检索结果-内蒙古大学图书馆

Antiferromagnetic nano-oscillator in external magnetic fields

Physical Review B 2017年第17期96卷 174438-174438页

作者： Jakub Chęciński Marek Frankowski Tomasz Stobiecki AGH University of Science and Technology Department of Electronics Al. Mickiewicza 30 30-059 Kraków Poland AGH University of Science and Technology Faculty of Physics and Applied Computer Science Al. Mickiewicza 30 30-059 Kraków Poland

We describe the dynamics of an antiferromagnetic nano-oscillator in an external magnetic field of any given time distribution. The oscillator is powered by a spin current originating from spin-orbit effects in a neighboring heavy metal layer and is capable of emitting a THz signal in the presence of an additional easy-plane anisotropy. We derive an analytical formula describing the interaction between such a system and an external field, which can affect the output signal character. Interactions with magnetic pulses of different shapes, with a sinusoidal magnetic field and with a sequence of rapidly changing magnetic fields are discussed. We also perform numerical simulations based on the Landau-Lifshitz-Gilbert equation with spin-transfer torque effects to verify the obtained results and find a very good quantitative agreement between analytical and numerical predictions.

关键词： Antiferromagnetism Spin transfer torque Antiferromagnets Landau-Lifschitz-Gilbert equation

来源：评论

学校读者我要写书评

暂无评论

From the Fire: A Deeper Look at the Phoenix Stream

arXiv

引用

arXiv 2021年

作者： Tavangar, Kiyan Ferguson, P. Shipp, N. Drlica-Wagner, A. Koposov, S. Erkal, D. Balbinot, E. García-Bellido, J. Kuehn, K. Lewis, G.F. Li, T.S. Mau, S. Pace, A.B. Riley, A.H. Abbott, T.M.C. Aguena, M. Allam, S. Andrade-Oliveira, F. Annis, J. Bertin, E. Burke, D.L. Brooks, D. Rosell, A. Carnero Kind, M. Carrasco Carretero, J. Costanzi, M. Pereira, M.E.S. De Vicente, J. Diehl, H.T. Everett, S. Ferrero, I. Flaugher, B. Frieman, J. Da Costa, L.N. Gaztanaga, E. Gerdes, D.W. Gruen, D. Gruendl, R.A. Gschwend, J. Gutierrez, G. Hinton, S.R. Hollowood, D.L. Honscheid, K. James, D.J. Kuropatkin, N. Maia, M.A.G. Marshall, J.L. Menanteau, F. Miquel, R. Morgan, R. Ogando, R.L.C. Palmese, A. Paz-Chinchón, F. Pieres, A. Malagón, A.A. Plazas Rodriguez-Monroy, M. Sanchez, E. Scarpine, V. Serrano, S. Sevilla-Noarbe, I. Smith, M. Suchyta, E. Swanson, M.E.C. Tarle, G. To, C. Varga, T.N. Walker, A.R. Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Physics Department 2320 Chamberlin Hall University of Wisconsin−Madison 1150 University Avenue MadisonWI53706-1390 United States George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Department of Physics and Astronomy Texas A&M University College StationTX77843 United States MIT Kavli Institute for Astrophysics and Space Research 77 Massachusetts Ave. CambridgeMA02139 United States Fermi National Accelerator Laboratory P.O. Box 500 BataviaIL60510 United States Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Department of Physics University of Surrey GuildfordGU2 7XH United Kingdom Kapteyn Astronomical Institute University of Groningen Postbus 800 GroningenNL-9700AV Netherlands Instituto de Fisica Teorica UAM CSIC Universidad Autonoma de Madrid MadridE-28049 Spain Lowell Observatory 1400 Mars Hill Rd. FlagstaffAZ86001 United States Australian Astronomical Optics Macquarie University North RydeNSW2113 Australia Sydney Institute for Astronomy School of Physics A28 The University of Sydney NSW2006 Australia Department of Astronomy and Astrophysics University of Toronto 50 St. George Street TorontoONM5S 3H4 Canada Observatories of the Carnegie Institution for Science 813 Santa Barbara St. PasadenaCA91101 United States Department of Astrophysical Sciences Princeton University Princeton NJ08544 United States Department of Physics Stanford University 382 Via Pueblo Mall StanfordCA94305 United States Kavli Institute for Particle Astrophysics & Cosmology

