rate of a hypothetical subpopulation of asymmetric, heavily precessing signals, not identified by other searches. Since our upper limit is consistent with the latest rate estimates from the LIGO-Virgo-KAGRA collaboration, our findings rule out the existence of a yet-to-be-discovered population of precessing binaries. © 2024, CC BY.

关键词： Matched filters

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New approaches to the general relativistic Poynting-Robertson effect

arXiv

引用

arXiv 2020年

作者： de Falco, Vittorio Research Centre for Computational Physics and Data Processing Faculty of Philosophy & Science Silesian University in Opava Bezručovo nám. 13 OpavaCZ-74601 Czech Republic

Objectives: A systematic study on the general relativistic Poynting-Robertson effect has been developed so far by introducing different complementary approaches, which can be mainly divided in two kinds: (1) improving the theoretical assessments and model in its simple aspects, and (2) extracting mathematical and physical information from such system with the aim to extend methods or results to other similar physical systems of analogue structure. Methods/Analysis: We use these theoretical approaches: relativity of observer splitting formalism;Lagrangian formalism and Rayleigh potential with a new integration method;Lyapunov theory os stability. Findings: We determined the three-dimensional formulation of the general relativistic Poynting-Robertson effect model. We determine the analytical form of the Rayleigh potential and discuss its implications. We prove that the critical hypersurfaces (regions where there is a balance between gravitational and radiation forces) are stable configurations. Novelty /Improvement: Our new contributions are: to have introduced the three-dimensional description;to have determined the general relativistic Rayleigh potential for the first time in the General Relativity literature;to have provided an alternative, general and more elegant proof of the stability of the critical hypersurfaces. Copyright © 2020, The Authors. All rights reserved.

关键词： Relativity

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Exploring the effect of different cosmologies on the Epoch of Reionization 21-cm signal with Polar

arXiv

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arXiv 2024年

作者： Acharya, Anshuman Ma, Qing-Bo Giri, Sambit K. Ciardi, Benedetta Ghara, Raghunath Mellema, Garrelt Zaroubi, Saleem Hothi, Ian Iliev, Ilian T. Koopmans, Léon V.E. Bianco, Michele Max-Planck-Institut für Astrophysik Garching85748 Germany School of Physics and Electronic Science Guizhou Normal University Guiyang550001 China Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing Guizhou Normal University Guiyang550001 China Nordita KTH Royal Institute of Technology Stockholm University Hannes Alfvéns väg 12 StockholmSE-106 91 Sweden Department of Physical Sciences Indian Institute of Science Education and Research Kolkata WB Mohanpur741 246 India The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova StockholmSE-10691 Sweden Kapteyn Astronomical Institute University of Groningen P.O. Box 800 Groningen9700AV Netherlands Astrophysics Research Centre The Open University of Israel Ra’anana4353701 Israel LERMA Observatoire de Paris PSL Research University CNRS Sorbonne Université ParisF-75014 France Laboratoire de Physique de l’ENS ENS Université PSL CNRS Sorbonne Université Universitée Paris Cité Paris75005 France Astronomy Centre Department of Physics & Astronomy Pevensey III Building University of Sussex Falmer BrightonBN1 9QH United Kingdom Institute for Particle Physics and Astrophysics ETH Zurich Wolfgang-Pauli-Str 27 Zurich8093 Switzerland

A detection of the 21-cm signal power spectrum from the Epoch of Reionization is imminent, thanks to consistent advancements from telescopes such as LOFAR, MWA, and HERA, along with the development of SKA. In light of this progress, it is crucial to expand the parameter space of simulations used to infer astrophysical properties from this signal. In this work, we explore the role of cosmological parameters such as the Hubble constant 0 and the matter clustering amplitude 8, whose values as provided by measurements at different redshifts are in tension. We run N-body simulations using Gadget-4, and post-process them with the reionization simulation code Polar, that uses L-Galaxies to include galaxy formation and evolution properties and Grizzly to execute 1-D radiative transfer of ionizing photons in the intergalactic medium (IGM). We compare our results with the latest JWST observations and explore which astrophysical properties for different cosmologies are necessary to match the observed UV luminosity functions at redshifts = 10 and 9. Additionally, we explore the impact of these parameters on the observed 21-cm signal power spectrum, focusing on the redshifts within the range of LOFAR 21-cm signal observations ( ≈ 8.5 − 10). Despite differences in cosmological and astrophysical parameters, the 21-cm power spectrum at these redshifts agrees with presently observed upper limits. This suggests the need for broader physical parameter spaces for inference modeling to account for all models that agree with observations. However, we also propose stronger constraining power by using a combination of galactic and IGM observables. © 2024, CC BY.

