Determination of the Dynamic ITER Energy Confinement Time Scalings

We derive the differential equation, which is satisfied by the ITER scalings for the dynamic energy confinement time. We show that this differential equation can also be obtained from the differential equation for the energy confinement time, derived from the energy balance equation, when the plasma is near the steady state. We find that the values of the scaling parameters are linked to the second derivative of the power loss, estimated at the steady state. As an example of an application, the solution of the differential equation for the energy confinement time is compared with the profile obtained by solving numerically the balance equations (closed by a transport model) for a concrete Tokamak-plasma.

HIGHLIGHTS OF THE 2014 EDITION OF THE REVIEW OF PARTICLE PHYSICS

899 new papers with 3283 new measurements Over 330 papers from LHC experiments （ATLAS, CMS, and LHCb）.

NEUTRINO BEAM LINES AT HIGH-ENERGY PROTON SYNCHROTRONS

Revised September 2013 with numbers verified by representatives of the synchrotrons （contact C.-J. Lin, LBNL）. For existing （future） neutrino beam lines the latest achieved （design） values are given.

Resolving Hubble tension with quintom dark energy model

Recent low-redshift observations have yielded the present-time Hubble parameter value H0=74 kms^-1 Mpc^-1.This value is approximately 10%higher than the predicted value of Ho=67.4 kms^-1 Mpc^-1,based on Planck's observations of the Cosmic Microwave Background radiatio n(CMB)and the AC DM model.Phenomenologically,we show that,by adding an extra component,X,with negative density to the Friedmann equation,it can address the Hubble tension without changing the Planck's constraint on the matter and dark energy densities.To achieve a sufficiently small extra negative density,its equation-of-state parameter must satisfy 1/3 ≤ wx ≤ 1.We propose a quintom model of two scalar fields that realizes this condition and potentially alleviate the Hubble tension.One scalar field acts as a quintessence,while another "Wphantom" scalar con formally couples to matter such that a viable cosmological scenario is achieved.The model only depends on two parameters,心and 6,which represent the rolling tendency of the self-interacting potential of the quintessenee and the strength of the conformal phantom-matter coupling,respectively.The toy quintom model with H0=73.4 kms^-1 Mpc^-1(Quintom I)yields a good Supernovae-Ia luminosity fit and acceptable rBAO fit but slightly small acoustic multipole lA=285.54.A full parameter scan revealed that the quintom model was superior to the ACDM model in certain regions of the parameter space,0.02<δ<0.10,Ω(0)m<0.31,while significantly alleviating the Hubble tension,although it is not completely resolved.A benchmark quintom model.Quintom II,is presented as an example.

REVIEW OF PARTICLE PHYSICS

The Review summarizes much of particle physics and cosmology. Using data from previous editions, plus 3,283 new measurements from 899 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 heavy neutrinos, supersymmetric and technicolor particles, 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 Supersymmetry, Extra Dimensions, Particle Detectors, Probability, and Statistics. Among the 112 reviews are many that are new or heavily revised including those on： Dark Energy, Higgs Boson Physics, Electroweak Model, Neutrino Cross Section Measurements, Monte Carlo Neutrino Generators, Top Quark, Dark Matter, Dynamical Electroweak Symmetry Breaking, Accelerator Physics of Colliders, High-Energy Collider Parameters, Big Bang Nucleosynthesis, Astrophysical Constants and Cosmological Parameters. A booklet is available containing the Summary Tables and abbreviated versions of some of the other sections of this full Review. All tables, listings, and reviews （and errata） are also available on the Particle Data Group website： http ：//pdg. lbl. gov.

