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arXiv 2022年

作者： Colangelo, G. Davier, M. El-Khadra, Aida X. Hoferichter, M. Lehner, C. Lellouch, L. Mibe, T. Roberts, B.L. Teubner, T. Wittig, H. Ananthanarayan, B. Bashir, A. Bijnens, J. Blum, T. Boyle, P. Bray-Ali, N. Caprini, I. Calame, C.M. Carloni Catà, O. Cè, M. Charles, J. Christ, N.H. Curciarello, F. Danilkin, I. Das, D. Deineka, O. Della Morte, M. Denig, A. DeTar, C.E. Dominguez, C.A. Eichmann, G. Fischer, C.S. Gérardin, A. Giusti, D. Golterman, M. Gottlieb, Steven Gülpers, V. Hagelstein, F. Hayakawa, M. Hermansson-Truedsson, N. Hoid, B.-L. Holz, S. Izubuchi, T. Jüttner, A. Keshavarzi, A. Knecht, M. Kronfeld, A.S. Kubis, B. Kupść, A. Lahert, S. Liu, K.F. Lüdtke, J. Lynch, M. Malaescu, B. Maltman, K. Marciano, W. Marinković, M.K. Masjuan, P. Meyer, H.B. Müller, S.E. Neil, E.T. Passera, M. Pepe, M. Peris, S. Petrov, A.A. Procura, M. Raya, K. Rebhan, A. Risch, A. Rodríguez-Sánchez, A. Roig, P. Sánchez-Puertas, P. Simula, S. Stoffer, P. Stokes, F.M. Sugar, R. Tsang, J.T. van de Water, R.S. Avilés-Casco, A. Vaquero Venanzoni, G. von Hippel, G.M. Zhang, Z. Albert Einstein Center for Fundamental Physics Institute for Theoretical Physics University of Bern Sidlerstrasse 5 Bern3012 Switzerland IJCLab Université Paris-Saclay CNRS IN2P3 Orsay 91405 France Department of Physics Illinois Center for Advanced Studies of the Universe University of Illinois UrbanaIL61801 United States Particle Physics Department Theory Division Fermi National Accelerator Laboratory BataviaIL60510 United States Universität Regensburg Fakultät für Physik Universitätsstraße 31 Regensburg93040 Germany Aix Marseille Univ Université de Toulon CNRS CPT Marseille France Tsukuba305-0801 Japan Department of Physics Boston University BostonMA02215 United States Department of Mathematical Sciences University of Liverpool LiverpoolL69 3BX United Kingdom PRISMA+ Cluster of Excellence Institute for Nuclear Physics Johannes Gutenberg University of Mainz Mainz55099 Germany Helmholtz Institute Mainz Mainz55099 Germany GSI Helmholtzzentrum für Schwerionenforschung Darmstadt64291 Germany Centre for High Energy Physics Indian Institute of Science Bangalore560 012 India Instituto de Física y Matemáticas Universidad Michoacana de San Nicolás de Hidalgo Michoacán Morelia58040 Mexico Department of Astronomy and Theoretical Physics Lund University Sölvegatan 14A Lund22362 Sweden Department of Physics Unit 3046 University of Connecticut 196 Auditorium Road StorrsCT06269-3046 United States RIKEN BNL Research Center Brookhaven National Laboratory UptonNY11973 United States Physics Department Brookhaven National Laboratory UptonNY11973 United States Department of Physical Sciences Mount Saint Mary's University Los Angeles United States Horia Hulubei National Institute for Physics and Nuclear Engineering P.O.B. MG-6 Bucharest-Magurele 077125 Romania Sezione di Pavia Via A. Bassi 6 Pavia27100 Italy Theoretische Physik 1 Universität Siegen Walter-Flex-Str. 3 Siegen57068 Germany Department of Physics Columbia Universi

We discuss the prospects for improving the precision on the hadronic corrections to the anomalous magnetic moment of the muon, and the plans of the Muon g−2 Theory Initiative to update the Standard Model prediction. C... 详细信息

关键词： Charged particles

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Constraints on Cosmic Strings Using Data from the Third Advanced LIGO–Virgo Observing Run

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Physical Review Letters 2021年第24期126卷 241102-241102页

