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arXiv 2021年

作者： Rodriguez, Carl L. Weatherford, Newlin C. Coughlin, Scott C. Seoane, Pau Amaro Breivik, Katelyn Chatterjee, Sourav Fragione, Giacomo Kiroǧlu, Fulya Kremer, Kyle Rui, Nicholas Z. Ye, Claire S. Zevin, Michael Rasio, Frederic A. McWilliams Center for Cosmology and Department of Physics Carnegie Mellon University PittsburghPA15213 United States Department of Physics & Astronomy Northwestern University EvanstonIL60208 United States Northwestern University EvanstonIL60208 United States Universitat Politècnica de València Camino de Vera s/n 46022 Valencia Spain DESY Zeuthen Platanenallee 6 ZeuthenD-15738 Germany Institute of Applied Mathematics Academy of Mathematics and Systems Science CAS Beijing100190 China Kavli Institute for Astronomy and Astrophysics Beijing100871 China Zentrum für Astronomie und Astrophysik TU Berlin Hardenbergstraße 36 Berlin10623 Germany Center for Computational Astrophysics Flatiron Institute 162 Fifth Ave New YorkNY10010 United States Tata Institute of Fundamental Research Homi Bhabha Road Mumbai400005 India TAPIR California Institute of Technology PasadenaCA91125 United States The Observatories of the Carnegie Institution for Science PasadenaCA91101 United States Kavli Institute for Cosmological Physics The University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Enrico Fermi Institute The University of Chicago 933 East 56th Street ChicagoIL60637 United States

We describe the public release of the Cluster Monte Carlo Code (CMC) a parallel, star-by-star N-body code for modeling dense star clusters. CMC treats collisional stellar dynamics using Hénon's method, where the cumulative effect of many two-body encounters is statistically reproduced as a single effective encounter between nearest-neighbor particles on a relaxation timescale. The star-by-star approach allows for the inclusion of additional physics, including strong gravitational three- and four-body encounters, two-body tidal and gravitational-wave captures, mass loss in arbitrary galactic tidal fields, and stellar evolution for both single and binary stars. The public release of CMC is pinned directly to the COSMIC population synthesis code, allowing dynamical star cluster simulations and population synthesis studies to be performed using identical assumptions about the stellar physics and initial conditions. As a demonstration, we present two examples of star cluster modeling: first, we perform the largest (N = 108) star-by-star N-body simulation of a Plummer sphere evolving to core collapse, reproducing the expected self-similar density profile over more than 15 orders of magnitude;second, we generate realistic models for typical globular clusters, and we show that their dynamical evolution can produce significant numbers of black hole mergers with masses greater than those produced from isolated binary evolution (such as GW190521, a recently reported merger with component masses in the pulsational pair-instability mass gap). © 2021, CC BY.

关键词： Stars

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Direct Monitoring of Li2S2Evolution and Its Influence on the Reversible Capacities of Lithium-Sulfur Batteries

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Angewandte Chemie 2023年第11期135卷

作者： Dr. Yufeng Luo Dr. Zhenhan Fang Dr. Shaorong Duan Hengcai Wu Dr. Haitao Liu Dr. Yuxing Zhao Dr. Ke Wang Prof. Qunqing Li Prof. Shoushan Fan Prof. Zijian Zheng Prof. Wenhui Duan Prof. Yuegang Zhang Prof. Jiaping Wang Tsinghua-Foxconn Nanotechnology Research Center Tsinghua University Beijing 100084 China Laboratory for Advanced Interfacial Materials and Devices School of Fashion and Textiles The Hong Kong Polytechnic University Hong Kong SAR 99077 China Department of Physics Tsinghua University Beijing 100084 China Laboratory of Computational Physics Institute of Applied Physics and Computational Mathematics Beijing 100088 China School of Materials Science and Technology China University of Geosciences Beijing 100083 China Frontier Science Center for Quantum Information Tsinghua University Beijing 100084 China State Key Laboratory of Low-Dimensional Quantum Physics Tsinghua University Beijing 100084 China