关键词： Cosmology

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Artificial intelligence for geoscience:Progress,challenges,and perspectives

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The Innovation 2024年第5期5卷 136-160,135页

作者： Tianjie Zhao Sheng Wang Chaojun Ouyang Min Chen Chenying Liu Jin Zhang Long Yu Fei Wang Yong Xie Jun Li Fang Wang Sabine Grunwald Bryan MWong Fan Zhang Zhen Qian Yongjun Xu Chengqing Yu Wei Han Tao Sun Zezhi Shao Tangwen Qian Zhao Chen Jiangyuan Zeng Huai Zhang Husi Letu Bing Zhang Li Wang Lei Luo Chong Shi Hongjun Su Hongsheng Zhang Shuai Yin Ni Huang Wei Zhao Nan Li Chaolei Zheng Yang Zhou Changping Huang Defeng Feng Qingsong Xu Yan Wu Danfeng Hong Zhenyu Wang Yinyi Lin Tangtang Zhang Prashant Kumar Antonio Plaza Jocelyn Chanussot Jiabao Zhang Jiancheng Shi Lizhe Wang Aerospace Information Research Institute Chinese Academy of SciencesBeijing 100094China School of Computer Science China University of GeosciencesWuhan 430078China State Key Laboratory of Mountain Hazards and Engineering Resilience Institute of Mountain Hazards and EnvironmentChinese Academy of SciencesChengdu 610299China Key Laboratory of Virtual Geographic Environment(Ministry of Education of PRC) Nanjing Normal UniversityNanjing 210023China Data Science in Earth Observation Technical University of Munich80333 MunichGermany The National Key Laboratory of Water Disaster Prevention Yangtze Institute for Conservation and DevelopmentHohai UniversityNanjing 210098China Institute of Computing Technology Chinese Academy of SciencesBeijing 100190China School of Geographical Sciences Nanjing University of Information Science and TechnologyNanjing 210044China State Key Laboratory of Soil and Sustainable Agriculture Institute of Soil ScienceChinese Academy of SciencesNanjing 210008China Soil Water and Ecosystem Sciences DepartmentUniversity of FloridaPO Box 110290GainesvilleFLUSA Materials Science Engineering Program Cooperating Faculty Member in the Department of Chemistry and Department of Physics Astronomy University of CaliforniaCaliforniaRiversideCA 92521USA Institute of Remote Sensing and Geographical Information System School of Earth and Space SciencesPeking UniversityBeijing 100871China Key Laboratory of Computational Geodynamics University of Chinese Academy of SciencesBeijing 100049China International Research Center of Big Data for Sustainable Development Goals Beijing 100094China College of Geography and Remote Sensing Hohai UniversityNanjing 211100China Department of Geography The University of Hong KongHong Kong 999077SARChina Jiangsu Key Laboratory of Atmospheric Environment Monitoring and Pollution Control Nanjing 210044China School of Environmental Science and Engineering Nanjing University of Information Science&TechnologyNanjing 210044China Collaborative Inno

