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arXiv 2018年

作者： Horowitz, C.J. Arcones, A. Cote, B. Dillmann, I. Nazarewicz, W. Roederer, I.U. Schatz, H. Aprahamian, A. Atanasov, D. Bauswein, A. Bliss, J. Brodeur, M. Clark, J.A. Frebel, A. Foucart, F. Hansen, C.J. Just, O. Kankainen, A. McLaughlin, G.C. Kelly, J.M. Liddick, S.N. Lee, D.M. Lippuner, J. Martin, D. Mendoza-Temis, J. Metzger, B.D. Mumpower, M.R. Perdikakis, G. Pereira, J. O'Shea, B.W. Reifarth, R. Rogers, A.M. Siegel, D.M. Spyrou, A. Surman, R. Tang, X. Uesaka, T. Wang, M. Department of Physics Center for the Exploration of Energy and Matter Indiana University BloomingtonIN47405 United States Columbia Astrophysics Laboratory Columbia University New YorkNY10027 United States Department of Physics North Carolina State University RaleighNC27695-8202 United States Department of Physics and Astronomy Michigan State University East LansingMI48864 United States Physics Department University of Notre Dame Notre DameIN46556 United States Institut fur Kernphysik Technische Universitat Darmstadt Schlossgartenstrabe 2 Darmstadt64289 Germany Max-Planck Institute for Nuclear Physics Sapfercheckweg 1 Heidelberg69117 Germany Heidelberg Institute for Theoretical Studies Schloss-Wolfsbrunnenweg 35 Heidelberg69118 Germany Physics Division Argonne National Laboratory ArgonneIL60439 United States TRIUMF 4004 Wesbrook Mall VancouverBCV6T2A3 Canada Department of Physics and Astronomy University of Victoria VictoriaBCV8W2Y2 Canada MIT United States Department of Physics University of New Hampshire DurhamNH03824 United States Dark Cosmology Centre University of Copenhagen Juliane Maries Vej 30 Copenhagen2100 Denmark Max-Planck-Institut fur Astrophysik Karl-Schwarzschild Str. 1 Garching85748 Germany University of Jyvaskyla P.O. Box 35 JyvaskylaFI-40014 Finland Department of Chemistry Michigan State University East LansingMI48864 United States Department of Physics Fisk University NashvilleTN37208 Department of Physics & Astronomy Vanderbilt University NashvilleTN37212 United States Facultad de Fisica Universidad Veracruzana Xalapa Mexico Instituto de Ciencias Nucleares y Centro de Ciencias de la Complejidad Universidad Nacional Autonoma de Mexico Circuito Cultural de Ciudad Universitaria S/N Cd. de Mexico04510 Mexico Theoretical Division Los Alamos National Laboratory Los AlamosNM87545 United States FRIB Laboratory Michigan State University East LansingMI48824 United States Department of Physics Central

This is an exciting time for the study of r-process nucleosynthesis. Recently, a neutron star merger GW170817 was observed in extraordinary detail with gravitational waves and electromagnetic radiation from radio to γ rays. The very red color of the associated kilonova suggests that neutron star mergers are an important r-process site. Astrophysical simulations of neutron star mergers and core collapse supernovae are making rapid progress. Detection of both, electron neutrinos and antineutrinos from the next galactic supernova will constrain the composition of neutrino-driven winds and provide unique nucleosynthesis information. Finally FRIB and other rare-isotope beam facilities will soon have dramatic new capabilities to synthesize many neutron-rich nuclei that are involved in the r-process. The new capabilities can significantly improve our understanding of the r-process and likely resolve one of the main outstanding problems in classical nuclear astrophysics However, to make best use of the new experimental capabilities and to fully interpret the results, a great deal of infrastructure is needed in many related areas of astrophysics, astronomy, and nuclear theory. We will place these experiments in context by discussing astrophysical simulations and observations of r-process sites, observations of stellar abundances, galactic chemical evolution, and nuclear theory for the structure and reactions of very neutron-rich nuclei. This review paper was initiated at a three-week International Collaborations in Nuclear Theory program in June 2016 where we explored promising r-process experiments and discussed their likely impact, and their astrophysical, astronomical, and nuclear theory context. Copyright © 2018, The Authors. All rights reserved.