The polysulfide (PS) dissolution and low conductivity of lithium sulfides (Li 2 S) are generally considered the main reasons for limiting the reversible capacity of the lithium-sulfur (Li-S) system. However, as the inevitable intermediate between PSs and Li 2 S, lithium disulfide (Li 2 S 2 ) evolutions are always overlooked. Herein, Li 2 S 2 evolutions are monitored from the operando measurements on the pouch cell level. Results indicate that Li 2 S 2 undergoes slow electrochemical reduction and chemical disproportionation simultaneously during the discharging process, leading to further PS dissolution and Li 2 S generation without capacity contribution. Compared with the fully oxidized Li 2 S, Li 2 S 2 still residues at the end of the charging state. Therefore, instead of the considered Li 2 S and PSs, slow electrochemical conversions and side chemical reactions of Li 2 S 2 are the determining factors in limiting the sulfur utilization, corresponding to the poor reversible capacity of Li-S batteries.

关键词： Lithium Disulfides Chemical Reactions Conductive Interlayer Lithium Sulfur Battery Operando Measurement

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Numerical Modeling of Currents Circulation in Balikpapan Bay during Oil Spill Event on March 31, 2018

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IOP Conference Series: Earth and Environmental Science 2020年第1期618卷

作者： A A Nur I M Radjawane T Suprijo I Mandang Department of Earth Science Faculty of Earth Science and Technology Bandung Institute of Technology Jalan Ganesha No 10 Bandung 40132 Indonesia Hydro-Atmosphere Environment Research Group Physical Oceanography and Computational Modeling Laboratory Program Study of Physics Faculty of Mathematics and Natural Sciences Mulawarman University Jalan Barong Tongkok No 04 Samarinda 75123 Indonesia

The coastal area in Balikpapan Bay and its surrounding area has been devastated after the burst of an underwater oil pipe at the bay on March 31st, 2018, and the crude oil still continues spreading for a few days later. A three-dimensional hydrodynamic model is used to simulate the currents dynamic and investigate the influence of the current circulation on the spreading of the oil spill in Balikpapan Bay from March 31th to April 15th, 2018, to cover the event i.e. several weeks after the oil spill incident. Model results are validated by calculating the RMSE, MAPE and model skill using water level between available observation data at Semayang Port, Balikpapan station and numerical model from October 1st, 2012 to January 1st, 2013. Verification result of tidal elevation data from observation and model prediction shows a good agreement with RMSE = 7.8 cm, MAPE = 14.3% and model skill = 0.995. Surface currents circulation in Balikpapan Bay can be distinguished by the currents pattern on the spring tide and neap tide condition. During the spring tide condition, the surface currents mostly move to the east after coming out from the bay. However, the surface currents are strongly going southward after come out from the bay on the neap tide condition. Based on the satellite images captured for the next days after the event, the spreading pattern of the oil spill seems to be matched to the pattern of surface currents circulation on the spring tide condition. From the analysis of the model result, it shows that the currents circulation playing the main role to disperse the oil spill in Balikpapan Bay towards the Makassar Strait.

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Open Hardware Solutions in Quantum Technology

arXiv

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arXiv 2023年

作者： Shammah, Nathan Roy, Anurag Saha Almudever, Carmen G. Bourdeauducq, Sébastien Butko, Anastasiia Cancelo, Gustavo Clark, Susan M. Heinsoo, Johannes Henriet, Loïc Huang, Gang Jurczak, Christophe Kotilahti, Janne Landra, Alessandro LaRose, Ryan Mari, Andrea Nowrouzi, Kasra Ockeloen-Korppi, Caspar Prawiroatmodjo, Guen Siddiqi, Irfan Zeng, William J. Unitary Fund San FranciscoCA94104 United States Qruise GmbH Saarbruecken66113 Germany Technical University of Valencia Spain M-Labs Limited North Point Hong Kong Applied Mathematics and Computational Research Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Fermi National Accelerator Laboratory BataviaIL60510 United States Sandia National Laboratories AlbuquerqueNM87123 United States IQM Quantum Computers Espoo02150 Finland PASQAL 7 rue Leonard de Vinci Massy91300 France Accelerator Technology and Applied Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Quantonation Paris75010 France Center for Quantum Computing Science and Engineering Michigan State University East LansingMI48824 United States School of Science and Technology Università di Camerino Camerino62032 Italy Microsoft Quantum RedmondWA98052 United States Quantum Nanoelectronics Laboratory Department of Physics University of California at Berkeley BerkeleyCA94720 United States

