Standard Model and Related Topics
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  • 英文篇名:Standard Model and Related Topics
  • 作者:C.Patrignani ; K.Agashe ; G.Aielli ; C.Amsler ; M.Antonelli ; D.M.Asner ; H.Baer ; Sw.Banerjee ; R.M.Barnett ; T.Basaglia ; C.W.Bauer ; J.J.Beatty ; V.I.Belousov ; J.Beringer ; S.Bethke ; H.Bichsel ; O.Biebel ; E.Blucher ; G.Brooijmans ; O.Buchmueller ; V.Burkert ; M.A.Bychkov ; R.N.Cahn ; M.Carena ; A.Ceccucci ; A.Cerri ; D.Chakraborty ; M.-C.Chen ; R.S.Chivukula ; K.Copic ; G.Cowan ; O.Dahl ; G.D'Ambrosio ; T.Damour ; D.de ; Florian ; A.de ; Gouvea ; T.DeGrand ; P.de ; Jong ; G.Dissertori ; B.A.Dobrescu ; M.D'Onofrio ; M.Doser ; M.Drees ; H.K.Dreiner ; D.A.Dwyer ; P.Eerola ; S.Eidelman ; J.Ellis ; J.Erler ; V.V.Ezhela ; W.Fetscher ; B.D.Fields ; B.Foster ; A.Freitas ; H.Gallagher ; L.Garren ; H.-J.Gerber ; G.Gerbier ; T.Gershon ; T.Gherghetta ; A.A.Godizov ; M.Goodman ; C.Grab ; A.V.Gritsan ; C.Grojean ; D.E.Groom ; M.Grnewald ; A.Gurtu ; T.Gutsche ; H.E.Haber ; K.Hagiwara ; C.Hanhart ; S.Hashimoto ; Y.Hayato ; K.G.Hayes ; A.Hebecker ; B.Heltsley ; J.J.Hernandez-Rey ; K.Hikasa ; J.Hisano ; A.Hcker ; J.Holder ; A.Holtkamp ; J.Huston ; T.Hyodo ; K.Irwin ; J.D.Jackson ; K.F.Johnson ; M.Kado ; M.Karliner ; U.F.Katz ; S.R.Klein ; E.Klempt ; R.V.Kowalewski ; F.Krauss ; M.Kreps ; B.Krusche ; Yu.V.Kuyanov ; Y.Kwon ; O.Lahav ; J.Laiho ; P.Langacker ; A.Liddle ; Z.Ligeti ; C.-J.Lin ; C.Lippmann ; T.M.Liss ; L.Littenberg ; K.S.Lugovsky ; S.B.Lugovsky ; A.Lusiani ; Y.Makida ; F.Maltoni ; T.Mannel ; A.V.Manohar ; W.J.Marciano ; A.D.Martin ; A.Masoni ; J.Matthews ; U.-G.Meiβner ; D.Milstead ; R.E.Mitchell ; P.Molaro ; K.Mnig ; F.Moortgat ; M.J.Mortonson ; H.Murayama ; K.Nakamura ; M.Narain ; P.Nason ; S.Navas ; M.Neubert ; P.Nevski ; Y.Nir ; K.A.Olive ; S.Pagan ; Griso ; J.Parsons ; J.A.Peacock ; M.Pennington ; S.T.Petcov ; V.A.Petrov ; A.Piepke ; A.Pomarol ; A.Quadt ; S.Raby ; J.Rademacker ; G.Raffelt ; B.N.Ratcliff ; P.Richardson ; A.Ringwald ; S.Roesler ; S.Rolli ; A.Romaniouk ; L.J.Rosenberg ; J.L.Rosner ; G.Rybka ; R.A.Ryutin ; C.T.Sachrajda ; Y.Sakai ; G.P.Salam ; S.Sarkar ; F.Sauli ; O.Schneider ; K.Scholberg ; A.J.Schwartz ; D.Scott ; V.Sharma ; S.R.Sharpe ; T.Shutt ; M.Silari ; T.Sjstrand ; P.Skands ; T.Skwarnicki ; J.G.Smith ; G.F.Smoot ; S.Spanier ; H.Spieler ; C.Spiering ; A.Stahl ; S.L.Stone ; Y.Sumino ; T.Sumiyoshi ; M.J.Syphers ; F.Takahashi ; M.Tanabashi ; K.Terashi ; J.Terning ; R.S.Thorne ; L.Tiator ; M.Titov ; N.P.Tkachenko ; N.A.Trnqvist ; D.Tovey ; G.Valencia ; R.Van ; de ; Water ; N.Varelas ; G.Venanzoni ; M.G.Vincter ; P.Vogel ; A.Vogt ; S.P.Wakely ; W.Walkowiak ; C.W.Walter ; D.Wands ; D.R.Ward ; M.O.Wascko ; G.Weiglein ; D.H.Weinberg ; E.J.Weinberg ; M.White ; L.R.Wiencke ; S.Willocq ; C.G.Wohl ; L.Wolfenstein ; J.Womersley ; C.L.Woody ; R.L.Workman ; W.-M.Yao ; G.P.Zeller ; O.V.Zenin ; R.-Y.Zhu ; F.Zimmermann ; P.A.Zyla ; J.Anderson ; G.Harper ; V.S.Lugovsky ; P.Schaffner
  • 英文作者:C.Patrignani;K.Agashe;G.Aielli;C.Amsler;M.Antonelli;D.M.Asner;H.Baer;Sw.Banerjee;R.M.Barnett;T.Basaglia;C.W.Bauer;J.J.Beatty;V.I.Belousov;J.Beringer;S.Bethke;H.Bichsel;O.Biebel;E.Blucher;G.Brooijmans;O.Buchmueller;V.Burkert;M.A.Bychkov;R.N.Cahn;M.Carena;A.Ceccucci;A.Cerri;D.Chakraborty;M.-C.Chen;R.S.Chivukula;K.Copic;G.Cowan;O.Dahl;G.D'Ambrosio;T.Damour;D.de Florian;A.de Gouvea;T.DeGrand;P.de Jong;G.Dissertori;B.A.Dobrescu;M.D'Onofrio;M.Doser;M.Drees;H.K.Dreiner;D.A.Dwyer;P.Eerola;S.Eidelman;J.Ellis;J.Erler;V.V.Ezhela;W.Fetscher;B.D.Fields;B.Foster;A.Freitas;H.Gallagher;L.Garren;H.-J.Gerber;G.Gerbier;T.Gershon;T.Gherghetta;A.A.Godizov;M.Goodman;C.Grab;A.V.Gritsan;C.Grojean;D.E.Groom;M.Grnewald;A.Gurtu;T.Gutsche;H.E.Haber;K.Hagiwara;C.Hanhart;S.Hashimoto;Y.Hayato;K.G.Hayes;A.Hebecker;B.Heltsley;J.J.Hernandez-Rey;K.Hikasa;J.Hisano;A.Hcker;J.Holder;A.Holtkamp;J.Huston;T.Hyodo;K.Irwin;J.D.Jackson;K.F.Johnson;M.Kado;M.Karliner;U.F.Katz;S.R.Klein;E.Klempt;R.V.Kowalewski;F.Krauss;M.Kreps;B.Krusche;Yu.V.Kuyanov;Y.Kwon;O.Lahav;J.Laiho;P.Langacker;A.Liddle;Z.Ligeti;C.