We use 6 yr of data from the Dark Energy Survey to perform a detailed photometric characterization of the Phoenix stellar stream, a 15° long, thin, dynamically cold, low-metallicity stellar system in the Southern Hemisphere. We use natural splines, a nonparametric modeling technique, to simultaneously fit the stream track, width, and linear density. This updated stream model allows us to improve measurements of the heliocentric distance (17.4 ± 0.1 (stat.) ± 0.8 (sys.) kpc) and distance gradient (−0.009 ± 0.006 kpc deg−1) of Phoenix, which corresponds to a small change of 0.13 ± 0.09 kpc in heliocentric distance along the length of the stream. We measure linear intensity variations on degree scales, as well as deviations in the stream track on ∼2° scales, suggesting that the stream may have been disturbed during its formation and/or evolution. We recover three peaks and one gap in linear intensity along with fluctuations in the stream track. Compared to other thin streams, the Phoenix stream shows more fluctuations and, consequently, the study of Phoenix offers a unique perspective on gravitational perturbations of stellar streams. We discuss possible sources of perturbations to Phoenix, including baryonic structures in the Galaxy and dark matter subhalos. © 2021, CC BY.

关键词： Galaxies

来源：评论

学校读者我要写书评

暂无评论

Superconductor-insulator transition driven by pressure-tuned intergrain coupling in nanodiamond films

引用

Physical Review Materials 2019年第3期3卷 034801-034801页

作者： Gufei Zhang Yonghui Zhou Svetlana Korneychuk Tomas Samuely Liwang Liu Paul W. May Zheng Xu Oleksandr Onufriienko Xuefeng Zhang Johan Verbeeck Peter Samuely Victor V. Moshchalkov Zhaorong Yang Horst-Günter Rubahn NanoSYD Mads Clausen Institute and DIAS Danish Institute for Advanced Study University of Southern Denmark Alsion 2 DK-6400 Sonderborg Denmark Anhui Province Key Laboratory of Condensed Matter Physics at Extreme Conditions High Magnetic Field Laboratory Chinese Academy of Sciences Hefei 230031 China EMAT University of Antwerp Groenenborgerlaan 171 B-2020 Antwerp Belgium Centre of Low Temperature Physics Institute of Experimental Physics Slovak Academy of Sciences & Faculty of Science P. J. Safarik University Kosice Slovakia Laboratory for Soft Matter and Biophysics Department of Physics and Astronomy KU Leuven B-3001 Heverlee Belgium School of Chemistry University of Bristol Bristol BS8 1TS United Kingdom School of Electrical and Computer Engineering University of California Davis California 95616 USA Innovative Center for Advanced Materials Hangzhou Dianzi University 310012 Hangzhou China Institute for Nanoscale Physics and Chemistry KU Leuven B-3001 Heverlee Belgium Collaborative Innovation Center of Advanced Microstructures Nanjing University Nanjing 210093 China Institute of Physical Science and Information Technology Anhui University Hefei 230601 China

We report on the pressure-driven superconductor-insulator transition in heavily boron-doped nanodiamond films. By systematically increasing the pressure, we suppress the Josephson coupling between the superconducting nanodiamond grains. The diminished intergrain coupling gives rise to an overall insulating state in the films, which is interpreted in the framework of a parallel-series circuit model to be the result of bosonic insulators with preserved localized intragrain superconducting order parameters. Our investigation opens up perspectives for the application of high pressure in research on quantum confinement and coherence. Our data unveil the percolative nature of the electrical transport in nanodiamond films, and highlight the essential role of grain boundaries in determining the electronic properties of this material.