作者： R. Abbott T. D. Abbott S. Abraham F. Acernese K. Ackley A. Adams C. Adams R. X. Adhikari V. B. Adya C. Affeldt D. Agarwal M. Agathos K. Agatsuma N. Aggarwal O. D. Aguiar L. Aiello A. Ain P. Ajith T. Akutsu K. M. Aleman G. Allen A. Allocca P. A. Altin A. Amato S. Anand A. Ananyeva S. B. Anderson W. G. Anderson M. Ando S. V. Angelova S. Ansoldi J. M. Antelis S. Antier S. Appert Koya Arai Koji Arai Y. Arai S. Araki A. Araya M. C. Araya J. S. Areeda M. Arène N. Aritomi N. Arnaud S. M. Aronson H. Asada Y. Asali G. Ashton Y. Aso S. M. Aston P. Astone F. Aubin P. Auclair P. Aufmuth K. AultONeal C. Austin S. Babak F. Badaracco M. K. M. Bader S. Bae Y. Bae A. M. Baer S. Bagnasco Y. Bai L. Baiotti J. Baird R. Bajpai M. Ball G. Ballardin S. W. Ballmer M. Bals A. Balsamo G. Baltus S. Banagiri D. Bankar R. S. Bankar J. C. Barayoga C. Barbieri B. C. Barish D. Barker P. Barneo S. Barnum F. Barone B. Barr L. Barsotti M. Barsuglia D. Barta J. Bartlett M. A. Barton I. Bartos R. Bassiri A. Basti M. Bawaj J. C. Bayley A. C. Baylor M. Bazzan B. Bécsy V. M. Bedakihale M. Bejger I. Belahcene V. Benedetto D. Beniwal M. G. Benjamin T. F. Bennett J. D. Bentley M. BenYaala F. Bergamin B. K. Berger S. Bernuzzi D. Bersanetti A. Bertolini J. Betzwieser R. Bhandare A. V. Bhandari D. Bhattacharjee S. Bhaumik J. Bidler I. A. Bilenko G. Billingsley R. Birney O. Birnholtz S. Biscans M. Bischi S. Biscoveanu A. Bisht B. Biswas M. Bitossi M.-A. Bizouard J. K. Blackburn J. Blackman C. D. Blair D. G. Blair R. M. Blair F. Bobba N. Bode M. Boer G. Bogaert M. Boldrini F. Bondu E. Bonilla R. Bonnand P. Booker B. A. Boom R. Bork V. Boschi N. Bose S. Bose V. Bossilkov V. Boudart Y. Bouffanais A. Bozzi C. Bradaschia P. R. Brady A. Bramley A. Branch M. Branchesi M. Breschi T. Briant J. H. Briggs A. Brillet M. Brinkmann P. Brockill A. F. Brooks J. Brooks D. D. Brown S. Brunett G. Bruno R. Bruntz J. Bryant A. Buikema T. Bulik H. J. Bulten A. Buonanno R. Buscicchio D. Buskulic L. Cadonati M. Caesar G. Cagnoli C. Cahillane H. W. Cain, III J. Calderón Bustillo J. D LIGO Laboratory California Institute of Technology Pasadena California 91125 USA Louisiana State University Baton Rouge Louisiana 70803 USA Inter-University Centre for Astronomy and Astrophysics Pune 411007 India Dipartimento di Farmacia Università di Salerno I-84084 Fisciano Salerno Italy INFN Sezione di Napoli Complesso Universitario di Monte S.Angelo I-80126 Napoli Italy OzGrav School of Physics and Astronomy Monash University Clayton 3800 Victoria Australia Christopher Newport University Newport News Virginia 23606 USA LIGO Livingston Observatory Livingston Louisiana 70754 USA OzGrav Australian National University Canberra Australian Capital Territory 0200 Australia Max Planck Institute for Gravitational Physics (Albert Einstein Institute) D-30167 Hannover Germany Leibniz Universität Hannover D-30167 Hannover Germany University of Cambridge Cambridge CB2 1TN United Kingdom Theoretisch-Physikalisches Institut Friedrich-Schiller-Universität Jena D-07743 Jena Germany University of Birmingham Birmingham B15 2TT United Kingdom Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) Northwestern University Evanston Illinois 60208 USA Instituto Nacional de Pesquisas Espaciais 12227-010 São José dos Campos São Paulo Brazil Gravity Exploration Institute Cardiff University Cardiff CF24 3AA United Kingdom Gran Sasso Science Institute (GSSI) I-67100 L’Aquila Italy INFN Laboratori Nazionali del Gran Sasso I-67100 Assergi Italy INFN Sezione di Pisa I-56127 Pisa Italy Università di Pisa I-56127 Pisa Italy International Centre for Theoretical Sciences Tata Institute of Fundamental Research Bengaluru 560089 India Gravitational Wave Science Project National Astronomical Observatory of Japan (NAOJ) Mitaka City Tokyo 181-8588 Japan Advanced Technology Center National Astronomical Observatory of Japan (NAOJ) Mitaka City Tokyo 181-8588 Japan California State University Fullerton Fullerton California 92831 USA NCSA University of Illi

