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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.

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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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H_∞ group consensus for clusters of agents with model uncertainty and external disturbance

H_∞ group consensus for clusters of agents with model uncer...

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IEEE Annual Conference on Decision and Control

作者： Jiahu Qin Qichao Ma Wei Xing Zheng Huijun Gao Department of Automation University of Science and Technology of China Hefei 230027 China School of Computing Engineering and Mathematics Western Sydney University Sydney NSW 2751 Australia Research Institute of Intelligent Control and Systems Harbin Institute of Technology Harbin 150001 China

ISBN: (纸本)9781479978878

In this paper, the problem of H_∞ group consensus is addressed for networks of agents modeled by single-integrator with model uncertainty and external disturbance. The first part of the work is to show that the group consensus with desired H_∞ performance can be achieved under some sufficient conditions that are established in terms of the structure and strength of the couplings among agents. Then given the observation that the theoretical values of the coupling strengths are usually much larger than expected in practical situations, the second part of the work is concerned with developing an adaptation law to tackle such coupling strength problem.

关键词： model uncertainty external disturbance Agents theoretical value Couplings Sufficient conditions

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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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Generalized Lenard-Balescu calculations of electron-ion temperature relaxation in beryllium plasma

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Physical Review E 2015年第3期92卷 033103-033103页

作者： Zhen-Guo Fu Zhigang Wang Da-Fang Li Wei Kang Ping Zhang Research Center for Fusion Energy Science and Technology China Academy of Engineering Physics Beijing 100088 People's Republic of China Institute of Applied Physics and Computational Mathematics Beijing 100088 People's Republic of China Center for Applied Physics and Technology Peking University Beijing 100871 People's Republic of China

The problem of electron-ion temperature relaxation in beryllium plasma at various densities (0.185–18.5g/cm3) and temperatures [(1.0–8)×103 eV] is investigated by using the generalized Lenard-Balescu theory. We consider the correlation effects between electrons and ions via classical and quantum static local field corrections. The numerical results show that the electron-ion pair distribution function at the origin approaches the maximum when the electron-electron coupling parameter equals unity. The classical result of the Coulomb logarithm is in agreement with the quantum result in both the weak (Γee<10−2) and strong (Γee>1) electron-electron coupling ranges, whereas it deviates from the quantum result at intermediate values of the coupling parameter (10−2<Γee<1). We find that with increasing density of Be, the Coulomb logarithm will decrease and the corresponding relaxation rate νie will increase. In addition, a simple fitting law νie/νie(0)=a(ρBe/ρ0)b is determined, where νie0 is the relaxation rate corresponding to the normal metal density of Be and ρ0, a, and b are the fitting parameters related to the temperature and the degree of ionization Z of the system. Our results are expected to be useful for future inertial confinement fusion experiments involving Be plasma.

关键词： ELECTRON impact ionization BERYLLIUM ION temperature ELECTRON-electron interactions COULOMB functions

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Supernovae 2016bdu and 2005gl, and their link with SN 2009ip-like transients: another piece of the puzzle

arXiv

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arXiv 2017年

作者： Pastorello, A. Kochanek, C.S. Fraser, M. Dong, S. Elias-Rosa, N. Benetti, S. Cappellaro, E. Tomasella, L. Drake, A.J. Hermanen, J. Reynolds, T. Shappee, B.J. Smartt, S.J. Chambers, K.C. Huber, M.E. Smith, K. Stanek, K.Z. Filippenko, A.V. Christensen, E.J. Denneau, L. Djorgovski, S.G. Flewelling, H. Gall, C. Gal-Yam, A. Geier, S. Heinze, A. Holoien, T.W.-S. Isern, J. Kangas, T. Kankare, E. Koff, R.A. Llapasset, J.-M. Lowe, T.B. Lundqvist, P. Magnier, E.A. Mattila, S. Morales-Garoffolo, A. Mutel, R. Nicolas, J. Ochner, P. Ofek, E.O. Prosperi, E. Rest, A. Sano, Y. Stalder, B. Stritzinger, M.D. Taddia, F. Terreran, G. Tonry, J.L. Wainscoat, R.J. Waters, C. Weiland, H. Willman, M. Young, D.R. Zheng, W. INAF-Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 PadovaI-35122 Italy Department of Astronomy Ohio State University 140 West 18th Avenue ColumbusOH43210 United States Ohio State University 191 W. Woodruff Ave. ColumbusOH43210 United States School of Physics O’Brien Centre for Science North University College Dublin Belfield Dublin 4 Ireland Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Royal Society – Science Foundation Ireland University Research Fellow Kavli Institute for Astronomy and Astrophysics Peking University Yi He Yuan Road 5 Hai Dian District Beijing100871 China Astronomy Department California Institute of Technology PasadenaCA91125 United States Tuorla Observatory Department of Physics and Astronomy University of Turku Väisäläntie 20 PiikkiöFI-21500 Finland Nordic Optical Telescope Apartado 474 Santa Cruz de La PalmaE-38700 Spain Carnegie Observatories 813 Santa Barbara Street PasadenaCA91101 United States Hubble Fellow and Carnegie-Princeton Fellow Astrophysics Research Centre School of Mathematics and Physics Queen’s University Belfast BelfastBT7 1NN United Kingdom Institute for Astronomy University of Hawaii 2680 Woodlawn Drive HonoluluHI96822 United States Department of Astronomy University of California BerkeleyCA94720-3411 United States Lunar and Planetary Lab Department of Planetary Sciences University of Arizona TucsonAZ85721 United States Dark Cosmology Centre Niels Bohr Institute University of Copenhagen Juliane Maries Vej 30 Copenhagen2100 Denmark Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark Department of Particle Physics and Astrophysics Faculty of Physics Weizmann Institute of Science Rehovot76100 Israel Cuesta de San José s/n Breña Baja La PalmaE-38712 Spain Instituto de Astrofísica de Canarias Vía Láctea s/n La Laguna TenerifeE-38200 Spain US Department of Energy Computatio