Quantum technologies such as communications, computing, and sensing offer vast opportunities for advanced research and development. While an open-source ethos currently exists within some quantum technologies, especially in quantum computer programming, we argue that there are additional advantages in developing open quantum hardware (OQH). Open quantum hardware encompasses open-source software for the control of quantum devices in labs, blueprints and open-source toolkits for chip design and other hardware components, as well as openly-accessible testbeds and facilities that allow cloud-access to a wider scientific community. We provide an overview of current projects in the OQH ecosystem, identify gaps, and make recommendations on how to close them today. More open quantum hardware would accelerate technology transfer to and growth of the quantum industry and increase accessibility in science. © 2023, CC BY.

关键词： Technology transfer

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The TRAPUM Large Magellanic Cloud pulsar survey with MeerKAT I: Survey setup and first seven pulsar discoveries

arXiv

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arXiv 2024年

作者： Prayag, V. Levin, L. Geyer, M. Stappers, B.W. Carli, E. Barr, E.D. Breton, R.P. Buchner, S. Burgay, M. Kramer, M. Possenti, A. Krishnan, V. Venkatraman Venter, C. Behrend, J. Chen, W. Horn, D.M. Padmanabh, P.V. Ridolfi, A. Department of Astronomy The University of Cape Town Private Bag X3 Rondebosch Cape Town7701 South Africa Group Department of Mathematics & Applied Mathematics University of Cape Town Cape Town7700 South Africa Jodrell Bank Centre for Astrophysics Department of Physics and Astronomy The University of Manchester ManchesterM13 9PL United Kingdom Max-Planck-Institut für Radioastronomie Auf Hügel 69 BonnD-53121 Germany 2 Fir Street Black River Park Observatory Cape Town7925 South Africa INAF-Osservatorio Astronomico di Cagliari via della Scienza 5 CA Selargius09047 Italy Centre for Space Research North-West University Private Bag X6001 Potchefstroom2520 South Africa National Institute for Theoretical and Computational Sciences South Africa Max-Planck-Institut für Gravitationsphysik Albert-Einstein-Institut HannoverD-30167 Germany Leibniz Universität Hannover HannoverD-30167 Germany

The Large Magellanic Cloud (LMC) presents a unique environment for pulsar population studies due to its distinct star formation characteristics and proximity to the Milky Way. As part of the TRAPUM (TRAnsients and PUlsars with MeerKAT) Large Survey Project, we are using the core array of the MeerKAT radio telescope (MeerKAT) to conduct a targeted search of the LMC for radio pulsars at L-band frequencies, 856–1712 MHz. The excellent sensitivity of MeerKAT, coupled with a 2-hour integration time, makes the survey 3 times more sensitive than previous LMC radio pulsar surveys. We report the results from the initial four survey pointings which has resulted in the discovery of seven new radio pulsars, increasing the LMC radio pulsar population by 30 per cent. The pulse periods of these new pulsars range from 278 to 1690 ms, and the highest dispersion measure is 254.20 pc cm–3. We searched for, but did not find any significant pulsed radio emission in a beam centred on the SN 1987A remnant, establishing an upper limit of 6.3 μJy on its minimum flux density at 1400 MHz. © 2024, CC BY.