We search for gravitational-wave signals produced by cosmic strings in the Advanced LIGO and Virgo full O3 dataset. Search results are presented for gravitational waves produced by cosmic string loop features such as cusps, kinks, and, for the first time, kink-kink collisions. A template-based search for short-duration transient signals does not yield a detection. We also use the stochastic gravitational-wave background energy density upper limits derived from the O3 data to constrain the cosmic string tension Gμ as a function of the number of kinks, or the number of cusps, for two cosmic string loop distribution models. Additionally, we develop and test a third model that interpolates between these two models. Our results improve upon the previous LIGO–Virgo constraints on Gμ by 1 to 2 orders of magnitude depending on the model that is tested. In particular, for the one-loop distribution model, we set the most competitive constraints to date: Gμ≲4×10−15. In the case of cosmic strings formed at the end of inflation in the context of grand unified theories, these results challenge simple inflationary models.

关键词： Cosmic strings & domain walls Gravitational waves

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Author Correction: Federated learning enables big data for rare cancer boundary detection

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Nature communications 2023年第1期14卷 436页

作者： Sarthak Pati Ujjwal Baid Brandon Edwards Micah Sheller Shih-Han Wang G Anthony Reina Patrick Foley Alexey Gruzdev Deepthi Karkada Christos Davatzikos Chiharu Sako Satyam Ghodasara Michel Bilello Suyash Mohan Philipp Vollmuth Gianluca Brugnara Chandrakanth J Preetha Felix Sahm Klaus Maier-Hein Maximilian Zenk Martin Bendszus Wolfgang Wick Evan Calabrese Jeffrey Rudie Javier Villanueva-Meyer Soonmee Cha Madhura Ingalhalikar Manali Jadhav Umang Pandey Jitender Saini John Garrett Matthew Larson Robert Jeraj Stuart Currie Russell Frood Kavi Fatania Raymond Y Huang Ken Chang Carmen Balaña Jaume Capellades Josep Puig Johannes Trenkler Josef Pichler Georg Necker Andreas Haunschmidt Stephan Meckel Gaurav Shukla Spencer Liem Gregory S Alexander Joseph Lombardo Joshua D Palmer Adam E Flanders Adam P Dicker Haris I Sair Craig K Jones Archana Venkataraman Meirui Jiang Tiffany Y So Cheng Chen Pheng Ann Heng Qi Dou Michal Kozubek Filip Lux Jan Michálek Petr Matula Miloš Keřkovský Tereza Kopřivová Marek Dostál Václav Vybíhal Michael A Vogelbaum J Ross Mitchell Joaquim Farinhas Joseph A Maldjian Chandan Ganesh Bangalore Yogananda Marco C Pinho Divya Reddy James Holcomb Benjamin C Wagner Benjamin M Ellingson Timothy F Cloughesy Catalina Raymond Talia Oughourlian Akifumi Hagiwara Chencai Wang Minh-Son To Sargam Bhardwaj Chee Chong Marc Agzarian Alexandre Xavier Falcão Samuel B Martins Bernardo C A Teixeira Flávia Sprenger David Menotti Diego R Lucio Pamela LaMontagne Daniel Marcus Benedikt Wiestler Florian Kofler Ivan Ezhov Marie Metz Rajan Jain Matthew Lee Yvonne W Lui Richard McKinley Johannes Slotboom Piotr Radojewski Raphael Meier Roland Wiest Derrick Murcia Eric Fu Rourke Haas John Thompson David Ryan Ormond Chaitra Badve Andrew E Sloan Vachan Vadmal Kristin Waite Rivka R Colen Linmin Pei Murat Ak Ashok Srinivasan J Rajiv Bapuraj Arvind Rao Nicholas Wang Ota Yoshiaki Toshio Moritani Sevcan Turk Joonsang Lee Snehal Prabhudesai Fanny Morón Jacob Mandel Konstantinos Kamnitsas Ben Glocker Luke V M Dixon Matthew Williams Peter Zamp Center for Biomedical Image Computing and Analytics (CBICA) University of Pennsylvania Philadelphia PA USA. Department of Radiology Perelman School of Medicine University of Pennsylvania Philadelphia PA USA. Department of Pathology and Laboratory Medicine Perelman School of Medicine University of Pennsylvania Philadelphia PA USA. Department of Informatics Technical University of Munich Munich Bavaria Germany. Intel Corporation Santa Clara CA USA. Department of Neuroradiology Heidelberg University Hospital Heidelberg Germany. Clinical Cooperation Unit Neuropathology German Cancer Consortium (DKTK) within the German Cancer Research Center (DKFZ) Heidelberg Germany. Department of Neuropathology Heidelberg University Hospital Heidelberg Germany. Division of Medical Image Computing German Cancer Research Center Heidelberg Germany. Pattern Analysis and Learning Group Department of Radiation Oncology Heidelberg University Hospital Heidelberg Germany. Neurology Clinic Heidelberg University Hospital Heidelberg Germany. Department of Radiology & Biomedical Imaging University of California San Francisco San Francisco CA USA. Symbiosis Center for Medical Image Analysis Symbiosis International University Pune Maharashtra India. Department of Neuroimaging and Interventional Radiology National Institute of Mental Health and Neurosciences Bangalore Karnataka India. Department of Radiology School of Medicine and Public Health University of Wisconsin Madison WI USA. Department of Medical Physics School of Medicine and Public Health University of Wisconsin Madison WI USA. Leeds Teaching Hospitals Trust Department of Radiology Leeds UK. Department of Radiology Brigham and Women's Hospital Harvard Medical School Boston MA USA. Athinoula A. Martinos Center for Biomedical Imaging Massachusetts General Hospital Charlestown MA USA. Catalan Institute of Oncology Badalona Spain. Consorci MAR Parc de Salut de Barcelona Catalonia Spain. Department of Radiology (IDI