关键词： Gamma rays

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Characterizations of α-Quasi uniformity and theory of α-P.Q. metrics 6

Characterizations of α-Quasi uniformity and theory of α-P....

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6th International Conference on Fuzzy Information and engineering, ICFIE 2012 and 6th academic conference from Fuzzy Information and engineering Branch of Operation Research Society of China, FIEBORSC 2012

作者： Wu, Xiu-Yun Xie, Li-Li Bai, Shi-Zhong Institute of Computational Mathematics Department of Mathematics Hunan Institute of Science and Engineering Yongzhong425100 China Department of English Teaching Hunan Institute of Science and Engineering Yongzhong425100 China Institute of Mathematics Wuyi university Jiangmen529020 China

ISBN: (纸本)9783642386664

In Wu Fuzzy Systems and mathematics 3:94–99, 2012, the author introduced concepts of α-remote neighborhood mapping and α-quasi uniform, and obtained many good results in α-quasi uniform spaces. This chapter will further investigate properties of α-remote neighborhood mapping, and give some characterizations of α-quasi uniforms. Based on this, this chapter also introduces concept of α-P.Q. metric, and establishes the relations between α-quasi uniforms and α-P.Q. metrics. © Springer-Verlag Berlin Heidelberg 2014.

关键词： Mapping

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Separation axioms in ωα-opos 6

Separation axioms in ωα-opos

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ISBN: (纸本)9783642386664

In this paper, concepts of ωα-Ti, (i = 0, 1, 2, 3, 4) sets are introduced in ωα-order preserving spaces and their characteristic properties are studied. They consist a new complete system of separation axiom, which is proved to be a good extension of both classical and fuzzy theories. Finally, their relationships are established and their differences are discussed by some exact examples. © Springer-Verlag Berlin Heidelberg 2014.

关键词： Soft computing

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Large-scale hydrodynamic brownian simulations on multicore and GPU architectures 14

Large-scale hydrodynamic brownian simulations on multicore a...

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2014 Annual Conference on Extreme science and engineering Discovery Environment, XSEDE 2014

作者： Lopez, M. Graham Horton, Mitchel D. Chow, Edmond School of Computational Science and Engineering College of Computing Georgia Institute of Technology Atlanta GA 30332 United States

ISBN: (纸本)9781450328937

We present here ongoing work to produce an implementation of Brownian dynamics simulation using a matrix-free method with hardware accelerators. This work describes the GPU acceleration of a smooth particle-mesh Ewald (SPME) algorithm which is used for the main part of the computation, previously ported to run on Intel Xeon Phi. Copyright 2014 ACM.

关键词： Graphics processing unit

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Hydrodynamic Interaction of Elastic Capsules in Bounded Shear Flow

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Communications in computational Physics 2014年第9期16卷 1031-1055页

作者： D.V.Le Zhijun Tan Institute of High Performance Computing Agency for ScienceTechnology and Research1 Fusionopolis Way#16-16 ConnexisSingapore 138632 School of Mathematics and Computational Science Sun Yat-sen UniversityGuangzhou 510275China Province Key Laboratory of Computational Science Sun Yat-sen UniversityGuangzhou 510275China.

This paper presents a modified Loop’s subdivision algorithm for studying the deformation of a single capsule,the hydrodynamic interaction between two capsules and the hydrodynamic diffusion of a suspension of capsules in bounded shear flow.A subdivision thin-shell model is employed to compute the forces generated on the surface of the elastic capsule during *** capsule surface is approximated using the modified Loop’s subdivision scheme which guarantees bounded curvature and C1 continuity everywhere on the limit *** present numerical technique has been validated by studying the deformation of a spherical capsule in shear *** are also performed for a biconcave capsule over a wide range of shear rates and viscosity ratios to investigate its *** addition,the hydrodynamic interaction between two elastic capsules in bounded shear flow is *** on the wall separation distance,the trajectory-bifurcation points that separate reversing and crossing motions for both spherical and biconcave capsules can be *** to the spherical capsules,the biconcave capsules exhibit additional types of interaction such as rotation and head-on *** head-on collision results in a large trajectory shift which contribute to the hydrodynamic diffusion of a suspension.A suspension of a large number of biconcave capsules in shear flow is also simulated to show the ability of the modified scheme in running a large-scale simulation over a long period of time.