-J.Lin;C.Lippmann;T.M.Liss;L.Littenberg;K.S.Lugovsky;S.B.Lugovsky;A.Lusiani;Y.Makida;F.Maltoni;T.Mannel;A.V.Manohar;W.J.Marciano;A.D.Martin;A.Masoni;J.Matthews;U.-G.Meiβner;D.Milstead;R.E.Mitchell;P.Molaro;K.Mnig;F.Moortgat;M.J.Mortonson;H.Murayama;K.Nakamura;M.Narain;P.Nason;S.Navas;M.Neubert;P.Nevski;Y.Nir;K.A.Olive;S.Pagan Griso;J.Parsons;J.A.Peacock;M.Pennington;S.T.Petcov;V.A.Petrov;A.Piepke;A.Pomarol;A.Quadt;S.Raby;J.Rademacker;G.Raffelt;B.N.Ratcliff;P.Richardson;A.Ringwald;S.Roesler;S.Rolli;A.Romaniouk;L.J.Rosenberg;J.L.Rosner;G.Rybka;R.A.Ryutin;C.T.Sachrajda;Y.Sakai;G.P.Salam;S.Sarkar;F.Sauli;O.Schneider;K.Scholberg;A.J.Schwartz;D.Scott;V.Sharma;S.R.Sharpe;T.Shutt;M.Silari;T.Sjstrand;P.Skands;T.Skwarnicki;J.G.Smith;G.F.Smoot;S.Spanier;H.Spieler;C.Spiering;A.Stahl;S.L.Stone;Y.Sumino;T.Sumiyoshi;M.J.Syphers;F.Takahashi;M.Tanabashi;K.Terashi;J.Terning;R.S.Thorne;L.Tiator;M.Titov;N.P.Tkachenko;N.A.Trnqvist;D.Tovey;G.Valencia;R.Van de Water;N.Varelas;G.Venanzoni;M.G.Vincter;P.Vogel;A.Vogt;S.P.Wakely;W.Walkowiak,95;C.W.Walter;D.Wands;D.R.Ward;M.O.Wascko;G.Weiglein;D.H.Weinberg;E.J.Weinberg;M.White;L.R.Wiencke;S.Willocq;C.G.Wohl;L.Wolfenstein;J.Womersley;C.L.Woody;R.L.Workman;W.-M.Yao;G.P.Zeller;O.V.Zenin;R.-Y.Zhu;F.Zimmermann;P.A.Zyla;J.Anderson;G.Harper;V.S.Lugovsky;P.Schaffner;Particle Data Group;Universita di Bologna and INFN,Dip.Scienze per la Qualita della Vita;University of Maryland,Department of Physics,College Park;Universit degli Studi di Roma "Tor Vergata";Albert Einstein Center for Fundamental Physics,Universitt Bern;Stefan Meyer Institute for Subatomic Physics,Austrian Academy of Sciences;Lab.Nazionali di Frascati dell'INFN;Pacific Northwest National Laboratory;Department of Physics and Astronomy,University of Oklahoma;University of Louisville;Physics Division,Lawrence Berkeley National Laboratory;CERN,European Organization for Nuclear Research;Department of Physics,The Ohio State University;COMPAS Group,Institute for High Energy Physics;Max-Planck-Institute of Physics;Department of Physics,University of Washington;Ludwig-Maximilians-Universitt,Fakultt fr Physik;Enrico Fermi Institute and Department of Physics,University of Chicago;Department of Physics,Columbia University;High Energy Physics Group,Blackett Laboratory,Imperial College;Jefferson Lab;Department of Physics,University of Virginia;Fermi National Accelerator Laboratory;Kavli Institute for Cosmological Physics,University of Chicago;Department of Physics and Astronomy,University of Sussex;Department of Physics,Northern Illinois University;Department of Physics and Astronomy,University of California;Michigan State University,Dept.of Physics and Astronomy;Department of Physics,Royal Holloway,University of London;INFN-Sezione di Napoli,Complesso Universitario Monte Sant'Angelo;Institut des Hautes Etudes Scientifiques;International Center for Advanced Studies(ICAS),UNSAM;Department of Physics and Astronomy,Northwestern University;Department of Physics,University of Colorado at Boulder;Nikhef,P.O.Box 41882,1009 DB Amsterdam,and University of Amsterdam;Institute for Particle Physics,ETH Zurich;University of Liverpool,Department of Physics,Oliver Lodge Lab;Physikalisches Institut,Universitt Bonn;Helsinki Institute of Physics;University of Helsinki;Department of Physics;Budker Institute of Nuclear Physics SB RAS;Novosibirsk State University;King's College London,Department of Physics;Departamento de Fisica Teorica,Instituto de Fisica,Universidad Nacional Autonoma de Mexico;Moscow Institute of Physics and Technology(State University);Department of Astronomy,University of Illinois;Department of Physics,University of Illinois;University of Hamburg;Deutsches Elektronen-Synchrotron DESY;Denys Wilkinson Building,Department of Physics,University of Oxford;University of Pittsburgh,Department of Physics and Astronomy;Department