Supernova (SN) 2016bdu is an unusual transient resembling SN 2009ip. SN 2009ip-like events are characterized by a long-lasting phase of erratic variability which ends with two luminous outbursts a few weeks apart. The second outburst is significantly more luminous (about 3 mag) than the first. In the case of SN 2016bdu, the first outburst (Event A) reached an absolute magnitude Mr ≈ −15.3 mag, while the second one (Event B) occurred over one month later and reached Mr ≈ −18 mag. By inspecting archival data, a faint source at the position of SN 2016bdu is detectable several times in the past few years. We interpret these detections as signatures of a phase of erratic variability, similar to that experienced by SN 2009ip between 2008 and mid-2012, and resembling the currently observed variability of the luminous blue variable SN 2000ch in NGC 3432. Spectroscopic monitoring of SN 2016bdu during the second peak initially shows features typical of a SN IIn. One month after the Event B maximum, the spectra develop broad Balmer lines with P Cygni profiles and broad metal features. At these late phases, the spectra resemble those of a typical Type II SN. All members of this SN 2009ip-like group are remarkably similar to the Type IIn SN 2005gl. For this object, the claim of a terminal SN explosion is supported by the disappearance of the progenitor star. The similarity with SN 2005gl suggests that all members of this family may finally explode as genuine SNe, although the unequivocal detection of nucleosynthesised elements in their nebular spectra is still missing. Copyright © 2017, The Authors. All rights reserved.

关键词： Supernovae

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A POSTERIORI ERROR ESTIMATES FOR LOCAL CO DISCONTINUOUS GALERKIN METHODS FOR KIRCHHOFF PLATE BENDING PROBLEMS

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Journal of computational mathematics 2014年第6期32卷 665-686页

作者： Yifeng Xu Jianguo Huang Xuehai Huang Department of Mathematics Shanghai Normal University Shanghai 200234 ChinaDivision of Computational Science E-Institute of Shanghai Universities Shanghai Normal University Shanghai 200234 China Scientific Computing Key Laboratory of Shanghai Universities Shanghai Normal University Shanghai 200234 China Department of Mathematics MOE-LSC Shanghai Jiao Tong University Shanghai 200240 China Division of Computational Science E-Institute of Shanghai Universities Shanghai Normal University Shanghai 200234 China College of Mathematics and Information Science Wenzhou University Wenzhou 325035 China Email: xuehaihuang@wzu edu. cn

We derive some residual-type a posteriori error estimates for the local CO discontinuous Galerkin （LCDG） approximations （[31]） of the Kirchhoff bending plate clamped on the boundary. The estimator is both reliable and efficient with respect to the moment-field approximation error in an energy norm. Some numerical experiments are reported to demonstrate theoretical results.

关键词： Kirchhoff bending plate Discontinuous Galerkin method A posteriori erroranalysis.