关键词： Density of states Electrical properties Localization Nanocrystals Order parameters Percolation Phase transitions Structural properties Superconducting order parameter Superconducting phase transition Superconductivity Transport phenomena

来源：评论

学校读者我要写书评

暂无评论

Constraints on dark matter to dark radiation conversion in the late universe with DES-Y1 and external data

引用

Physical Review D 2021年第12期103卷 123528-123528页

作者： A. Chen D. Huterer S. Lee A. Ferté N. Weaverdyck O. Alves C. D. Leonard N. MacCrann M. Raveri A. Porredon E. Di Valentino J. Muir P. Lemos A. R. Liddle J. Blazek A. Campos R. Cawthon A. Choi S. Dodelson J. Elvin-Poole D. Gruen A. J. Ross L. F. Secco I. Sevilla-Noarbe E. Sheldon M. A. Troxel J. Zuntz T. M. C. Abbott M. Aguena S. Allam J. Annis S. Avila E. Bertin S. Bhargava S. L. Bridle D. Brooks A. Carnero Rosell M. Carrasco Kind J. Carretero M. Costanzi M. Crocce L. N. da Costa M. E. S. Pereira T. M. Davis P. Doel T. F. Eifler I. Ferrero P. Fosalba J. Frieman J. García-Bellido E. Gaztanaga D. W. Gerdes R. A. Gruendl J. Gschwend G. Gutierrez S. R. Hinton D. L. Hollowood K. Honscheid B. Hoyle D. J. James M. Jarvis K. Kuehn O. Lahav M. A. G. Maia J. L. Marshall F. Menanteau R. Miquel R. Morgan A. Palmese F. Paz-Chinchón A. A. Plazas A. Roodman E. Sanchez V. Scarpine M. Schubnell S. Serrano M. Smith E. Suchyta G. Tarle D. Thomas C. To T. N. Varga J. Weller R. D. Wilkinson Department of Physics University of Michigan Ann Arbor Michigan 48109 USA Department of Physics Duke University Durham North Carolina 27708 USA Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive Pasadena California 91109 USA Instituto de Física Teórica Universidade Estadual Paulista São Paulo Brazil School of Mathematics Statistics and Physics Newcastle Unviersity NE1 7RU United Kingdom Center for Cosmology and Astro-Particle Physics The Ohio State University Columbus Ohio 43210 USA Department of Physics The Ohio State University Columbus Ohio 43210 USA Kavli Institute for Cosmological Physics University of Chicago Chicago Illinois 60637 USA Institut d’Estudis Espacials de Catalunya (IEEC) Barcelona 08034 Spain Institute of Space Sciences (ICE CSIC) Campus UAB Carrer de Can Magrans s/n Barcelona 08193 Spain Jodrell Bank Center for Astrophysics School of Physics and Astronomy University of Manchester Oxford Road Manchester M13 9PL United Kingdom Kavli Institute for Particle Astrophysics & Cosmology P. O. Box 2450 Stanford University Stanford California 94305 USA Department of Physics & Astronomy University College London Gower Street London WC1E 6BT United Kingdom Instituto de Astrofísica e Ciências do Espaço Faculdade de Ciências Universidade de Lisboa 1769-016 Lisboa Portugal Institute for Astronomy University of Edinburgh Edinburgh EH9 3HJ United Kingdom Perimeter Institute for Theoretical Physics 31 Caroline Street North Waterloo Ontario N2L 2Y5 Canada Institute of Physics Laboratory of Astrophysics École Polytechnique Fédérale de Lausanne (EPFL) Observatoire de Sauverny 1290 Versoix Switzerland Department of Physics Carnegie Mellon University Pittsburgh Pennsylvania 15312 USA Physics Department 2320 Chamberlin Hall University of Wisconsin-Madison 1150 University Avenue Madison Wisconsin 53706-1390 USA Department of Physics Stanford University 382 Via Pueblo Mall Stanford California 94305 USA SLA