of Physics and Astronomy,Tufts University;CEA Saclay,DSM/IRFU/SPP;Department of Physics,University of Warwick;University of Minnesota,School of Physics and Astronomy;Argonne National Laboratory;Johns Hopkins University;Institucio Catalana de Recerca iEstudis Avancats,Institut de Fisica d'Altes Energies;School of Physics,University College Dublin;TIFR;Institut fur Theoretische Physik,Universitat Tubingen;Santa Cruz Institute for Particle Physics,University of California;KEK,High Energy Accelerator Research Organization;Institut fr Kernphysik and Institute for Advanced Simulation,Forschungszentrum Julich;Department of Physics,University of Tokyo;Department of Physics,Hillsdale College;Institute for Theoretical Physics,Heidelberg University;Laboratory of Elementary-Particle Physics,Cornell University;IFIC—Instituto de Fisica Corpuscular,Universitat de Valencia-C.S.I.C.;Department of Physics,Tohoku University;Kobayashi-Maskawa Institute,Nagoya University;Department of Physics and Astronomy,University of Delaware;Bartol Research Institute,University of Delaware;Yukawa Institute for Theoretical Physics,Kyoto University;Department of Physics,Stanford University;SLAC National Accelerator Laboratory;Los Alamos National Laboratory;LAL,IN2P3-CNRS et Univ.;Department of Particle Physics,Tel-Aviv University;University of Erlangen-Nuremberg,Erlangen Centre for Astroparticle Physics;Nuclear Science Division,Lawrence Berkeley National Laboratory;Helmholtz-Institut fur Strahlen- und Kernphysik,Universitat Bonn;University of Victoria;Institute for Particle Physics Phenomenology,Department of Physics,University of Durham;Institute of Physics,University of Basel;Yonsei University,Department of Physics;Department of Physics and Astronomy,University College London;Department of Physics,Syracuse University;School of Natural Science,Institute for Advanced Study;Institute for Astronomy,University of Edinburgh;GSI,Helmholtzzentrum fr Schwerionenforschung;Division of Science,City College of New York;Physics Department,Brookhaven National Laboratory;INFN and Dipartimento di Fisica,Universita di Pisa;Centre for Cosmology,Particle Physics and Phenomenology(CP3),Universite catholique de Louvain;Department fur Physik,Universitat Siegen;Department of Physics,University of California at San Diego;INFN Sezione di Cagliari,Cittadella Universitaria di Monserrato;Department of Physics and Astronomy,Louisana State University;Fysikum,Stockholms Universitet,AlbaNova University Centre;Deparment of Physics,Indiana University;INAF-OATS;DESY;The Space Sciences Laboratory(SSL),University of California;Kavli IPMU(WPI),Todai Institutes for Advanced Study,University of Tokyo;Department of Physics,University of California;Brown University,Department of Physics;INFN,Sez.di Milano-Bicocca;Dpto,de Fisica Teorica y del Cosmos & C.A.F.P.E.,Universidad de Granada;PRISMA Cluster of Excellence and Mainz Institute for Theoretical Physics,Johannes Gutenberg University;Department of Particle Physics and Astrophysics,Weizmann Institute of Science;SISSA/INFN;INRNE,Bulgarian Academy of Sciences;Department of Physics and Astronomy,University of Alabama;Departament de Fisica,Universitat Autonoma de Barcelona;Georg-August-Universitat Gottingen,Ⅱ.Physikalisches Institut;HH Wills Physics Laboratory,University of Bristol;Max-Planck-Institut fur Physik(Werner-Heisenberg-Institut);DOE;National Research Nuclear University "MEPhI"(Moscow Engineering Physics Institute);School of Physics and Astronomy,University of Southampton;LPTHE,UPMC Universite de Paris 6;Rudolf Peierls Centre for Theoretical Physics,University of Oxford;Niels Bohr Institute;Ecole Polytechnique Federale de Lausanne(EPFL);Physics Department,Duke University;Department of Physics,University of Cincinnati;Department of Physics and Astronomy,University of British Columbia;Department of Astronomy and Theoretical Physics,Lund University;School of Physics,Monash University;Paris Centre for