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Multilevel convergence analysis of multigrid-reduction-in-time

arXiv

引用

arXiv 2018年

作者： HESSENTHALER, ANDREAS SOUTHWORTH, BEN S. NORDSLETTEN, DAVID RÖHRLE, OLIVER FALGOUT, ROBERT D. SCHRODER, JACOB B. Institute for Modelling and Simulation of Biomechanical Systems University of Stuttgart Pfaffenwaldring 5a Stuttgart70565 Germany Department of Applied Mathematics University of Colorado at Boulder CO United States Division of Imaging Sciences and Biomedical Engineering King's College London St. Thomas Hospital 4th Floor Lambeth Wing LondonSE1 7EH United Kingdom Center for Applied Scientific Computing Lawrence Livermore National Laboratory P.O. Box 808 L-561 LivermoreCA94551 United States Department of Mathematics and Statistics University of New Mexico 310 SMLC AlbuquerqueNM87131 United States

This paper presents a multilevel convergence framework for multigrid-reduction-intime (MGRIT) as a generalization of previous two-grid estimates. The framework provides a priori upper bounds on the convergence of MGRIT V- and F-cycles, with different relaxation schemes, by deriving the respective residual and error propagation operators. The residual and error operators are functions of the time stepping operator, analyzed directly and bounded in norm, both numerically and analytically. We present various upper bounds of different computational cost and varying sharpness. These upper bounds are complemented by proposing analytic formulae for the approximate convergence factor of V-cycle algorithms that take the number of fine grid time points, the temporal coarsening factors, and the eigenvalues of the time stepping operator as parameters. The paper concludes with supporting numerical investigations of parabolic (anisotropic diffusion) and hyperbolic (wave equation) model problems. We assess the sharpness of the bounds and the quality of the approximate convergence factors. Observations from these numerical investigations demonstrate the value of the proposed multilevel convergence framework for estimating MGRIT convergence a priori and for the design of a convergent algorithm. We further highlight that observations in the literature are captured by the theory, including that two-level Parareal and multilevel MGRIT with F-relaxation do not yield scalable algorithms and the benefit of a stronger relaxation scheme. An important observation is that with increasing numbers of levels MGRIT convergence deteriorates for the hyperbolic model problem, while constant convergence factors can be achieved for the diffusion equation. The theory also indicates that L-stable Runge-Kutta schemes are more amendable to multilevel parallel-in-time integration with MGRIT than A-stable Runge-Kutta schemes. Copyright © 2018, The Authors. All rights reserved.