We study a phenomenological class of models where dark matter converts to dark radiation in the low redshift epoch. This class of models, dubbed DMDR, characterizes the evolution of comoving dark-matter density with two extra parameters, and may be able to help alleviate the observed discrepancies between early and late-time probes of the Universe. We investigate how the conversion affects key cosmological observables such as the cosmic microwave background (CMB) temperature and matter power spectra. Combining 3x2pt data from Year 1 of the Dark Energy Survey, Planck-2018 CMB temperature and polarization data, supernovae (SN) Type Ia data from Pantheon, and baryon acoustic oscillation (BAO) data from BOSS DR12, MGS and 6dFGS, we place new constraints on the amount of dark matter that has converted to dark radiation and the rate of this conversion. The fraction of the dark matter that has converted since the beginning of the Universe in units of the current amount of dark matter, ζ, is constrained at 68% confidence level to be <0.32 for DES-Y1 3x2pt data, <0.030 for CMB+SN+BAO data, and <0.037 for the combined dataset. The probability that the DES and CMB+SN+BAO datasets are concordant increases from 4% for the ΛCDM model to 8% (less tension) for DMDR. The tension in S8=σ8Ωm/0.3 between DES-Y1 3x2pt and CMB+SN+BAO is slightly reduced from 2.3σ to 1.9σ. We find no reduction in the Hubble tension when the combined data is compared to distance-ladder measurements in the DMDR model. The maximum-posterior goodness-of-fit statistics of DMDR and ΛCDM model are comparable, indicating no preference for the DMDR cosmology over ΛCDM.

关键词： Cosmological parameters Dark energy Dark matter Evolution of the Universe Large scale structure of the Universe

来源：评论

学校读者我要写书评

暂无评论

Dwarf AGNs from Optical Variability for the Origins of Seeds (DAVOS): Insights from the Dark Energy Survey Deep Fields

arXiv

引用

arXiv 2021年

作者： Burke, Colin J. Liu, Xin Shen, Yue Phadke, Kedar A. Yang, Qian Hartley, Will G. Harrison, Ian Palmese, Antonella Guo, Hengxiao Zhang, Kaiwen Kron, Richard Turner, David J. Giles, Paul A. Lidman, Christopher Chen, Yu-Ching Gruendl, Robert A. Choi, Ami Amon, Alexandra Sheldon, Erin Aguena, M. Allam, S. Andrade-Oliveira, F. Bacon, D. Bertin, E. Brooks, D. Rosell, A. Carnero Kind, M. Carrasco Carretero, J. Conselice, C. Costanzi, M. da Costa, L.N. Pereira, M.E.S. Davis, T.M. De Vicente, J. Desai, S. Diehl, H.T. Everett, S. Ferrero, I. Flaugher, B. García-Bellido, J. Gaztanaga, E. Gruen, D. Gschwend, J. Gutierrez, G. Hinton, S.R. Hollowood, D.L. Honscheid, K. Hoyle, B. James, D.J. Kuehn, K. Maia, M.A.G. Marshall, J.L. Menanteau, F. Miquel, R. Morgan, R. Paz-Chinchón, F. Pieres, A. Malagón, A.A. Plazas Reil, K. Romer, A.K. Sanchez, E. Schubnell, M. Serrano, S. Sevilla-Noarbe, I. Smith, M. Suchyta, E. Tarle, G. Thomas, D. To, C. Varga, T.N. Wilkinson, R.D. Department of Astronomy University of Illinois at Urbana-Champaign 1002 West Green Street UrbanaIL61801 United States Center for AstroPhysical Surveys National Center for Supercomputing Applications 1205 West Clark Street UrbanaIL61801 United States National Center for Supercomputing Applications 1205 West Clark Street UrbanaIL61801 United States Department of Astronomy University of Geneva ch. d’Ecogia 16 VersoixCH-1290 Switzerland Jodrell Bank Centre for Astrophysics School of Physics & Astronomy The University of Manchester ManchesterM13 9PL United Kingdom Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Department of Physics and Astronomy 4129 Frederick Reines Hall University of California IrvineCA92697-4575 United States Department of Physics University of Illinois at Urbana-Champaign 1110 West Green Street UrbanaIL61801 United States Department of Astronomy & Astrophysics The University of Chicago ChicagoIL60637 United States Department of Physics and Astronomy Pevensey Building University of Sussex BrightonBN1 9QH United Kingdom The Research School of Astronomy and Astrophysics Australian National University ACT2601 Australia Center for Cosmology and Astro-Particle Physics The Ohio State University ColumbusOH43210 United States Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 StanfordCA94305 United States Brookhaven National Laboratory Bldg 510 UptonNY11973 United States Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 RJ Rio de Janeiro20921-400 Brazil Instituto de Física Teórica Universidade Estadual Paulista SP São Paulo01140-070 Brazil Institute of Cosmology and Gravitation University of Portsmouth PortsmouthPO1 3FX United Kingdom CNRS UMR 7095 Institut d’Astrophysique de Paris ParisF-75014 France Sorbonne Universi