Cosmological Physics,APC(CNRS),Universite Paris Diderot,Universite Sorbonne Paris Cite;Department of Physics and Astronomy,University of Tennessee;Ⅲ.Physikalisches Institut,Physikzentrum,RWTH Aachen University;High Energy Physics Laboratory,Tokyo Metropolitan University;Institut fur Kernphysik,Johannes-Gutenberg Universitat Mainz;Department of Physics and Astronomy,University of Sheffield;Department of Physics,Carleton University;California Institute of Technology,Kellogg Radiation Laboratory 106-38;Division of Theoretical Physics,Department of Mathematical Sciences,The University of Liverpool;Institute of Cosmology and Gravitation,University of Portsmouth;Cavendish Laboratory;Department of Astronomy and CCAPP,The Ohio State University;Dept.of Physics,Colorado School of Mines;Department of Physisc,University of Massachusetts;Department of Physics,Carnegie Mellon University;STFC Rutherford Appleton Laboratory;Department of Physics,George Washington University Virginia Campus;California Institute of Technology;
  • 中文刊名:KNWL
  • 英文刊名:中国物理C
  • 机构:Particle Data Group;Universita di Bologna and INFN,Dip.Scienze per la Qualita della Vita;University of Maryland,Department of Physics,College Park;Universit degli Studi di Roma "Tor Vergata";Albert Einstein Center for Fundamental Physics,Universitt Bern;Stefan Meyer Institute for Subatomic Physics,Austrian Academy of Sciences;Lab.Nazionali di Frascati dell'INFN;Pacific Northwest National Laboratory;Department of Physics and Astronomy,University of Oklahoma;University of Louisville;Physics Division,Lawrence Berkeley National Laboratory;CERN,European Organization for Nuclear Research;Department of Physics,The Ohio State University;COMPAS Group,Institute for High Energy Physics;Max-Planck-Institute of Physics;Department of Physics,University of Washington;Ludwig-Maximilians-Universitt,Fakultt fr Physik;Enrico Fermi Institute and Department of Physics,University of Chicago;Department of Physics,Columbia University;High Energy Physics Group,Blackett Laboratory,Imperial College;Jefferson Lab;Department of Physics,University of Virginia;Fermi National Accelerator Laboratory;Kavli Institute for Cosmological Physics,University of Chicago;Department of Physics and Astronomy,University of Sussex;Department of Physics,Northern Illinois University;Department of Physics and Astronomy,University of California;Michigan State University,Dept.of Physics and Astronomy;Department of Physics,Royal Holloway,University of London;INFN-Sezione di Napoli,Complesso Universitario Monte Sant'Angelo;Institut des Hautes Etudes Scientifiques;International Center for Advanced Studies(ICAS),UNSAM;Department of Physics and Astronomy,Northwestern University;Department of Physics,University of Colorado at Boulder;Nikhef,P.O.Box 41882,1009 DB Amsterdam,and University of Amsterdam;Institute for Particle Physics,ETH Zurich;University of Liverpool,Department of Physics,Oliver Lodge Lab;Physikalisches Institut,Universitt Bonn;Helsinki Institute of Physics;University of Helsinki;Department of Physics;Budker Institute of Nuclear Physics SB RAS;Novosibirsk State University;King's College London,Department of Physics;Departamento de Fisica Teorica,Instituto de Fisica,Universidad Nacional Autonoma de Mexico;Moscow Institute of Physics and Technology(State University);Department of Astronomy,University of Illinois;Department of Physics,University of Illinois;University of Hamburg;Deutsches Elektronen-Synchrotron DESY;Denys Wilkinson Building,Department of Physics,University of Oxford;University of Pittsburgh,Department of Physics and Astronomy;Department of Physics and Astronomy,Tufts University;CEA Saclay,DSM/IRFU/SPP;Department of Physics,University of Warwick;University of Minnesota,School of Physics and Astronomy;Argonne National Laboratory;Johns Hopkins University;Institucio Catalana de Recerca iEstudis Avancats,Institut de Fisica d'Altes Energies;School of Physics,University College