关键词： Thin shell elastic capsules red-blood cells subdivision surfaces immersed boundary method Navier-Stokes equations.

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324. Sensitivity and specificity of fractal analysis to distinguish between healthy and pathological rectal mucosa microvasculature seen during colonoscopy

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European Journal of Surgical Oncology 2016年第9期42卷 S147-S148页

作者： Henry, B.M. Taterra, D. Gryglewski, A. Mrozek, M. Zelawski, M. Piech, K. Tomaszewski, K.A. Jagiellonian University Medical College Department of Anatomy Krakow Poland Jagiellonian University Medical College First Department of General- Oncological and Gastrointestinal Surgery Krakow Poland Jagiellonian University Institute of Computer Science Krakow Poland Jagiellonian University Chair of Computational Mathematics Krakow Poland AGH University of Science and Technology Faculty of Electrical Engineering- Automatics- Computer Science and Biomedical Engineering Krakow Poland

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The tess-hermes survey data release 1: High-resolution spectroscopy of the tess southern continuous viewing zone

arXiv

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arXiv 2017年

作者： Sharma, Sanjib Stello, Dennis Buder, Sven Kos, Janez Bland-Hawthorn, Joss Asplund, Martin Duong, Ly Lin, Jane Lind, Karin Ness, Melissa Huber, Daniel Zwitter, Tomaz Traven, Gregor Hon, Marc Kafle, Prajwal R. Khanna, Shourya Saddon, Hafiz Anguiano, Borja Casey, Andrew R. Freeman, Ken Martell, Sarah Silva, Gayandhi M.D.E. Simpson, Jeffrey D. Wittenmyer, Rob A. Zucker, Daniel B. Sydney Institute for Astronomy School of Physics University of Sydney NSW2006 Australia School of Physics University of New South Wales SydneyNSW2052 Australia Stellar Astrophysics Centre Department of Physics and Astronomy Aarhus University Aarhus CDK-8000 Denmark Koenigstuhl 17 HeidelbergD-69117 Fellow of the International Max Planck Research School for Astronomy & Cosmic Physics University of Heidelberg Research School of Astronomy & Astrophysics Australian National University ACT2611 Australia Department of Physics and Astronomy Uppsala University Box 516 UppsalaSE-751 20 Sweden Institute for Astronomy University of Hawai‘i 2680 Woodlawn Drive HonoluluHI96822 United States School of Physics University of Sydney NSW2006 Australia SETI Institute 189 Bernardo Avenue Mountain ViewCA94043 United States Stellar Astrophysics Centre Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark Faculty of Mathematics and Physics University of Ljubljana Jadranska 19 Ljubljana1000 Slovenia University of Western Australia 35 Stirling Highway CrawleyWA6009 Australia Department of Astronomy University of Virginia CharlottesvilleVA22904-4325 United States Department of Physics & Astronomy Macquarie University SydneyNSW2109 Australia School of Physics & Astronomy Monash University ClaytonVIC3800 Australia Faculty of Information Technology Monash University ClaytonVIC3800 Australia Australian Astronomical Observatory 105 Delhi Rd North RydeNSW2113 Australia University of Southern Queensland Computational Engineering and Science Research Centre ToowoombaQLD4350 Australia Research Centre in Astronomy Astrophysics & Astrophotonics Macquarie University SydneyNSW2109 Australia