We present a sample of 706, z 2. We construct light curves using difference imaging aperture photometry for resolved sources and non-difference imaging PSF photometry for unresolved sources, respectively, and characterize the variability significance. Our DES light curves have a mean cadence of 7 days, a 6 year baseline, and a single-epoch imaging depth of up to g ∼ 24.5. Using spectral energy distribution (SED) fitting, we find 26 out of total 706 variable galaxies are consistent with dwarf galaxies with a reliable stellar mass estimate (M∗ 9.5 M;median photometric redshift of 0.9). We were able to constrain rapid characteristic variability timescales (∼ weeks) using the DES light curves in 15 dwarf AGN candidates (a subset of our variable AGN candidates) at a median photometric redshift of 0.4. This rapid variability is consistent with their low black hole masses. We confirm the low-mass AGN nature of one source with a high S/N optical spectrum. We publish our catalog, optical light curves, and supplementary data, such as X-ray properties and optical spectra, when available. We measure a variable AGN fraction versus stellar mass and compare to results from a forward model. This work demonstrates the feasibility of optical variability to identify AGNs with lower black hole masses in deep fields, which may be more "pristine" analogs of supermassive black hole seeds. Copyright © 2021, The Authors. All rights reserved.

关键词： Active Galactic Nuclei

来源：评论

学校读者我要写书评

暂无评论

The SST-1M project for the cherenkov telescope array 36

The SST-1M project for the cherenkov telescope array

引用

36th International Cosmic Ray Conference, ICRC 2019

作者： Heller, M. Alispach, C. Al Samarai, I. Balbo, M. Barbano, A. Beshley, V. Biland, A. Blazek, J. Blocki, J. Borkowski, J. Bulik, T. Cadoux, F. Chytka, L. Coco, V. de Angelis, N. Della Volpe, D. Favre, Y. Gieras, T. Grudzinska, M. Hamal, P. Hrabovsky, M. Juryšek, J. Kasperek, J. Koncewicz, K. Kotarba, A. Lyard, E. Mach, E. Mandat, D. Michal, S. Michalowski, J. Moderski, R. Montaruli, T. Nagai, A. Neise, D. Niemiec, J. Njoh Ekoume, T.R.S. Ostrowski, M. Palatka, M. Pasko, P. Pech, M. Pilszyk, B. Przybilski, H. Rajda, P. Renier, Y. Rozwadowski, P. Schovanek, P. Seweryn, K. Sliusar, V. Smakulska, D. Sobczynska, D. Stawarz, L. Swierblewski, J. Swierk, P. Travnicek, P. Troyano Pujadas, I. Walter, R. Wiecek, M. Zagdanski, A. Zietara, K. DPNC - Université de Genève 24 Quai Ernest Ansermet GenèveCH-1211 Switzerland Département d'Astronomie Université de Genève Chemin d'Ecogia 16 VersoixCH-1290 Switzerland ETH Zurich Institute for Particle Physics and Astrophysics Otto-Stern-Weg 5 Zurich8093 Switzerland Institute of Nuclear Physics Polish Academy of Sciences KrakowPL-31342 Poland Astronomical Observatory University of Warsaw Al. Ujazdowskie 4 Warsaw00-478 Poland Astronomical Observatory Jagiellonian University ul. Orla 171 Kraków30-244 Poland Centrum Badan Kosmicznych Polskiej Akademii Nauk 18a Bartycka str. Warsaw00-716 Poland Nicolaus Copernicus Astronomical Center Polish Academy of Sciences ul. Bartycka 18 Warsaw00-716 Poland FZU - Institute of Physics of the Czech Academy of Sciences 17. listopadu 50 Olomouc & Na Slovance 2 Prague Czech Republic AGH University of Science and Technology al.Mickiewicza 30 Kraków30-059 Poland Palacky University Olomouc Faculty of Science RCPTM 17. listopadu 50 Olomouc Czech Republic Department of Astrophysics University of Lódz ul. Pomorska 149/153 Lódz90-236 Poland Pidstryhach Institute for Applied Problems of Mechanics and Mathematics National Academy of Sciences of Ukraine 3-b Naukova St. Lviv79060 Ukraine