Dublin;TIFR;Institut fur Theoretische Physik,Universitat Tubingen;Santa Cruz Institute for Particle Physics,University of California;KEK,High Energy Accelerator Research Organization;Institut fr Kernphysik and Institute for Advanced Simulation,Forschungszentrum Julich;Department of Physics,University of Tokyo;Department of Physics,Hillsdale College;Institute for Theoretical Physics,Heidelberg University;Laboratory of Elementary-Particle Physics,Cornell University;IFIC—Instituto de Fisica Corpuscular,Universitat de Valencia-C.S.I.C.;Department of Physics,Tohoku University;Kobayashi-Maskawa Institute,Nagoya University;Department of Physics and Astronomy,University of Delaware;Bartol Research Institute,University of Delaware;Yukawa Institute for Theoretical Physics,Kyoto University;Department of Physics,Stanford University;SLAC National Accelerator Laboratory;Los Alamos National Laboratory;LAL,IN2P3-CNRS et Univ.;Department of Particle Physics,Tel-Aviv University;University of Erlangen-Nuremberg,Erlangen Centre for Astroparticle Physics;Nuclear Science Division,Lawrence Berkeley National Laboratory;Helmholtz-Institut fur Strahlen- und Kernphysik,Universitat Bonn;University of Victoria;Institute for Particle Physics Phenomenology,Department of Physics,University of Durham;Institute of Physics,University of Basel;Yonsei University,Department of Physics;Department of Physics and Astronomy,University College London;Department of Physics,Syracuse University;School of Natural Science,Institute for Advanced Study;Institute for Astronomy,University of Edinburgh;GSI,Helmholtzzentrum fr Schwerionenforschung;Division of Science,City College of New York;Physics Department,Brookhaven National Laboratory;INFN and Dipartimento di Fisica,Universita di Pisa;Centre for Cosmology,Particle Physics and Phenomenology(CP3),Universite catholique de Louvain;Department fur Physik,Universitat Siegen;Department of Physics,University of California at San Diego;INFN Sezione di Cagliari,Cittadella Universitaria di Monserrato;Department of Physics and Astronomy,Louisana State University;Fysikum,Stockholms Universitet,AlbaNova University Centre;Deparment of Physics,Indiana University;INAF-OATS;DESY;The Space Sciences Laboratory(SSL),University of California;Kavli IPMU(WPI),Todai Institutes for Advanced Study,University of Tokyo;Department of Physics,University of California;Brown University,Department of Physics;INFN,Sez.di Milano-Bicocca;Dpto,de Fisica Teorica y del Cosmos & C.A.F.P.E.,Universidad de Granada;PRISMA Cluster of Excellence and Mainz Institute for Theoretical Physics,Johannes Gutenberg University;Department of Particle Physics and Astrophysics,Weizmann Institute of Science;SISSA/INFN;INRNE,Bulgarian Academy of Sciences;Department of Physics and Astronomy,University of Alabama;Departament de Fisica,Universitat Autonoma de Barcelona;Georg-August-Universitat Gottingen,Ⅱ.Physikalisches Institut;HH Wills Physics Laboratory,University of Bristol;Max-Planck-Institut fur Physik(Werner-Heisenberg-Institut);DOE;National Research Nuclear University "MEPhI"(Moscow Engineering Physics Institute);School of Physics and Astronomy,University of Southampton;LPTHE,UPMC Universite de Paris 6;Rudolf Peierls Centre for Theoretical Physics,University of Oxford;Niels Bohr Institute;Ecole Polytechnique Federale de Lausanne(EPFL);Physics Department,Duke University;Department of Physics,University of Cincinnati;Department of Physics and Astronomy,University of British Columbia;Department of Astronomy and Theoretical Physics,Lund University;School of Physics,Monash University;Paris Centre for Cosmological Physics,APC(CNRS),Universite Paris Diderot,Universite Sorbonne Paris Cite;Department of Physics and Astronomy,University of Tennessee;Ⅲ.Physikalisches Institut,Physikzentrum,RWTH Aachen University;High Energy Physics Laboratory,Tokyo Metropolitan University;Institut fur Kernphysik,Johannes-Gutenberg Universitat Mainz;Department of