The Transiting Exoplanet Survey Satellite (TESS) will provide high precision time-series photometry for millions of stars with at least a half-hour cadence. Of particular interest are the circular regions of 12-degree radius centered around the ecliptic poles that will be observed continuously for a full year. Spectroscopic stellar parameters are desirable to characterize and select suitable targets for TESS, whether they are focused on exploring exoplanets, stellar astrophysics, or Galactic archaeology. Here, we present spectroscopic stellar parameters (Teff, log g, [Fe/H], vsin i, vmicro) for about 16,000 dwarf and subgiant stars in TESS’ southern continuous viewing zone. For almost all the stars, we also present Bayesian estimates of stellar properties including distance, extinction, mass, radius, and age using theoretical isochrones. Stellar surface gravity and radius are made available for an additional set of roughly 8,500 red giants. All our target stars are in the range 10 V 13.1. Among them, we identify and list 227 stars belonging to the Large Magellanic Cloud. The data were taken using the the High Efficiency and Resolution Multi-Element Spectrograph (HERMES, R ∼ 28, 000) at the Anglo-Australian Telescope as part of the TESS-HERMES survey. Comparing our results with the TESS Input Catalog (TIC) shows that the TIC is generally efficient in separating dwarfs and giants, but it has flagged more than hundred cool dwarfs (Teff 4800 K) as giants, which ought to be high-priority targets for the exoplanet search. The catalog can be accessed via http://***/tess-hermes/, or at MAST. Copyright © 2017, The Authors. All rights reserved.

关键词： Surveys

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FlashGraph: processing billion-node graphs on an array of commodity SSDs 15

FlashGraph: processing billion-node graphs on an array of co...

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Proceedings of the 13th USENIX Conference on File and Storage Technologies

作者： Da Zheng Disa Mhembere Randal Burns Joshua Vogelstein Carey E. Priebe Alexander S. Szalay Department of Computer Science Johns Hopkins University Institute for Computational Medicine Department of Biomedical Engineering Johns Hopkins University Department of Applied Mathematics and Statistics Johns Hopkins University Department of Physics and Astronomy Johns Hopkins University

ISBN: (纸本)9781931971201

Graph analysis performs many random reads and writes, thus, these workloads are typically performed in memory. Traditionally, analyzing large graphs requires a cluster of machines so the aggregate memory exceeds the graph size. We demonstrate that a multicore server can process graphs with billions of vertices and hundreds of billions of edges, utilizing commodity SSDs with minimal performance loss. We do so by implementing a graph-processing engine on top of a user-space SSD file system designed for high IOPS and extreme parallelism. Our semi-external memory graph engine called FlashGraph stores vertex state in memory and edge lists on SSDs. It hides latency by overlapping computation with I/O. To save I/O bandwidth, FlashGraph only accesses edge lists requested by applications from SSDs; to increase I/O throughput and reduce CPU overhead for I/O, it conservatively merges I/O requests. These designs maximize performance for applications with different I/O characteristics. FlashGraph exposes a general and flexible vertex-centric programming interface that can express a wide variety of graph algorithms and their optimizations. We demonstrate that FlashGraph in semi-external memory performs many algorithms with performance up to 80% of its in-memory implementation and significantly outperforms PowerGraph, a popular distributed in-memory graph engine.

关键词：

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Laser interferometric gravitational wave detection in space and structure formation in the early universe

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Chinese Astronomy and Astrophysics 2015年第4期39卷 411-446页

作者： Gong, Xue-Fei Xu, Sheng-Nian Yuan, Ye-Fei Bai, Shan Bian, Xing Cao, Zhou-Jian Chen, Ge-Rui Dong, Peng Gao, Tian-Shu Gao, Wei Huang, Shuang-Lin Luo, Zi-Ren Shao, Ming-Xue Sun, Bao-San Tang, Wen-Lin Yu, Pin Xu, Peng Zang, Yun-Long Zhang, Hai-Peng Lau, Yun-Kau Academy of Mathematics and Systems Science Chinese Academy of Sciences Beijing 100190 China University of Science and Technology of China Department of Astronomy Hefei 230026 China Theoretisch-Physikalisches Institut Friedrich-Schiller-Universität Jena Jena D-07743 Germany University of Chinese Academy of Sciences Beijing 100049 China State Key Laboratory of Scientific and Engineering Computing Academy of Mathematics and Systems Science Chinese Academy of Sciences Beijing 100190 China State Key Laboratory of Theoretical Physics Institute of Theoretical Physics Chinese Academy of Sciences Beijing 100190 China Beijing University of Technology College of Applied Sciences Beijing 100124 China Morningside Center of Mathematics Chinese Academy of Sciences Beijing 100190 China Capital Normal University Beijing 100089 China Henan University Department of Mathematics Kaifeng 475001 China Institute of Mechanics Chinese Academy of Sciences Beijing 100190 China Henan Polytechnic University Jiaozuo Henan 454000 China Huazhong University of Science and Technology School of Physics Wuhan 430074 China Tshinghua University Mathematical Sciences Center Beijing 100083 China Institute of Theoretical Physics Chinese Academy of Sciences Beijing 100190 China