This paper explores the evolution of geoscientific inquiry,tracing the progression from traditional physics-based models to modern data-driven approaches facilitated by significant advancements in artificial intelligence(AI)and data collection *** models,which are grounded in physical and numerical frameworks,provide robust explanations by explicitly reconstructing underlying physical ***,their limitations in comprehensively capturing Earth’s complexities and uncertainties pose challenges in optimization and real-world *** contrast,contemporary data-driven models,particularly those utilizing machine learning(ML)and deep learning(DL),leverage extensive geoscience data to glean insights without requiring exhaustive theoretical *** techniques have shown promise in addressing Earth science-related ***,challenges such as data scarcity,computational demands,data privacy concerns,and the“black-box”nature of AI models hinder their seamless integration into *** integration of physics-based and data-driven methodologies into hybrid models presents an alternative *** models,which incorporate domain knowledge to guide AI methodologies,demonstrate enhanced efficiency and performance with reduced training data *** review provides a comprehensive overview of geoscientific research paradigms,emphasizing untapped opportunities at the intersection of advanced AI techniques and *** examines major methodologies,showcases advances in large-scale models,and discusses the challenges and prospects that will shape the future landscape of AI in *** paper outlines a dynamic field ripe with possibilities,poised to unlock new understandings of Earth’s complexities and further advance geoscience exploration.

关键词： Earth utilizing landscape

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When to Point Your Telescopes: Gravitational Wave Trigger Classification for Real-Time Multi-Messenger Followup Observations

arXiv

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arXiv 2023年

作者： Ray, Anarya Niu, Wanting Sakon, Shio Ewing, Becca Creighton, Jolien D.E. Hanna, Chad Adhicary, Shomik Baral, Pratyusava Baylor, Amanda Cannon, Kipp Caudill, Sarah Cousins, Bryce Fong, Heather George, Richard N. Godwin, Patrick Harada, Reiko Huang, Yun-Jing Huxford, Rachael Joshi, Prathamesh Kapadia, Shasvath Kennington, James Kuwahara, Soichiro Li, Alvin K.Y. Magee, Ryan Meacher, Duncan Messick, Cody Morisaki, Soichiro Mukherjee, Debnandini Pace, Alex Posnansky, Cort Sachdev, Surabhi Singh, Divya Tapia, Ron Tsukada, Leo Tsutsui, Takuya Ueno, Koh Viets, Aaron Wade, Leslie Wade, Madeline Leonard E. Parker Center for Gravitation Cosmology and Astrophysics University of Wisconsin-Milwaukee MilwaukeeWI53201 United States Department of Physics The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States RESCEU The University of Tokyo Tokyo113-0033 Japan Department of Physics University of Massachusetts DartmouthMA02747 United States Center for Scientific Computing and Data Science Research University of Massachusetts DartmouthMA02747 United States Department of Physics University of Illinois UrbanaIL61801 United States Department of Physics and Astronomy University of British Columbia VancouverBCV6T 1Z4 Canada Graduate School of Science The University of Tokyo Tokyo113-0033 Japan Center for Gravitational Physics University of Texas at Austin AustinTX78712 United States LIGO Laboratory California Institute of Technology MS 100-36 PasadenaCA91125 United States The Inter-University Centre for Astronomy and Astrophysics Post Bag 4 Ganeshkhind Pune411007 India MIT Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Institute for Cosmic Ray Research The University of Tokyo 5-1-5 Kashiwanoha Kashiwa Chiba277-8582 Japan NASA Marshall Space Flight Center HuntsvilleAL35811 United States Center for Space Plasma and Aeronomic Research University of Alabama in Huntsville HuntsvilleAL35899 United States School of Physics Georgia Institute of Technology AtlantaGA30332 United States Institute for Computational and Data Sciences The Pennsylvania State University University ParkPA16802 United States Concordia University Wisconsin MequonWI53097 United States Department of Physics Hayes Hall Kenyon College GambierOH43022 United States

We develop a robust and self-consistent framework to extract and classify gravitational wave candidates from noisy data, for the purpose of assisting in real-time multi-messenger follow-ups during LIGO-Virgo-KAGRA’s fourth observing run (O4). Our formalism implements several improvements to the low latency calculation of the probability of astrophysical origin (Pastro), so as to correctly account for various factors such as the sensitivity change between observing runs, and the deviation of the recovered template waveform from the true gravitational wave signal that can strongly bias said calculation. We demonstrate the high accuracy with which our new formalism recovers and classifies gravitational wave triggers, by analyzing replay data from previous observing runs injected with simulated sources of different categories. We show that these improvements enable the correct identification of the majority of simulated sources, many of which would have otherwise been misclassified. We carry out the aforementioned analysis by implementing our formalism through the GstLAL search pipeline even though it can be used in conjunction with potentially any matched filtering pipeline. Armed with robust and self-consistent Pastro values, the GstLAL pipeline can be expected to provide accurate source classification information for assisting in multi-messenger follow-up observations to gravitational wave alerts sent out during O4. © 2023, CC BY.