关键词： Coarsening

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Search for Continuous Gravitational Waves from Known Pulsars in the First Part of the Fourth LIGO-Virgo-KAGRA Observing Run

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Astrophysical Journal 2025年第2期983卷 99-99页

作者： Abac, A.G. Abbott, R. Abouelfettouh, I. Acernese, F. Ackley, K. Adhicary, S. Adhikari, N. Adhikari, R.X. Adkins, V.K. Agarwal, D. Agathos, M. Aghaei Abchouyeh, M. Aguiar, O.D. Aguilar, I. Aiello, L. Ain, A. Ajith, P. Akutsu, T. Albanesi, S. Alfaidi, R.A. Al-Jodah, A. Alléné, C. Allocca, A. Al-Shammari, S. Altin, P.A. Alvarez-Lopez, S. Amato, A. Amez-Droz, L. Amorosi, A. Amra, C. Ananyeva, A. Anderson, S.B. Anderson, W.G. Andia, M. Ando, M. Andrade, T. Andres, N. Andrés-Carcasona, M. Andrić, T. Anglin, J. Ansoldi, S. Antelis, J.M. Antier, S. Aoumi, M. Appavuravther, E.Z. Appert, S. Apple, S.K. Arai, K. Araya, A. Araya, M.C. Areeda, J.S. Argianas, L. Aritomi, N. Armato, F. Arnaud, N. Arogeti, M. Aronson, S.M. Ashton, G. Aso, Y. Assiduo, M. Assis de Souza Melo, S. Aston, S.M. Astone, P. Attadio, F. Aubin, F. AultONeal, K. Avallone, G. Babak, S. Badaracco, F. Badger, C. Bae, S. Bagnasco, S. Bagui, E. Baier, J.G. Baiotti, L. Bajpai, R. Baka, T. Ball, M. Ballardin, G. Ballmer, S.W. Banagiri, S. Banerjee, B. Bankar, D. Baral, P. Barayoga, J.C. Barish, B.C. Barker, D. Barneo, P. Barone, F. Barr, B. Barsotti, L. Barsuglia, M. Barta, D. Bartoletti, A.M. Barton, M.A. Bartos, I. Basak, S. Basalaev, A. Bassiri, R. Basti, A. Bates, D.E. Bawaj, M. Baxi, P. Bayley, J.C. Baylor, A.C. Baynard, P.A. Bazzan, M. Bedakihale, V.M. Beirnaert, F. Bejger, M. Belardinelli, D. Bell, A.S. Benedetto, V. Benoit, W. Bentley, J.D. Ben Yaala, M. Bera, S. Berbel, M. Bergamin, F. Berger, B.K. Bernuzzi, S. Beroiz, M. Bersanetti, D. Bertolini, A. Betzwieser, J. Beveridge, D. Bevins, N. Bhandare, R. Bhardwaj, U. Bhatt, R. Bhattacharjee, D. Bhaumik, S. Bhowmick, S. Bianchi, A. Bilenko, I.A. Billingsley, G. Binetti, A. Bini, S. Birnholtz, O. Biscoveanu, S. Bisht, A. Bitossi, M. Bizouard, M.-A. Blackburn, J.K. Blagg, L.A. Blair, C.D. Blair, D.G. Bobba, F. Bode, N. Boileau, G. Boldrini, M. Bolingbroke, G.N. Bolliand, A. Bonavena, L.D. Bondarescu, R. Bondu, F. Bonilla, E. Bonilla, M.S. Bonino, A. Bonnand, R. Booker, P. Borchers, A. Boschi, V. Bose, S. Boss Max Planck Institute for Gravitational Physics (Albert Einstein Institute) Potsdam D-14476 Germany LIGO Laboratory California Institute of Technology Pasadena 91125 CA United States LIGO Hanford Observatory Richland 99352 WA United States Dipartimento di Farmacia Università di Salerno Fisciano Salerno I-84084 Italy INFN Sezione di Napoli Napoli I-80126 Italy University of Warwick Coventry CV 47AL United Kingdom The Pennsylvania State University University Park 16802 PA United States University of Wisconsin-Milwaukee Milwaukee 53201 WI United States Louisiana State University Baton Rouge 70803 LA United States Université Catholique de Louvain Louvain-la-Neuve B-1348 Belgium Inter-University Centre for Astronomy and Astrophysics Pune 411007 India Queen Mary University of London London E1 4NS United Kingdom Department of Physics and Astronomy Sejong University 209 Neungdong-ro Gwangjin-gu Seoul 143-747 South Korea Instituto Nacional de Pesquisas Espaciais São José dos Campos São Paulo 12227-010 Brazil Stanford University Stanford 94305 CA United States Università di Roma Tor Vergata Roma I-00133 Italy INFN Sezione di Roma Tor Vergata Roma I-00133 Italy Cardiff University Cardiff CF24 3AA United Kingdom Universiteit Antwerpen Antwerpen 2000 Belgium International Centre for Theoretical Sciences Tata Institute of Fundamental Research Bengaluru 560089 India Gravitational Wave Science Project National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka City Tokyo 181-8588 Japan Advanced Technology Center National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka City Tokyo 181-8588 Japan INFN Sezione di Torino Torino I-10125 Italy Theoretisch-Physikalisches Institut Friedrich-Schiller-Universität Jena Jena D-07743 Germany Dipartimento di Fisica Università degli Studi di Torino Torino I-10125 Italy SUPA University of Glasgow Glasgow G12 8QQ United Kingdom OzGrav University of Western Australia Crawley 6009 WA