The laser interferometric gravitational wave detection in space is an important and realistic approach to studying some key problems of astronomy and cosmology, such as the stellar evolution and galactic formation in the early universe, the co-evolution of black holes and galaxies, etc. After performing two stages of the Advance Research Project of Space science commissioned by the Chinese Academy of sciences, and by weighing the feasibility of technology and the foresight of science, we have selected the gravitational wave sources including the high-redshift intermediate-and-large mass binary black hole mergers, and the intermediate-mass black holes in clusters and other dense dynamic environments, as the main scientific objectives, and given a preliminary design for the project of Chinese space gravitational wave detection in the frequency range from millihertz to hertz. Based on this, here we introduce briefly the science of the space gravitational wave detection, as a new measure of astronomical observations, as well as the scientific objectives and potential detectivity of the design for the Chinese space gravitational wave detection mission.

关键词： Binary black hole coalescence Gravitational wave intermediate mass black hole ΛCDM hierarchical structure formation picture

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Bs → Kν form factors with 2+1 flavors

arXiv

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arXiv 2017年

作者： Liu, Yuzhi Bailey, Jon A. Bazavov, A. Bernard, C. Bouchard, C.M. DeTar, C. Du, Daping El-Khadra, A.X. Freeland, E.D. Gámiz, E. Gelzer, Z. Gottlieb, Steven Heller, U.M. Kronfeld, A.S. Laiho, J. Mackenzie, P.B. Meurice, Y. Neil, E.T. Simone, J.N. Sugar, R. Toussaint, D. van de Water, R.S. Zhou, Ran Department of Physics Indiana University BloomingtonIN47405 United States Department of Physics and Astronomy Seoul National University Seoul Korea Republic of Department of Computational Mathematics Science and Engineering Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Department of Physics Washington University St. LouisMO63130 United States School of Physics and Astronomy University of Glasgow GlasgowG12 8QQ United Kingdom Department of Physics and Astronomy University of Utah Salt Lake CityUT84112 United States Department of Physics Syracuse University SyracuseNY13244 United States Department of Physics University of Illinois UrbanaIL61801 United States Fermi National Accelerator Laboratory BataviaIL60510 United States School of the Art Institute of Chicago ChicagoIL60603 United States CAFPE Departamento de Física Teórica y del Cosmos Universidad de Granada Granada Spain Department of Physics and Astronomy University of Iowa Iowa CityIA52242 United States American Physical Society RidgeNY11961 United States Institute for Advanced Study Technische Universität München GarchingD-85748 Germany Department of Physics University of Colorado BoulderCO80309 United States RIKEN-BNL Research Center Brookhaven National Laboratory UptonNY11973 United States Department of Physics University of California Santa BarbaraCA93106 United States Department of Physics University of Arizona TucsonAZ85721 United States

Using the MILC 2+1 flavor asqtad quark action ensembles, we are calculating the form factors f0 and f+ for the semileptonic Bs → Kν decay. A total of six ensembles with lattice spacing from ≈ 0.12 to 0.06 fm are being used. At the coarsest and finest lattice spacings, the light quark mass m′l is one-tenth the strange quark mass m′s. At the intermediate lattice spacing, the ratio m′l/m′s ranges from 0.05 to 0.2. The valence b quark is treated using the Sheikholeslami-Wohlert Wilson-clover action with the Fermilab interpretation. The other valence quarks use the asqtad action. When combined with (future) measurements from the LHCb and Belle II experiments, these calculations will provide an alternate determination of the CKM matrix element |Vub|. Copyright © 2017, The Authors. All rights reserved.

关键词： Elementary particles

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