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Creation and analysis of biochemical constraint-based models: The COBRA Toolbox v3.0

arXiv

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arXiv 2017年

作者： Heirendt, Laurent Arreckx, Sylvain Pfau, Thomas Mendoza, Sebastián N. Richelle, Anne Heinken, Almut Haraldsdóttir, Hulda S. Wachowiak, Jacek Keating, Sarah M. Vlasov, Vanja Magnusdóttir, Stefania Ng, Chiam Yu Preciat, German Žagare, Alise Chan, Siu H.J. Aurich, Maike K. Clancy, Catherine M. Modamio, Jennifer Sauls, John T. Noronha, Alberto Bordbar, Aarash Cousins, Benjamin El Assal, Diana C. Valcarcel, Luis V. Apaolaza, Iñigo Ghaderi, Susan Ahookhosh, Masoud Guebila, Marouen Ben Kostromins, Andrejs Sompairac, Nicolas Le, Hoai M. Ma, Ding Sun, Yuekai Wang, Lin Yurkovich, James T. Oliveira, Miguel A.P. Vuong, Phan T. El Assal, Lemmer P. Kuperstein, Inna Zinovyev, Andrei Scott Hinton, H. Bryant, William A. Aragón Artacho, Francisco J. Planes, Francisco J. Stalidzans, Egils Maass, Alejandro Vempala, Santosh Hucka, Michael Saunders, Michael A. Maranas, Costas D. Lewis, Nathan E. Sauter, Thomas Palsson, Bernhard Ø. Thiele, Ines Fleming, Ronan M.T. Luxembourg Centre for Systems Biomedicine University of Luxembourg 6 avenue du Swing BelvauxL-4367 Luxembourg Life Sciences Research Unit University of Luxembourg 6 avenue du Swing BelvauxL-4367 Luxembourg University of Chile Blanco Encalada 2085 Santiago Chile Department of Pediatrics University of California San Diego School of Medicine San DiegoCA92093 United States Hinxton CambridgeCB10 1SD United Kingdom Department of Chemical Engineering Pennsylvania State University University University ParkPA16802 United States Department of Physics University of California San Diego 9500 Gilman Dr. San DiegoCA92093 United States Bioinformatics and Systems Biology Program University of California San Diego San DiegoCA United States Sinopia Biosciences San DiegoCA United States School of Computer Science Algorithms and Randomness Center Georgia Institute of Technology AtlantaGA United States Biomedical Engineering and Sciences Department TECNUN University of Navarra Paseo de Manuel Lardizabal 13 San Sebastian20018 Spain Institute of Microbiology and Biotechnology University of Latvia Jelgavas iela 1 RigaLV-1004 Latvia Department of Management Science and Engineering Stanford University StanfordCA94305-4026 United States Bioengineering Department University of California San Diego San DiegoCA United States Utah State University Research Foundation 1695 North Research Park Way North LoganUT84341 United States Centre for Integrative Systems Biology and Bioinformatics Department of Life Sciences Imperial College London London United Kingdom Department of Mathematics University of Alicante Spain California Institute of Technology Computing and Mathematical Sciences MC 305-16 1200 E. California Blvd. PasadenaCA91125 United States Mathomics Center for Mathematical Modeling University of Chile Beauchef 851 Santiago Chile Novo Nordisk Foundation Center for Biosustainability University of California San Diego San DiegoCA92093 Uni

COnstraint-Based Reconstruction and Analysis (COBRA) provides a molecular mechanistic framework for integrative analysis of experimental data and quantitative prediction of physicochemically and biochemically feasible phenotypic states. The COBRA Toolbox is a comprehensive software suite of interoperable COBRA methods. It has found widespread applications in biology, biomedicine, and biotechnology because its functions can be flexibly combined to implement tailored COBRA protocols for any biochemical network. Version 3.0 includes new methods for quality controlled reconstruction, modelling, topological analysis, strain and experimental design, network visualisation as well as network integration of chemoinformatic, metabolomic, transcriptomic, proteomic, and thermochemical data. New multi-lingual code integration also enables an expansion in COBRA application scope via high-precision, high-performance, and nonlinear numerical optimisation solvers for multi-scale, multi-cellular and reaction kinetic modelling, respectively. This protocol can be adapted for the generation and analysis of a constraint-based model in a wide variety of molecular systems biology scenarios. This protocol is an update to the COBRA Toolbox 1.0 and 2.0. The COBRA Toolbox 3.0 provides an unparalleled depth of constraint-based reconstruction and analysis methods. Copyright © 2017, The Authors. All rights reserved.

关键词： Data integration

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On the Effect of Ghost Force in the Quasicontinuum Method:Dynamic Problems in One Dimension

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Communications in computational Physics 2014年第3期15卷 647-676页

作者： Xiantao Li Pingbing Ming Department of Mathematics the Pennsylvania State UniversityUniversity ParkPennsylvania16802USA LSEC Institute of Computational Mathematics and Scientific/Engineering ComputingAMSSChinese Academy of SciencesNo.55East Road Zhong-Guan-CunBeijing100190P.R.China

Numerical error caused by“ghost forces”in a quasicontinuum method is studied in the context of dynamic *** error in the discrete W^(1,∞)norm is analyzed for the time scale O(ε)and the time scale O(1)withεbeing th... 详细信息

关键词： Quasicontinuum methods ghost force dynamic problems

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