The SST-1M project, run by a Consortium of institutes from Czech Republic, Poland and Switzerland, has been proposed as a solution for implementing the small-size telescope array of the southern site of the Cherenkov Telescope Array. The technology is a pathfinder for efficient production of cost-effective imaging air Cherenkov telescopes. We report on the main system features and recent upgrades, the performances validation and the operation campaign carried out in 2018. © Copyright owned by the author(s) under the terms of the Creative Commons

关键词： Cost effectiveness

来源：评论

学校读者我要写书评

暂无评论

Embedded Software of the KM3NeT Central Logic Board

arXiv

引用

arXiv 2023年

作者： Aiello, S. Albert, A. Alves Garre, S. Aly, Z. Ambrosone, A. Ameli, F. Andre, M. Androutsou, E. Anghinolfi, M. Anguita, M. Aphecetche, L. Ardid, M. Ardid, S. Atmani, H. Aublin, J. Bagatelas, C. Bailly-Salins, L. Bardačová, Z. Baret, B. du Pree, S. Basegmez Becherini, Y. Bendahman, M. Benfenati, F. Benhassi, M. Benoit, D.M. Berbee, E. Bertin, V. van Beveren, V. Biagi, S. Boettcher, M. Boumaaza, J. Bouta, M. Bouwhuis, M. Bozza, C. Bozza, R.M. Brânzaş, H. Bretaudeau, F. Bruijn, R. Brunner, J. Bruno, R. Buis, E. Buompane, R. Busto, J. Caiffi, B. Calvo, D. Campion, S. Capone, A. Carenini, F. Carretero, V. Cartraud, T. Castaldi, P. Cecchini, V. Celli, S. Cerisy, L. Chabab, M. Chadolias, M. Chen, A. Cherubini, S. Chiarusi, T. Circella, M. Cocimano, R. Coelho, J.A.B. Coleiro, A. Coniglione, R. Coyle, P. Creusot, A. Cruz, A. Cuttone, G. Dallier, R. Darras, Y. De Benedittis, A. De Martino, B. Decoene, V. Del Burgo, R. Di Mauro, L.S. Di Palma, I. Díaz, A.F. Diego-Tortosa, D. Distefano, C. Domi, A. Donzaud, C. Dornic, D. Dörr, M. Drakopoulou, E. Drouhin, D. Dvornický, R. Eberl, T. Eckerová, E. Eddymaoui, A. van Eeden, T. Eff, M. van Eijk, D. El Bojaddaini, I. El Hedri, S. Enzenhöfer, A. Ferrara, G. Filipović, M.D. Filippini, F. Fusco, L.A. Gabella, O. Gabriel, J. Gagliardini, S. Gal, T. García Méndez, J. Garcia Soto, A. Gatius Oliver, C. Geißelbrecht, N. Ghaddari, H. Gialanella, L. Gibson, B.K. Giorgio, E. Girardi, A. Goos, I. Goupilliere, D. Gozzini, S.R. Gracia, R. Graf, K. Guidi, C. Guillon, B. Gutiérrez, M. van Haren, H. Heijboer, A. Hekalo, A. Hennig, L. Hernández-Rey, J.J. Huang, F. Idrissi Ibnsalih, W. Illuminati, G. James, C.W. Jansweijer, P. de Jong, M. de Jong, P. Jung, B.J. Kalaczyński, P. Kalekin, O. Katz, U.F. Khan Chowdhury, N.R. Khatun, A. Kistauri, G. Kopper, C. Kouchner, A. Kulikovskiy, V. Kvatadze, R. Labalme, M. Lahmann, R. Larosa, G. Lastoria, C. Lazo, A. Le Stum, S. Lehaut, G. Leonora, E. INFN Sezione di Catania Via Santa Sofia 64 Catania95123 Italy Université de Strasbourg CNRS IPHC UMR 7178 StrasbourgF-67000 France IFIC - Instituto de Física Corpuscular CSIC - Universitat de València c/Catedrático José Beltrán 2 Paterna Valencia46980 Spain Aix Marseille Univ. CNRS IN2P3 CPPM Marseille France INFN Sezione di Napoli Complesso Universitario di Monte S. Angelo Via Cintia ed. G Napoli80126 Italy Università di Napoli "Federico II" Dip. Scienze Fisiche "E. Pancini" Complesso Universitario di Monte