Physics and Astronomy,University of Sheffield;Department of Physics,Carleton University;California Institute of Technology,Kellogg Radiation Laboratory 106-38;Division of Theoretical Physics,Department of Mathematical Sciences,The University of Liverpool;Department fur Physik,University of California at San Diego;Institute of Cosmology and Gravitation,University of Portsmouth;Cavendish Laboratory;Department of Astronomy and CCAPP,The Ohio State University;Dept.of Physics,Colorado School of Mines;Department of Physisc,University of Massachusetts;Department of Physics,Carnegie Mellon University;STFC Rutherford Appleton Laboratory;Department of Physics,George Washington University Virginia Campus;California Institute of Technology;
  • 出版日期:2016-10-15
  • 出版单位:Chinese Physics C
  • 年:2016
  • 期:v.40
  • 基金:supported by PAPIIT(DGAPA-UNAM) project IN106913;; CONACyT(Mexico) project 151234;; supported in part by the National Science Foundation under grant no.PHY-1519175;; supported by Fermilab,that is operated by Fermi Research Alliance,LLC under Contract No.DE-AC02-07CH11359 with the United States Department of Energy;; supported by the European Commission through the Marie Curie Career Integration Grant 631962;; by the Helmholtz Association;; supported by the ANR HiggsNet grant;; supported by the grant DE-SC0009919 of the United States Department of Energy
  • 语种:英文;
  • 页:KNWL201610005
  • 页数:217
  • CN:10
  • ISSN:11-5641/O4
  • 分类号:136-352
摘要
The Review summarizes much of particle physics and cosmology.Using data from previous editions,plus 3,062 new measurements from 721 papers,we list,evaluate,and average measured properties of gauge bosons and the recently discovered Higgs boson,leptons,quarks,mesons,and baryons.We summarize searches for hypothetical particles such as supersymmetric particles,heavy bosons,axions,dark photons,etc.All the particle properties and search limits are listed in Summary Tables.We also give numerous tables,figures,formulae,and reviews of topics such as Higgs Boson Physics,Supersymmetry,Grand Unified Theories,Neutrino Mixing,Dark Energy,Dark Matter,Cosmology,Particle Detectors,Colliders,Probability and Statistics.Among the 117 reviews are many that are new or heavily revised,including new reviews on Pentaquarks and Inflation.
        The Review summarizes much of particle physics and cosmology.Using data from previous editions,plus 3,062 new measurements from 721 papers,we list,evaluate,and average measured properties of gauge bosons and the recently discovered Higgs boson,leptons,quarks,mesons,and baryons.We summarize searches for hypothetical particles such as supersymmetric particles,heavy bosons,axions,dark photons,etc.All the particle properties and search limits are listed in Summary Tables.We also give numerous tables,figures,formulae,and reviews of topics such as Higgs Boson Physics,Supersymmetry,Grand Unified Theories,Neutrino Mixing,Dark Energy,Dark Matter,Cosmology,Particle Detectors,Colliders,Probability and Statistics.Among the 117 reviews are many that are new or heavily revised,including new reviews on Pentaquarks and Inflation.
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    1 On leave from LPTHE,UMR 7589,CNHS,Paris,France
    The situation is significantly worse near thresholds,e.g.the tt production threshold.An overview of some of the methods used in such cases is to be found for example in Ref.31.
    There is an important caveat to this statement:at sufficiently high orders,perturbative series generally suffer from"renormalon"divergencesα_s~n n!(reviewed in Ref.23).This phenomenon is not usually visible with the limited number of perturbative terms available today.However it is closely connected with non-perturbative contributions and sets a limit on the possible precision of perturbative predictions.The cancellation of scale dependence will also ultimately be affected by this renormalon-induced breakdown of perturbation theory.