Continuous gravitational waves (CWs) emission from neutron stars carries information about their internal structure and equation of state, and it can provide tests of general relativity. We present a search for CWs from a set of 45 known pulsars in the first part of the fourth LIGO-Virgo-KAGRA observing run, known as O4a. We conducted a targeted search for each pulsar using three independent analysis methods considering single-harmonic and dual-harmonic emission models. We find no evidence of a CW signal in O4a data for both models and set upper limits on the signal amplitude and on the ellipticity, which quantifies the asymmetry in the neutron star mass distribution. For the single-harmonic emission model, 29 targets have the upper limit on the amplitude below the theoretical spin-down limit. The lowest upper limit on the amplitude is 6.4 × 10^-27 for the young energetic pulsar J0537-6910, while the lowest constraint on the ellipticity is 8.8 × 10^-9 for the bright nearby millisecond pulsar J0437-4715. Additionally, for a subset of 16 targets, we performed a narrowband search that is more robust regarding the emission model, with no evidence of a signal. We also found no evidence of nonstandard polarizations as predicted by the Brans-Dicke theory. © 2025. The Author(s). Published by the American Astronomical Society.

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Classification of crystallization outcomes using deep convolutional neural networks

arXiv

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arXiv 2018年

作者： Bruno, Andrew E. Charbonneau, Patrick Newman, Janet Snell, Edward H. So, David R. Vanhoucke, Vincent Watkins, Christopher J. Williams, Shawn Wilson, Julie Center for Computational Research University at Buffalo BuffaloNY United States Department of Chemistry Duke University DurhamNC United States Department of Physics Duke University DurhamNC United States Collaborative Crystallisation Centre CSIRO ParkvilleVIC Australia Hauptman-Woodward Medical Research Institute and SUNY Buffalo Department of Materials Design and Innovation BuffaloNY14203 United States Google Brain Google Inc. Mountain ViewCA United States IMandT Scientific Computing CSIRO Clayton SouthVIC Australia Platform Technology and Sciences GlaxoSmithKline Inc. CollegevillePA United States Department of Mathematics University of York York United Kingdom

The Machine Recognition of Crystallization Outcomes (MARCO) initiative has assembled roughly half a million annotated images of macromolecular crystallization experiments from various sources and setups. Here, state-of-the-art machine learning algorithms are trained and tested on different parts of this data set. We find that more than 94% of the test images can be correctly labeled, irrespective of their experimental origin. Because crystal recognition is key to high-density screening and the systematic analysis of crystallization experiments, this approach opens the door to both industrial and fundamental research applications. Author summary: Protein crystal growth experiments are routinely imaged, but the mass of accumulated data is difficult to manage and analyze. Using state-of-the-art machine learning algorithms on a large and diverse set of reference images, we manage to recapitulate the labels of a remarkably large fraction of the set. This automation should enable a number of industrial and fundamental applications. Copyright © 2018, The Authors. All rights reserved.