关键词： Gravity waves

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Cosmogenic background simulations for the DARWIN observatory at different underground locations

arXiv

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arXiv 2023年

作者： Adrover, M. Althueser, L. Andrieu, B. Angelino, E. Angevaare, J.R. Antunovic, B. Aprile, E. Babicz, M. Bajpai, D. Barberio, E. Baudis, L. Bazyk, M. Bell, N. Bellagamba, L. Biondi, R. Biondi, Y. Bismark, A. Boehm, C. Breskin, A. Brookes, E.J. Brown, A. Bruno, G. Budnik, R. Capelli, C. Cardoso, J.M.R. Chauvin, A. Cimental Chavez, A.P. Colijn, A.P. Conrad, J. Jose. Cuenca-García, J. Andrea, V.D. Decowski, M.P. Deisting, A. Di Gangi, P. Diglio, S. Doerenkamp, M. Drexlin, G. Eitel, K. Elykov, A. Engel, R. Farrell, S. Ferella, A.D. Ferrari, C. Fischer, H. Flierman, M. Fulgione, W. Gaemers, P. Gaior, R. Galloway, M. Garroum, N. Ghosh, S. Girard, F. Glade-Beucke, R. Glück, F. Grandi, L. Grigat, J. Größle, R. Guan, H. Guida, M. Hammann, R. Hannen, V. Hansmann-Menzemer, S. Hargittai, N. Hasegawa, T. Hils, C. Higuera, A. Hiraoka, K. Hoetzsch, L. Iacovacci, M. Itow, Y. Jakob, J. Jörg, F. Kara, M. Kavrigin, P. Kazama, S. Keller, M. Kilminster, B. Kleifges, M. Kobayashi, M. Kopec, A. von Krosigk, B. Kuger, F. Landsman, H. Lang, R.F. Li, I. Li, S. Liang, S. Lindemann, S. Lindner, M. Lombardi, F. Loizeau, J. Luce, T. Ma, Y. Macolino, C. Mahlstedt, J. Mancuso, A. Marrodán Undagoitia, T. Lopes, J.A.M. Marignetti, F. Martens, K. Masbou, J. Mastroianni, S. Milutinovic, S. Miuchi, K. Miyata, R. Molinario, A. Monteiro, C.M.B. Morå, K. Morteau, E. Mosbacher, Y. Müller, J. Murra, M. Newstead, J.L. Ni, K. Oberlack, U.G. Ostrovskiy, I. Paetsch, B. Pandurovic, M. Pellegrini, Q. Peres, R. Pienaar, J. Pierre, M. Piotter, M. Plante, G. Pollmann, T.R. Principe, L. Qi, J. Qin, J. Rajado Silva, M. Ramírez García, D. Razeto, A. Sakamoto, S. Sanchez, L. Sanchez-Lucas, P. dos Santos, J.M.F. Sartorelli, G. Scaffidi, A. Schulte, P. Schultz-Coulon, H.-C. Schulze Eißing, H. Schumann, M. Scotto Lavina, L. Selvi, M. Semeria, F. Shagin, P. Sharma, S. Shen, W. Silva, M. Simgen, H. Singh, R. Solmaz, M. Stanley, O. Steidl, M. Tan, P.-L. Terliuk, A. Physik-Institut University of Zürich Zürich8057 Switzerland Institut für Kernphysik Westfälische Wilhelms-Universität Münster Münster48149 Germany LPNHE Sorbonne Université CNRS IN2P3 Paris75005 France INAF-Astrophysical Observatory of Torino Department of Physics University of Torino INFN-Torino Torino10125 Italy Nikhef The University of Amsterdam Science Park Amsterdam1098XG Netherlands Vinca Institute of Nuclear Science University of Belgrade Mihajla Petrovica Alasa 12-14 Belgrade Serbia Physics Department Columbia University New YorkNY10027 United States New York University Abu Dhabi Center for Astro Particle and Planetary Physics Abu Dhabi United Arab Emirates Department of Physics and Astronomy University of Alabama TuscaloosaAL35487 United States Institute for Data Processing and Electronics Karlsruhe Institute of Technology Karlsruhe76021 Germany ARC Centre of Excellence for Dark Matter Particle Physics School of Physics The University of Melbourne VIC3010 Australia SUBATECH IMT Atlantique CNRS IN2P3 Université de Nantes Nantes44307 France Department of Physics and Astronomy University of Bologna INFN-Bologna Bologna40126 Italy Max-Planck-Institut für Kernphysik Heidelberg69117 Germany Institute for Astroparticle Physics Karlsruhe Institute of Technology Karlsruhe76021 Germany School of Physics The University of Sydney NSW 2006 Camperdown Sydney Australia Department of Particle Physics and Astrophysics Weizmann Institute of Science Rehovot7610001 Israel Physikalisches Institut Universität Freiburg Freiburg79104 Germany LIBPhys Department of Physics University of Coimbra Coimbra3004-516 Portugal Physikalisches Institut Universität Heidelberg Heidelberg Germany Oskar Klein Centre Department of Physics Stockholm University AlbaNova StockholmSE-10691 Sweden INFN-Laboratori Nazionali del Gran Sasso Gran Sasso Science Institute L’Aquila67100 Italy Institut für Physik & Exzellenzcluster PRISMA+ Johannes Gutenber