    LO is generally taken to mean the lowest order at which a quantity is non-zero.This definition is nearly always unambiguous,the one major exception being for the case of the hadronic branching ratio of virtual photons,Z,τ,etc.,for which two conventions exist:LO can either mean the lowest order that contributes to the hadronic branching fraction,i.e.the term"1"in Eq.(9.7);or it can mean the lowest order at which the hadronic branching ratio becomes sensitive to the coupling,n=1 in Eq.(9.8),as is relevant when extracting the value of the coupling from a measurement of the branching ratio.Because of this ambiguity,we avoid use of the term"LO"in that context.
    Processes with jets or photons in the final state have divergent cross sections unless one places cut on the jet or photon momentum.Accordingly they are discussed below in Section 9.2.3.2.
    To be precise one should be aware of two causes of the divergence of perturbative series.That which interests us here is associated with the presence of a new large parameter(e.g.ratio of scales).It is distinct from the"renormalon"induced factorial divergences of perturbation theory that were discussed above.
    Whether or not this happens depends on the quantity being resummed.A classic example involves jet rates in e~+e~-collisions as a function of a jet-resolution parameter y_(cut).The logarithms of 1/y_(cut)exponentiate for the k_t(Durham)jet algorithm[154],but not[155]for the JADE algorithm[156](both are discussed below in Sec.9.3.1.1).
    The program ARIADNE[201]has also been widely used for simulating e~+e~-and DIS collisions.
    A number of prescriptions also exist for setting the scale automatically,e.g.Refs.214-217,eliminating uncertainties from scale variation,though not from the truncation of the perturbative series itself.Recently,there have also been studies of how to estimate uncertainties from missing higher orders that go beyond scale variations[218,219,220].
    The time evolution ofα_s combinations can be followed by consulting Refs.[330-332]as well as earlier editions of this Review.
    In most practical cases,this procedure arrives at similar values as obtained from the'range averaging'method which we used in previous Reviews,while it avoids potential shortcomings and biases of the latter.
    Note that for jet production at a hadron collider,only NLO predictions are available,while for the structure functions full NNLO was utilized.
    The weighted average,treating all inputs as uncorrelated measurements with Gaussian uncertainties,results inα_s(M_Z~2)=0.11810±0.00078 with x~2/d.o.f.=3.7/5.Requiring x~2/d.o.f.to reach unity calls for an overall correlation factor of 0.28,which increases the overall uncertainty to±0.00114.
    We note,however,that in many such studies,like those based on exclusive states of jet multiplicities,the relevant energy scale of the measurement is not uniquely defined.For instance,in studies of the ratio of 3-to 2-jet cross sections at the LHC,the relevant scale was taken to be the average of the transverse momenta of the two leading jets[381],but could alternatively have been chosen to be the transverse momentum of the 3~(rd)jet.
    There is no generally accepted convention to write the quartic term.Our numerical coefficient simplifies Eq.(10.3a)below and the squared coupling preserves the relation between the number of external legs and the power counting of couplings at a given loop order.This structure also naturally emerges from physics beyond the SM,such as supersymmetry.
    We emphasize that in the fits described in Sec.10.6 and Sec.10.7the values of the SM parameters are affected by all observables that depend on them.This is of no practical consequence forαand G_f,however,since they are very precisely known.
    In the spirit of the Fermi theory,we incorporated the small propagator correction,3/5 m_μ~2/M_W~2,into△r(see below).This is also the convention adopted by the MuLan collaboration[11].While this breaks with historical consistency,the numerical difference was negligible in the past.
    In practice,α(Mz)is directly evaluated in the ms scheme using the FORTRAN package GAPP[21],including the QED contributions of both leptons and quarks.The leptonic three-loop contribution in the on-shell scheme has been obtained in Ref.22.
    Other authors[46]advocate to evaluate and quote m_c(μ=3 GeV)instead.We use m_c(μ=m_c)because in the global analysis it is convenient to nullify any explicitly m_c dependent logarithms.Note also that our uncertainty for m_c(and to a lesser degree for m_b)is larger than in Refs.46 and 47,for example.The reason is that we determine the continuum contribution for charm pair production using only resonance data and theoretical consistency across various sum rule moments,and then use any difference to the experimental continuum data as an additional uncertainty.We also include an uncertainty for the condensate terms which grows rapidly for higher moments in the sum rule analysis.
    All explicit numbers quoted here and below include the two-and three-loop corrections described near the end of Sec.10.2.
    We use here slightly different definitions(and to avoid confusion also a different notation)for the coefficients of these four-Fermi operators than we did in previous editions of this Review.The new couplings[80]are defined in the static limit,Q~2→0,with specific radiative corrections included,while others(more experiment specific ones)are assumed to be removed by the experimentalist.They are convenient in that their determinations from very different types of processes can be straightforwardly combined.