关键词： Deep neural networks

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Existence of a martingale weak solution to the equations of non-stationary motion of non-Newtonian fluids with a stochastic perturbation

arXiv

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arXiv 2017年

作者： Tan, Zhong Wang, Huaqiao Wang, Yucong School of Mathematical Sciences Fujian Provincial Key Laboratory on Mathematical Modeling and Scientific Computing Xiamen University XiamenFujian361005 China Institute of Applied Physics and Computational Mathematics P.O.Box 8009 Beijing100088 China School of Mathematical Sciences Xiamen University Xiamen361005 China

In this paper, we consider the stochastic incompressible non-Newtonian fluids driven by a cylindrical Wiener process W with shear rate dependent on viscosity in a bounded Lipschitz domain D ∈ Rn during the time interval (0, T). For (Formula present) in the growth conditions (1.2), we prove the existence of a martingale weak solution with ∇ · u = 0 by using a pressure decomposition which is adapted to the stochastic setting, the stochastic compactness method and the L∞-truncation. Copyright © 2017, The Authors. All rights reserved.

关键词： Flow measurement

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The CECAM Electronic Structure Library and the modular software development paradigm

arXiv

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arXiv 2020年

作者： Oliveira, Micael J. T. Papior, Nick Pouillon, Yann Blum, Volker Artacho, Emilio Caliste, Damien Corsetti, Fabiano Gironcoli, Stefanode Elena, Alin M. Garca, Alberto Garca-Suarez, Vctor M. Genovese, Luigi Huhn, William P. Huhs, Georg Kokott, Sebastian Kucukbenli, Emine Larsen, Ask H. Lazzaro, Alo Lebedeva, Irina V. Li, Yingzhou Lopez-Duran, David Lopez-Tarifa, Pablo Luders, Martin Marques, Miguel A. L. Minar, Jan Mohr, Stephan Mosto, Arash A. O'Cais, Alan Payne, Mike C. Ruh, Thomas Smith, Daniel G. A. Soler, Jose M. Strubbe, David A. Tancogne-Dejean, Nicolas Tildesley, Dominic Torrent, Marc Wen-Zhe, Victor Max Planck Institute for the Structure and Dynamics of Matter HamburgD-22761 Germany DTU Computing Center Technical University of Denmark Lyngby2800 Denmark Departamento CITIMAC Universidad de Cantabria Santander Spain Simune Atomistics San Sebastian20018 Spain Department of Mechanical Engineering and Materials Science Duke University DurhamNC27708 United States Department of Chemistry Duke University DurhamNC27708 United States CIC Nanogune BRTA DIPC San Sebastian20018 Spain Ikerbasque Basque Foundation for Science Bilbao48011 Spain Theory of Condensed Matter Cavendish Laboratory University of Cambridge CambridgeCB30HE United Kingdom Department of Physics IRIG Univ. Grenoble Alpes CEA GrenobleF-38000 France Departments of Materials and Physics Thomas Young Centre for Theory and Simulation of Materials Imperial College London LondonSW72AZ United Kingdom Synopsys Denmark Copenhagen2100 Denmark Scuola Internazionale Superiore di Studi Avanzati Trieste34136 Italy Scientific Computing Department Daresbury Laboratory WarringtonWA44AD United Kingdom Institut de Ciencia de Materials de Barcelona BellaterraE-08193 Spain Departamento de Fisica Universidad de Oviedo CINN Oviedo33007 Spain Barcelona Supercomputing Center Barcelona08034 Spain Fritz Haber Institut Berlin14195 Germany John A. Paulson School of Engineering and Applied Sciences Harvard University CambridgeMA02138 United States Nano-Bio Spectroscopy Group ETSF Departamento de Fisica de Materiales Universidad Del Pais Vasco San Sebastian20018 Spain Department of Chemistry University of Zurich ZurichCH-8057 Switzerland CIC Nanogune BRTA San Sebastian20018 Spain Department of Mathematics Duke University DurhamNC27708-0320 United States Centro de Fisica de Materiales Centro Mixto CSIC-UPV San Sebastian20018 Spain Institut fur Physik Martin-Luther-Universitat Halle-Wittenberg Halle Saale06120 Germany New Technologies Research Centre University of West Bohemia Plzen3