关键词： Galaxies

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Exploring Modified Gravity: Constraints on the μ and Σ Parametrization with WMAP, ACT, and SPT

arXiv

引用

arXiv 2023年

作者： Andrade, Uendert Capistrano, Abraão J.S. Di Valentino, Eleonora Nunes, Rafael C. Leinweber Center for Theoretical Physics University of Michigan 450 Church Street Ann ArborMI48109-1040 United States Department of Physics College of Literature Science and the Arts University of Michigan 450 Church Street Ann ArborMI48109-1040 United States Observatório Nacional RJ Rio de Janeiro20921-400 Brazil Universidade Federal do Paraná PR Palotina85950-000 Brazil Applied physics graduation program UNILA PR Foz do Iguaçu85867-670 Brazil School of Mathematics and Statistics University of Sheffield United Kingdom Instituto de Física Universidade Federal do Rio Grande do Sul Porto Alegre RS 91501-970 Brazil Divisão de Astrofísica Instituto Nacional de Pesquisas Espaciais Avenida dos Astronautas 1758 SP São José dos Campos12227-010 Brazil

The cosmic acceleration problem remains one of the most significant challenges in cosmology. One of the proposed solutions to this problem is the modification of gravity on large scales. In this paper, we explore the well-known μ-Σ parametrization scenarios and confront them with observational data, including the cosmic microwave background (CMB) radiation from the Wilkinson Microwave Anisotropy Probe (WMAP), Atacama Cosmology Telescope (ACT), and South Pole Telescope (SPT), as well as large-scale structure data from the Sloan Digital Sky Survey (SDSS: BAO+RSD) and Pantheon Supernovae (SN) catalog. We employ a Bayesian framework to constrain the model parameters and discuss the implications of our results on the viability of modified gravity theories. Our analysis reveals the strengths and limitations of the μ-Σ parametrization and provides valuable insights into the nature of gravity on cosmological scales. From the joint analysis of the ACT + WMAP + SDSS + SN, we find μ0 − 1 = 0.02 ± 0.19 and Σ0 − 1 = 0.021 ± 0.068 at 68% CL. In light of the SPT + WMAP + SDSS + SN, we find μ0 − 1 = 0.07 ± 0.18 and Σ0 − 1 = −0.009+−0007811 at 68% CL. In all the analyses carried out, we do not find any deviations from the theory of general relativity. Our results represent an observational update on the well-known μ-Σ parameterization in view of current CMB data, independent and competitive with the constraints obtained with the Planck data. Copyright © 2023, The Authors. All rights reserved.

关键词： Telescopes

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A demonstration of improved constraints on primordial gravitational waves with delensing

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Physical Review D 2021年第2期103卷 022004-022004页