    Note thatσ_(had)receives additional EW corrections that are not captured in the partial widths[163,153],but they only enter at twoloop order.
    In what follows,we summarize the most important aspects of g_μ-2,and give some details on the evaluation in our fits.For more details see the dedicated contribution on"The Muon Anomalous Magnetic Moment"in this Review.There are some numerical differences,which are well understood and arise because internal consistency of the fits requires the calculation of all observables from analytical expressions and common inputs and fit parameters,so that an independent evaluation is necessary for this Section.Note,that in the spirit of a global analysis based on all available information we have chosen here to use an analysis[20]which considers the r decay data,as well.
    Alternatively,one can use A_e=0.1481±0.0027,which is from LEP 1 alone and in excellent agreement with the SM,and obtain A_b=0.893±0.022 which is 1.9σlow.This illustrates that some of the discrepancy is related to the one in A_(LR).
    1 In the case of neutrinos,it is possible that the electroweak symmetry breaking mechanism plays only a partial role in generating the observed neutrino masses,with additional contributions at a higher scale via the so called see-saw mechanism.
    2Another solution to the naturalness problem is to lower the fundamental scale of quantum gravity,like for instance in models with large extra-dimensions,see Ref.[8].
    3 Similarly at the Tevatron where the CDF and DO experiments have gathered approximately 10 fb-1 of data at 1.96 TeV,the predicted numbers of SM Higgs boson events produced per experiment are approximately 10,000 and 2,000 events in the gluon fusion and VH associated production,respectively.
    4 In the combination performed by the ATLAS and CMS experiments the systematic uncertainties on these parameters are taken into account by allowing these parameters to vary in the fit.
    5Complete classifications of D=8 operators have recently appeared in the literature,see Ref.[222].Still,in this review,the EFT Lagrangians will be truncated at the level of dimension-6 operators.
    6There remains an accidental flat direction[227]in the fit of anomalous gauge boson couplings using LEP2 data on diboson production alone.This flat direction can be lifted when LHC Higgs data are considered[228].
    7For a pedagogical introduction to models of partial compositeness,see Ref.[248].
    8Observe that in the SM sections of this review,H denotes the SM Higgs,whereas in the sections about SUSY,or extensions of the SM with two Higgs doublets,H is used for the heaviest CP-even Higgs boson,since this is the standard notation in the literature,and the125 GeV SM-like light Higgs boson will be denoted by h.
    9 Additional gauge interactions in the UMSSM contribute to this increase with a term of O{g′_1~2(Q_(φ2)~2 cos~2β+Q_(φ1)~2 sin~2β)).
    10 For instance in the SO(5)/SO(4)composite models,when the top quark is embedded into a spinorial representation of SO(5),thenγ=0and when it is part of a 5,10 or 14 representation,α=0 as it can be inferred by looking at the structure of the H-dependent invariants built out of these representations[394].The coefficientγalso generically comes with an extra power of the top compositeness fractions.
    1 For lattice QCD inputs,we use the averages from Ref.[14]whenever possible,unless the minireviews[10,15]choose other values.We only use unquenched lattice QCD results.Hereafter,the first error is statistical and the second is systematic,unless mentioned otherwise.
    In our convention the electric charge is Q=T_3+F/2 and all our spinor fields are left-handed.
    Equivalently,the SU(2)_L and U(1)_Y couplings are denoted as g=g_2 and g'=(3/5)~(1/2)g_1.One also usesα_s=α_3=(g_3~2/4π),α_(EM)=(e~2/4π)with e=g sinθ_W and sin~2θ_W=(g')~2/(g~2+(g')~2).
    Useful references on group theory in the present context include[15]and refs.therein.
    The solution of[28]relies on the absence of the fundamental superpotential termμH_u H_d(orμ5_H5_H).This is ensured by a U(1)_R.The latter clashes with typical superpotentials for the GUT breaking sector.However,higher-dimensional or stringy GUTs,where the triplet Higgs is simply projected out,can be consistent with the U(1)_R symmetry.
    See however[40].
    The DR scheme is frequently used in a supersymmetric regularization[63].The renormalization transformation of the gauge coupling constants from MS to DR scheme is given in Ref.[64].For an alternative treatment using holomorphic gauge couplings and NSVZβ-functions see e.g.[65].
    It is interesting to note that a ratio M_*/M_c~100,needed for gauge coupling unification to work in orbifold GUTs,is typically the maximum value for this ratio consistent with perturbativity[78].
    Adding extra vector-like sets of fields,e.g.two fermions which only transform under U(1)and have charges Y and-Y,is considered to violate minimality.
    The value ofη~(CC)deduced from Ref.1 is found to be a factor of two too small;η~(CC)of Eq.(19.9)agrees with Refs.[2,3].

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