S. Angelo Via Cintia ed. G Napoli80126 Italy INFN Sezione di Roma Piazzale Aldo Moro 2 Roma00185 Italy Universitat Politècnica de Catalunya Laboratori d’Aplicacions Bioacústiques Centre Tecnològic de Vilanova i la Geltrú Avda. Rambla Exposició s/n Vilanova i la Geltrú08800 Spain NCSR Demokritos Institute of Nuclear and Particle Physics Ag. Paraskevi Attikis Athens15310 Greece INFN Sezione di Genova Via Dodecaneso 33 Genova16146 Italy University of Granada Dept. of Computer Architecture and Technology CITIC Granada18071 Spain Subatech IMT Atlantique IN2P3-CNRS Université de Nantes 4 rue Alfred Kastler - La Chantrerie BP 20722 Nantes44307 France Universitat Politècnica de València Instituto de Investigación para la Gestión Integrada de las Zonas Costeras C/Paranimf 1 Gandia46730 Spain University Mohammed V in Rabat Faculty of Sciences 4 av. Ibn Battouta B.P. 1014 RabatR.P. 10000 Morocco Université Paris Cité CNRS Astroparticule et Cosmologie ParisF-75013 France LPC CAEN Normandie Univ. ENSICAEN UNICAEN CNRS IN2P3 6 boulevard Maréchal Juin Caen14050 France Czech Technical University in Prague Institute of Experimental and Applied Physics Husova 240/5 Prague110 00 Czech Republic Comenius University in Bratislava Department of Nuclear Physics and Biophysics Mlynska dolina F1 Bratislava842 48 Slovakia National Institute for Subatomic Physics PO Box 41882 Amsterdam1009 DB Netherlands INFN Sezione di Bologna

The KM3NeT Collaboration is building and operating two deep sea neutrino telescopes at the bottom of the Mediterranean Sea. The telescopes consist of latices of photomultiplier tubes housed in pressure-resistant glass spheres, called digital optical modules and arranged in vertical detection units. The two main scientific goals are the determination of the neutrino mass ordering and the discovery and observation of high-energy neutrino sources in the Universe. Neutrinos are detected via the Cherenkov light, which is induced by charged particles originated in neutrino interactions. The photomultiplier tubes convert the Cherenkov light into electrical signals that are acquired and timestamped by the acquisition electronics. Each optical module houses the acquisition electronics for collecting and timestamping the photomultiplier signals with one nanosecond accuracy. Once finished, the two telescopes will have installed more than six thousand optical acquisition nodes, completing one of the more complex networks in the world in terms of operation and synchronization. The embedded software running in the acquisition nodes has been designed to provide a framework that will operate with different hardware versions and functionalities. The hardware will not be accessible once in operation, which complicates the embedded software architecture. The embedded software provides a set of tools to facilitate remote manageability of the deployed hardware, including safe reconfiguration of the firmware. This paper presents the architecture and the techniques, methods and implementation of the embedded software running in the acquisition nodes of the KM3NeT neutrino telescopes. © 2023, CC BY-NC-ND.