First-principles electronic structure calculations are now accessible to a very large community of users across many disciplines thanks to many successful software packages, some of which are described in this special issue. The traditional coding paradigm for such packages is monolithic, i.e., regardless of how modular its internal structure may be, the code is built independently from others, essentially from the compiler up, possibly with the exception of linear-algebra and message-passing libraries. This model has endured and been quite successful for decades. The successful evolution of the electronic structure methodology itself, however, has resulted in an increasing complexity and an ever longer list of features expected within all software packages, which implies a growing amount of replication between different packages, not only in the initial coding but, more importantly, every time a code needs to be re-engineered to adapt to the evolution of computer hardware architecture. The Electronic Structure Library (ESL) was initiated by CECAM (the European Centre for Atomic and Molecular Calculations) to catalyze a paradigm shift away from the monolithic model and promote modularization, with the ambition to extract common tasks from electronic structure codes and redesign them as open-source libraries available to everybody. Such libraries include, e.g., \heavy-duty"ones that have the potential for a high degree of parallelisation and adaptation to novel hardware within them, thereby separating the sophisticated computer science aspects of performance optimization and reengineering from the computational science done by, e.g., physicists and chemists when implementing new ideas. We envisage that this modular paradigm will improve overall coding eficiency and enable specialists (whether they be computer scientists or computational scientists) to use their skills more effectively, and will lead to a more dynamic evolution of software in the community as well as

关键词： Libraries

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Galaxy formation efficiency and the multiverse explanation of the cosmological constant with eagle simulations

arXiv

引用

arXiv 2018年

作者： Barnes, Luke A. Elahi, Pascal J. Salcido, Jaime Bower, Richard G. Lewis, Geraint F. Theuns, Tom Schaller, Matthieu Crain, Robert A. Schaye, Joop Sydney Institute for Astronomy School of Physics A28 University of Sydney NSW2006 Australia Western Sydney University School of Computing Engineering and Mathematics Locked Bag 1797 PenrithNSW2751 Australia International Centre for Radio Astronomy Research University of Western Australia 35 Stirling Highway CrawleyWA6009 Australia Institute for Computational Cosmology Department of Physics University of Durham South Road DurhamDH1 3LE United Kingdom Astrophysics Research Institute Liverpool John Moores University 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Leiden Observatory Leiden University P.O. Box 9513 Leiden2300 RA Netherlands

Models of the very early universe, including inflationary models, are argued to produce varying universe domains with different values of fundamental constants and cosmic parameters. Using the cosmological hydrodynamical simulation code from the eagle collaboration,we investigate the effect of the cosmological constant on the formation of galaxies and stars. We simulate universes with values of the cosmological constant ranging from Λ = 0 to Λ0 x300, where Λ0 is the value of the cosmological constant in our Universe. Because the global star formation rate in our Universe peaks at t = 3:5 Gyr, before the onset of accelerating expansion, increases in Λ of even an order of magnitude have only a small effect on the star formation history and efficiency of the universe. We use our simulations to predict the observed value of the cosmological constant, given a measure of the multiverse. Whether the cosmological constant is successfully predicted depends crucially on the measure. The impact of the cosmological constant on the formation of structure in the universe does not seem to be a sharp enough function of Λ to explain its observed value alone. Copyright © 2018, The Authors. All rights reserved.

关键词： Cosmology

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Efficient second order unconditionally stable schemes for a phase-field moving contact line model using invariant energy quadratization approach

arXiv

引用

arXiv 2017年

作者： YANG, XIAOFENG YU, HAIJUN Department of Mathematics University of South Carolina ColumbiaSC29208 United States School of Mathematical Sciences University of Electronic Science and Technology of China Chengdu610054 China NCMIS and LSEC Institute of Computational Mathematics and Scien-tific/Engineering Computing Academy of Mathematics and Systems Science Beijing100190 China School of Mathematical Sciences University of Chinese Academy of Sciences Beijing100049 China

We consider the numerical approximations for a phase field model consisting of incompressible Navier-Stokes equations with a generalized Navier boundary condition, and the Cahn-Hilliard equation with a dynamic moving contact line boundary condition. A crucial and challenging issue for solving this model numerically is the time marching problem, due to the high order, nonlinear and coupled properties of the system. We solve this issue by developing two linear, second-order accurate and energy stable schemes based on the projection method for the Navier-Stokes equations, the invariant energy quadratization for the nonlinear gradient terms in the bulk and boundary, and a subtle implicit-explicit treatment for the stress and convective terms. The well-posedness of the semi-discretized system and the unconditional energy stabilities are proved. Various numerical results based on a spectral-Galerkin spatial discretization are presented to verify the accuracy and efficiency of the proposed *** Codes 65M12, 65Z05, 65P40 Copyright © 2017, The Authors. All rights reserved.

关键词： Viscous flow

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