作者： P. A. R. Ade Z. Ahmed M. Amiri A. J. Anderson J. E. Austermann J. S. Avva D. Barkats R. Basu Thakur J. A. Beall A. N. Bender B. A. Benson F. Bianchini C. A. Bischoff L. E. Bleem J. J. Bock H. Boenish E. Bullock V. Buza J. E. Carlstrom C. L. Chang J. R. Cheshire, IV H. C. Chiang T-L. Chou R. Citron J. Connors C. Corbett Moran J. Cornelison T. M. Crawford A. T. Crites M. Crumrine A. Cukierman T. de Haan M. Dierickx M. A. Dobbs L. Duband W. Everett S. Fatigoni J. P. Filippini S. Fliescher J. Gallicchio E. M. George T. St. Germaine N. Goeckner-Wald D. C. Goldfinger J. Grayson N. Gupta G. Hall M. Halpern N. W. Halverson S. Harrison S. Henderson J. W. Henning S. R. Hildebrandt G. C. Hilton G. P. Holder W. L. Holzapfel J. D. Hrubes N. Huang J. Hubmayr H. Hui K. D. Irwin J. Kang K. S. Karkare E. Karpel S. Kefeli S. A. Kernasovskiy L. Knox J. M. Kovac C. L. Kuo K. Lau A. T. Lee E. M. Leitch D. Li A. Lowitz A. Manzotti J. J. McMahon K. G. Megerian S. S. Meyer M. Millea L. M. Mocanu L. Moncelsi J. Montgomery A. Nadolski T. Namikawa T. Natoli C. B. Netterfield H. T. Nguyen J. P. Nibarger G. Noble V. Novosad R. O’Brient R. W. Ogburn, IV Y. Omori S. Padin S. Palladino S. Patil T. Prouve C. Pryke B. Racine C. L. Reichardt C. D. Reintsema S. Richter J. E. Ruhl B. R. Saliwanchik K. K. Schaffer A. Schillaci B. L. Schmitt R. Schwarz C. D. Sheehy C. Sievers G. Smecher A. Soliman A. A. Stark B. Steinbach R. V. Sudiwala G. P. Teply K. L. Thompson J. E. Tolan C. Tucker A. D. Turner C. Umiltà T. Veach J. D. Vieira A. G. Vieregg A. Wandui G. Wang A. C. Weber N. Whitehorn D. V. Wiebe J. Willmert C. L. Wong W. L. K. Wu H. Yang V. Yefremenko K. W. Yoon E. Young C. Yu L. Zeng C. Zhang Cardiff University Cardiff CF10 3XQ United Kingdom SLAC National Accelerator Laboratory 2575 Sand Hill Road Menlo Park California 94025 USA Kavli Institute for Particle Astrophysics and Cosmology Stanford University 452 Lomita Mall Stanford California 94305 USA Department of Physics and Astronomy University of British Columbia Vancouver British Columbia V6T 1Z1 Canada Fermi National Accelerator Laboratory MS209 P.O. Box 500 Batavia Illinois 60510 USA NIST Quantum Devices Group 325 Broadway Mailcode 817.03 Boulder Colorado 80305 USA Department of Physics University of Colorado Boulder Colorado 80309 USA Department of Physics University of California Berkeley California 94720 USA Harvard-Smithsonian Center for Astrophysics 60 Garden Street Cambridge Massachusetts 02138 USA California Institute of Technology MS 249-17 1216 E. California Blvd. Pasadena California 91125 USA High Energy Physics Division Argonne National Laboratory 9700 S. Cass Avenue Argonne Illinois 60439 USA Kavli Institute for Cosmological Physics University of Chicago 5640 South Ellis Avenue Chicago Illinois 60637 USA Department of Astronomy and Astrophysics University of Chicago 5640 South Ellis Avenue Chicago Illinois 60637 USA School of Physics University of Melbourne Parkville Victoria 3010 Australia Department of Physics University of Cincinnati Cincinnati Ohio 45221 USA Jet Propulsion Laboratory Pasadena California 91109 USA Department of Physics Harvard University Cambridge Massachusetts 02138 USA Minnesota Institute for Astrophysics University of Minnesota Minneapolis Minnesota 55455 USA Department of Physics University of Chicago 5640 South Ellis Avenue Chicago Illinois 60637 USA Enrico Fermi Institute University of Chicago 5640 South Ellis Avenue Chicago Illinois 60637 USA Department of Physics McGill University 3600 Rue University Montreal Quebec H3A 2T8 Canada School of Mathematics Statistics and Computer Science University of KwaZulu-Natal Dur

We present a constraint on the tensor-to-scalar ratio, r, derived from measurements of cosmic microwave background (CMB) polarization B-modes with “delensing,” whereby the uncertainty on r contributed by the sample variance of the gravitational lensing B-modes is reduced by cross-correlating against a lensing B-mode template. This template is constructed by combining an estimate of the polarized CMB with a tracer of the projected large-scale structure. The large-scale-structure tracer used is a map of the cosmic infrared background derived from Planck satellite data, while the polarized CMB map comes from a combination of South Pole Telescope, bicep/Keck, and Planck data. We expand the bicep/Keck likelihood analysis framework to accept a lensing template and apply it to the bicep/Keck dataset collected through 2014 using the same parametric foreground modeling as in the previous analysis. From simulations, we find that the uncertainty on r is reduced by ∼10%, from σ(r)=0.024 to 0.022, which can be compared with a ∼26% reduction obtained when using a perfect lensing template or if there were zero lensing B-modes. Applying the technique to the real data, the constraint on r is improved from r0.05<0.090 to r0.05<0.082 (95% C.L.). This is the first demonstration of improvement in an r constraint through delensing.