ACCELERATOR PHYSICS OF COLLIDERS

Revised August 2013 by M.J. Syphers （MSU） and F. Zimmermann （CERN）.29.1. Luminosity This article provides background for the High-Energy Collider Parameter Tables that follow. The number of events, Nexp, is the product of the cross section of interest,

ELECTROWEAK MODEL AND CONSTRAINTS ON NEW PHYSICS

Revised November 2013 by J. Erler （U. Mexico） and A. Freit＆s （Pittsburgh U.）.10.1 Introduction 10.2 Renormalization and radiative corrections

ONLINE PARTICLE PHYSICS INFORMATION

1. IntroductionThe collection of online information resources in particle physics and related areas presented in this chapter is of necessity incomplete. An expanded and regularly updated online version can be found at：

STATUS OF HIGGS BOSON PHYSICS

Written November 2013 by M. Carena （Fermi National Accelerator Laboratory and the University of Chicago）, C. Grojean （ICREA at IFAE, Universitat Autbnoma de Barcelona）, M, Kado （Laboratoire de l＇Accelerateur Lineaire, LAL and CERN）, and V. Sharma （University of California San Diego）.

DARK ENERGY

Written November 2013 by M. J. Mortonson （UCB, LBL）, D. H. Weinberg （OSU）, and M. White （UCB, LBL）.26.1. Repulsive Gravity and Cosmic Acceleration In the first modern cosmological model, Einstein [1] modified his field equation of General Relativity （GR）, introducing a ＂cosmological term＂ that enabled a solution with time-independent spatially homogeneous matter density Pm and constant positive space curvature.

PARTICLE DETECTORS FOR NON-ACCELERATOR PHYSICS

Updated 2013 （see the various sections for authors）.34.1. Introduction Non-accelerator experiments have become increasingly important in particle physics. These include classical cosmic ray experiments, neutrino oscillation measurements, and searches for double-beta decay, dark matter candidates, and magnetic monopoles.

BOTTOM MESONS(B=±1)B^+=u,B^0=d,B^0=db,B^-=b,similarly for B~*'s

Many measurements of B decays involve admixtures of B hadrons. Previously we arbitrarily included such admixtures in the B±section, but because of their importance we have created two new sections：

N BARYONS(S=0,I=1/2)p,N^+=uud;n,N^0=udd

p MASS （atomic mass units u）The mass is known much more precisely in u （atomic mass units） than in MeV. See the next data block.

BOTTOM,CHARMED MESONS(B=C=±1)B_c^+=c,B_c^-=cb,similarly for B_c~*'s

I（JP） = 0（0-）I, J, P need confirmation.Quantum numbers shown are quark-model predictions.

INTRODUCTION

1. Overview The Review of Particle Physics and the abbreviated version, the Particle Physics Booklet, are reviews of the field of Particle Physics. This complete Review includes a compilation/evaluation of data on particle properties, called the ＂Particle Listings.＂ These Listings include 3,283 new measurements from 899 papers, in addition to the 32,153 measurements from 8,944 papers that first appeared in previous editions [1].

BOTTOM BARYONS(B=-1)∧_b^0=udb,≡_b^0=usb,≡_b^-=dsb,Ω_b^-=ssb

In the quark model, a ∧b0 is an isospin-0 udb state. The lowest ∧b0 ought to have JP = 1/2＋. None of I, J, or P have actually been measured.

CHARMED BARYONS(C=+1)∧_c^+=udc,∑_c^(++)=uuc,∑_c^+=udc,∑_c^0=ddc,≡_c^+=usc,≡_c^0=dsc,Ω_c^0=ssc

CHARMED BARYONS Revised March 2012 by C.G. Wohl （LBNL）. There are 17 known charmed baryons, and four other candidates not well enough established to be promoted to the Summary Tables.＊ Fig. l（a） shows the mass spectrum,

∧ BARYONS(S=-1,I=0)∧~0=uds

We have omitted some results that have been superseded by later experiments. See our earlier editions.

QUARKS

QUARK MASSESUpdated Jan 2014 by A.V. Manohar （University of California, San Diego） and C.T. Sachrajda （University of Southampton）

SU(3) ISOSCALAR FACTORS AND REPRESENTATION MATRICES

Written by R.L. Kelly （LBNL）. The most commonly used SU（3） isoscalar factors, corresponding to the singlet, octet, and deeuplet content of 8 8 and 10 8, are shown at the right. The notation uses particle names to identify the coefficients, so that the pattern of relative couplings may be seen at a glance. We illustrate the use of the coefficients below.