Xenon dual-phase time projections chambers (TPCs) have proven to be a successful technology in studying physical phenomena that require low-background conditions. With 40t of liquid xenon (LXe) in the TPC baseline design, DARWIN will have a high sensitivity for the detection of particle dark matter, neutrinoless double beta decay (0νββ), and axion-like particles (ALPs). Although cosmic muons are a source of background that cannot be entirely eliminated, they may be greatly diminished by placing the detector deep underground. In this study, we used Monte Carlo simulations to model the cosmogenic background expected for the DARWIN observatory at four underground laboratories: Laboratori Nazionali del Gran Sasso (LNGS), Sanford Underground research Facility (SURF), Laboratoire Souterrain de Modane (LSM) and SNOLAB. We determine the production rates of unstable xenon isotopes and tritium due to muon-included neutron fluxes and muon-induced spallation. These are expected to represent the dominant contributions to cosmogenic backgrounds and thus the most relevant for site selection. Copyright © 2023, The Authors. All rights reserved.

关键词： Observatories

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Reflection-asymmetric wormholes and their double shadows

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Physical Review D 2020年第8期102卷 084044-084044页

作者： Maciek Wielgus Jiří Horák Frederic Vincent Marek Abramowicz Nicolaus Copernicus Astronomical Centre Polish Academy of Sciences Bartycka 18 00-716 Warsaw Poland Research Center for Computational Physics and Data Processing Institute of Physics Silesian University in Opava Bezručovo náměstí 1150/13746 01 Opava Czech Republic and Department of Physics Göteborg University 412-96 Göteborg Sweden

We discuss construction and observational properties of wormholes obtained by connecting two Reissner-Nordström spacetimes with distinct mass and charge parameters. These objects are spherically symmetric, but not reflection symmetric, as the connected spacetimes differ. The reflection-asymmetric wormholes may reflect a significant fraction of the infalling radiation back to the spacetime of its origin. We interpret this effect in a simple framework of the effective photon potential. Depending on the model parameters, image of such a wormhole seen by a distant observer (its “shadow”) may contain a photon ring formed on the observer’s side, photon ring formed on the other side of the wormhole, or both photon rings. These unique topological features would allow us to firmly distinguish this class of objects from Kerr black holes using radioastronomical observations.

关键词： Classical black holes General relativity General relativity equations & solutions Radio, microwave, & sub-mm astronomy

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