关键词： Cosmic microwave background Inflation Large scale structure of the Universe

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LtU-ILI: AN ALL-IN-ONE FRAMEWORK FOR IMPLICIT INFERENCE IN ASTROphysics AND COSMOLOGY

arXiv

引用

arXiv 2024年

作者： Ho, Matthew Bartlett, Deaglan J. Chartier, Nicolas Cuesta-Lazaro, Carolina Ding, Simon Lapel, Axel Lemos, Pablo Lovell, Christopher C. Makinen, T. Lucas Modi, Chirag Pandya, Viraj Pandey, Shivam Perez, Lucia A. Wandelt, Benjamin Bryan, Greg L. UMR 7095 98 bis bd Arago ParisF-75014 France Center for the Gravitational-Wave Universe Astronomy Program Department of Physics and Astronomy Seoul National University Seoul08826 Korea Republic of Center for Astrophysics Harvard & Smithsonian 60 Garden St CambridgeMA02138 United States The NSF AI Institute for Artificial Intelligence and Fundamental Interactions United States Department of Physics Massachusetts Institute of Technology CambridgeMA02139 United States Department of Physics Université de Montréal Montréal Canada Mila - Quebec Artificial Intelligence Institute Montréal Canada Ciela - Montreal Institute for Astrophysical Data Analysis and Machine Learning Montréal Canada Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States Institute of Cosmology and Gravitation University of Portsmouth Burnaby Road PortsmouthPO1 3FX United Kingdom & Astrophysics Group Imperial College London Blackett Laboratory Prince Consort Road LondonSW7 2AZ United Kingdom Center for Computational Mathematics Flatiron Institute 162 5th Avenue New YorkNY10010 United States Columbia Astrophysics Laboratory Columbia University 550 West 120th Street New YorkNY10027 United States 4 place Jussieu ParisF-75252 Cedex 5 France

This paper presents the Learning the Universe Implicit Likelihood Inference (LtU-ILI) pipeline, a codebase for rapid, user-friendly, and cutting-edge machine learning (ML) inference in astrophysics and cosmology. The pipeline includes software for implementing various neural architectures, training schemata, priors, and density estimators in a manner easily adaptable to any research workflow. It includes comprehensive validation metrics to assess posterior estimate coverage, enhancing the reliability of inferred results. Additionally, the pipeline is easily parallelizable and is designed for efficient exploration of modeling hyperparameters. To demonstrate its capabilities, we present real applications across a range of astrophysics and cosmology problems, such as: estimating galaxy cluster masses from X-ray photometry;inferring cosmology from matter power spectra and halo point clouds;characterizing progenitors in gravitational wave signals;capturing physical dust parameters from galaxy colors and luminosities;and establishing properties of semi-analytic models of galaxy formation. We also include exhaustive benchmarking and comparisons of all implemented methods as well as discussions about the challenges and pitfalls of ML inference in astronomical sciences. All code and examples are made publicly available at https://***/maho3/ltu-ili. © 2024, CC BY.

关键词： Cosmology

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Bridging HPC Communities through the Julia programming Language

arXiv

引用

arXiv 2022年

作者： Churavy, Valentin Godoy, William F. Bauer, Carsten Ranocha, Hendrik Schlottke-Lakemper, Michael Räss, Ludovic Blaschke, Johannes Giordano, Mosè Schnetter, Erik Omlin, Samuel Vetter, Jeffrey S. Edelman, Alan Massachussetts Institute of Technology United States Oak Ridge National Laboratory United States Paderborn Center for Parallel Computing Paderborn University Germany Department of Mathematics University of Hamburg Germany Applied and Computational Mathematics RWTH Aachen University Germany University of Stuttgart Germany ETH Zurich Switzerland Birmensdorf Switzerland National Energy Research Scientific Computing Center Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States Centre for Advanced Research Computing University College London Gower Street LondonWC1E 6BT United Kingdom Perimeter Institute 31 Caroline St. N. WaterlooONN2L 2Y5 Canada Department of Physics and Astronomy University of Waterloo 200 University Avenue West WaterlooONN2L 3G1 Canada Center for Computation & Technology Louisiana State University Baton RougeLA70803 United States ETH Zurich Switzerland