关键词： Photomultipliers

来源：评论

学校读者我要写书评

暂无评论

Preface

Smart Innovation, Systems and Technologies

引用

Smart Innovation, Systems and Technologies 2019年 133卷 v页

作者： Petrov, Igor B. Favorskaya, Alena V. Favorskaya, Margarita N. Simakov, Sergey S. Jain, Lakhmi C. Department of Computer Science and Numerical Mathematics Moscow Institute of Physics and Technology The Moscow Area Dolgoprudny Russia Department of Applied Computational Geophysics Moscow Institute of Physics and Technology The Moscow Area Dolgoprudny Russia Institute of Informatics and Telecommunications Reshetnev Siberian State University of Science and Technology Krasnoyarsk Russia Department of Computational Physics Moscow Institute of Physics and Technology The Moscow Area Dolgoprudny Russia Faculty of Engineering and Information Technology Centre for Artificial Intelligence University of Technology SydneyNSW Australia Faculty of Science and Technology University of Canberra CanberraACT Australia Faculty of Science Liverpool Hope University Liverpool United Kingdom KES International Shoreham-by-Sea United Kingdom

来源：评论

学校读者我要写书评

暂无评论

Rapidity dependence of proton cumulants and correlation functions

引用

Physical Review C 2017年第5期96卷 054905-054905页

作者： Adam Bzdak Volker Koch AGH University of Science and Technology Faculty of Physics and Applied Computer Science 30-059 Kraków Poland Nuclear Science Division Lawrence Berkeley National Laboratory Berkeley California 94720 USA

The dependence of multiproton correlation functions and cumulants on the acceptance in rapidity and transverse momentum is studied. We find that the preliminary data of various cumulant ratios are consistent, within errors, with rapidity and transverse momentum-independent correlation functions. However, rapidity correlations which moderately increase with rapidity separation between protons are slightly favored. We propose to further explore the rapidity dependence of multiparticle correlation functions by measuring the dependence of the integrated reduced correlation functions as a function of the size of the rapidity window.

关键词： Particle correlations & fluctuations Relativistic heavy-ion collisions

来源：评论

学校读者我要写书评

暂无评论

Cumulants and correlation functions versus the QCD phase diagram

引用

Physical Review C 2017年第5期95卷 054906-054906页

作者： Adam Bzdak Volker Koch Nils Strodthoff AGH University of Science and Technology Faculty of Physics and Applied Computer Science 30-059 Kraków Poland Nuclear Science Division Lawrence Berkeley National Laboratory Berkeley California 94720 USA

In this paper we discuss the relation of particle number cumulants and correlation functions. It is argued that measuring couplings of the genuine multiparticle correlation functions could provide cleaner information on possible nontrivial dynamics in heavy-ion collisions. We extract integrated multiproton correlation functions from the presently available experimental data on proton cumulants. We find that the STAR data contain significant four-proton correlations, at least at the lower energies, with indication of changing dynamics in central collisions. We also find that these correlations are rather long ranged in rapidity. Finally, using the Ising model, we demonstrate how the signs of the multiproton correlation functions may be used to exclude certain regions of the phase diagram close to the critical point.

关键词： Particle correlations & fluctuations QCD phase transitions Relativistic heavy-ion collisions

来源：评论

学校读者我要写书评

暂无评论

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

请选择保存的检索档案：

请选择收藏分类：

通借通还

建议与咨询 留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

请选择保存的检索档案： 新增检索档案 确定 取消

请选择收藏分类： 新增自定义分类 确定 取消

通借通还

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

请选择保存的检索档案：

请选择收藏分类：