The Julia programming language has evolved into a modern alternative to fill existing gaps in scientific computing and data science applications. Julia leverages a unified and coordinated single-language and ecosystem paradigm and has a proven track record of achieving high performance without sacrificing user productivity. These aspects make Julia a viable alternative to high-performance computing's (HPC's) existing and increasingly costly many-body workflow composition strategy in which traditional HPC languages (e.g., Fortran, C, C++) are used for simulations, and higher-level languages (e.g., Python, R, MATLAB) are used for data analysis and interactive computing. Julia's rapid growth in language capabilities, package ecosystem, and community make it a promising universal language for HPC. This paper presents the views of a multidisciplinary group of researchers from academia, government, and industry that advocate for an HPC software development paradigm that emphasizes developer productivity, workflow portability, and low barriers for entry. We believe that the Julia programming language, its ecosystem, and its community provide modern and powerful capabilities that enable this group's objectives. Crucially, we believe that Julia can provide a feasible and less costly approach to programming scientific applications and workflows that target HPC facilities. In this work, we examine the current practice and role of Julia as a common, end-to-end programming model to address major challenges in scientific reproducibility, data-driven AI/machine learning, co-design and workflows, scalability and performance portability in heterogeneous computing, network communication, data management, and community education. As a result, the diversification of current investments to fulfill the needs of the upcoming decade is crucial as more supercomputing centers prepare for the exascale era. © 2022, CC BY.

关键词： Productivity

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Estimation of Shear Wave Velocity of Darul Imarah District, Aceh Besar, Indonesia by Using 1D HVSR Inversion

引用

IOP Conference Series: Materials Science and Engineering 2020年第1期846卷

作者： Y Yusran Aulia Khalqillah Umar Muksin Muhammad Syukri Syamsul Rizal Nazli Ismail Doctoral Program of Mathematics and Applied Sciences Universitas Syiah Kuala Banda Aceh Indonesia Education of Physics Universitas Islam Negeri Ar-Raniry Banda Aceh Indonesia Department of Physics Universitas Syiah Kuala Banda Aceh Indonesia Tsunami and Disaster Mitigation Research Center (TDMRC) Universitas Syiah Kuala Banda Aceh Indonesia Department of Marine Sciences Universitas Syiah Kuala Banda Aceh Indonesia

A total of 19 locations of Horizontal to Vertical Spectral Ratio (HVSR) measurements was conducted in Darul Imarah District, Aceh Besar, Indonesia. The objective of the research is to investigate the shear wave velocity (Vs) structure. This survey is important to analyze a structural characteristic through a Vs, considering the measurement points intersect to Aceh Segment Fault. One of the methods to obtain Vs is 1D HVSR inversion. In this paper, we analyzed only four of 19 measurement points of HVSR data to estimate Vs, they are AB03, AB08, AB09 and AB19 points. The inversion results show that the four points have four layers with different Vs. The average of Vs30 of AB03, AB08, AB09 and AB19 were calculated, they are 150.90 m/s, 197.16 m/s, 150.45 m/s and 316.80 m/s, respectively. The AB09 has the lowest average of Vs30 (highest amplification) than the other points and has soft soil composition. Furthermore, based on the average of Vs30 and amplification, the subsurface of AB03, AB08 and AB19 may have combination soft soil and stiff soil in 30 m depth. The complete analysis of average of Vs30 structure will be conducted at all sites including a 3D velocity structure will be derived from the interpolation of 1D velocity.

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