• #### Dark Matter as a Trigger for Periodic Comet Impacts

Although statistical evidence is not overwhelming, possible support for an approximately 35 million year periodicity in the crater record on Earth could indicate a nonrandom underlying enhancement of meteorite impacts at regular intervals. A proposed explanation in terms of tidal effects on Oort cloud comet perturbations as the Solar System passes through the galactic midplane is hampered by lack of an underlying cause for sufficiently enhanced gravitational effects over a sufficiently short time interval and by the time frame between such possible enhancements. We show that a smooth dark disk in the galactic midplane would address both these issues and create a periodic enhancement of the sort that has potentially been observed. Such a disk is motivated by a novel dark matter component with dissipative cooling that we considered in earlier work. We show how to evaluate the statistical evidence for periodicity by input of appropriate measured priors from the galactic model, justifying or ruling out periodic cratering with more confidence than by evaluating the data without an underlying model. We find that, marginalizing over astrophysical uncertainties, the likelihood ratio for such a model relative to one with a constant cratering rate is 3.0, which moderately favors the dark disk model. Our analysis furthermore yields a posterior distribution that, based on current crater data, singles out a dark matter disk surface density of approximately 10 solar masses per square parsec. The geological record thereby motivates a particular model of dark matter that will be probed in the near future.
Dark matterCometSunSolar systemGalaxyStatisticsEarthExergyCoolingMeteorites...
• #### Spontaneous R-Symmetry Breaking in O'Raifeartaigh Modelsver. 3

We study the question of whether spontaneous U(1)_R breaking can occur in O'Raifeartaigh-type models of spontaneous supersymmetry breaking. We show that in order for it to occur, there must be a field in the theory with R-charge different from 0 or 2. We construct the simplest O'Raifeartaigh model with this property, and we find that for a wide range of parameters, it has a meta-stable vacuum where U(1)_R is spontaneously broken. This suggests that spontaneous U(1)_R breaking actually occurs in generic O'Raifeartaigh models.
Supersymmetry breakingR-symmetryU(1)VacuumField...
• #### Spontaneous R-symmetry Breaking with Multiple Pseudomoduli

We examine generalized O'Raifeartaigh models that feature multiple tree-level flat directions and only contain fields with R-charges 0 or 2. We show that spontaneous R-breaking at up to one-loop order is impossible in such theories. Specifically, we prove that the R-symmetric origin of field space is always a local minimum of the one-loop Coleman-Weinberg potential, generalizing an earlier result for the case of a single flat direction. This result has consequences for phenomenology and helps elucidate the behavior of various models of dynamical SUSY breaking.
Supersymmetry breakingEffective potentialSuperpotentialZero modeWess-Zumino modelSupersymmetryColeman-Weinberg potentialGauge fieldTachyonCompleteness...
• #### Magnetism induced by vacuum polarization at the gold-monolayer interface

Giant magnetization of polyalanine monolayers on gold observed in resent years along with unusual large spin selectivity, the potential of the film and its temperature dependence are all explained in the context of vacuum polarization at the gold-monolayer interface. The enhancement is directly related to the fine structure constant, and involves a change in basic physical parameters including changes in the permeability of the vacuum and in the local zero point energy of the gold monolayer interface. Formation of an ordered state by the self-assembly process and the interaction of the monolayer with the gold plasmons form a new state of matter that can interact strongly with the zero point energy.
Vacuum polarizationZero-point energySelf-assemblyA giantsPermeabilityState of matterFine structure constantPlasmonMagneticsFormate...
• #### Dynamical Supersymmetry Breaking at Low Energiesver. 2

Conventional approaches to supersymmetric model building suffer from several naturalness problems: they do not explain the large hierarchy between the weak scale and the Planck mass, and they require fine tuning to avoid large flavor changing neutral currents and particle electric dipole moments. The existence of models with dynamical supersymmetry breaking, which can explain the hierarchy, has been known for some time, but efforts to build such models have suffered from unwanted axions and difficulties with asymptotic freedom. In this paper, we describe an approach to model building with supersymmetry broken at comparatively low energies which solves these problems, and give a realistic example.
Supersymmetry breakingAsymptotic freedomElectric dipole momentSupersymmetryAxionPlanck scaleEnergyParticles...
• #### Dynamical Supersymmetry Breaking on Quantum Moduli Spaces

Supersymmetry breaking by the quantum deformation of a classical moduli space is considered. A simple, non-chiral, renormalizable model is presented to illustrate this mechanism. The well known, chiral, $SU(3) \times SU(2)$ model and its generalizations are shown to break supersymmetry by this mechanism in the limit $\Lambda_2 \gg \Lambda_3$. Other supersymmetry breaking models, with classical flat directions that are only lifted quantum mechanically, are presented. Finally, by integrating in vector matter, the strongly coupled region of chiral models with a dynamically generated superpotential is shown to be continuously connected to a weakly coupled description in terms of confined degrees of freedom, with supersymmetry broken at tree level.
SuperpotentialSupersymmetrySupersymmetry breakingExpectation ValueKahler potentialVacuum energyInstantonDegree of freedomGaugino condensationQuark...
• #### Testing the Minimal Direct Gauge Mediation at the LHC

We reexamine the models with gauge mediation in view of the minimality. As a result, we arrive at a very simple model of direct gauge mediation which does not suffer from the flavor problems nor the CP problems. We show that the parameter space which is consistent with the Higgs boson mass at around 126 GeV can be tested through the stable stau searches at the 14TeV run of the LHC. The gravitino is a viable candidate for a dark matter. We also give a short discussion on a possible connection of our model to the recently discovered X-ray line signal at 3.5 keV in the XMM Newton X-ray observatory data.
SupersymmetryNext to lightest supersymmetric particleGravitinoHiggs boson massDark matterMinimal supersymmetric Standard ModelSupersymmetry breakingElectroweak symmetry breakingRenormalization groupYukawa coupling...
• #### On the relative importance of second-order terms in relativistic dissipative fluid dynamicsver. 2

In Denicol et al., Phys. Rev. D 85, 114047 (2012), the equations of motion of relativistic dissipative fluid dynamics were derived from the relativistic Boltzmann equation. These equations contain a multitude of terms of second order in Knudsen number, in inverse Reynolds number, or their product. Terms of second order in Knudsen number give rise to non-hyperbolic (and thus acausal) behavior and must be neglected in (numerical) solutions of relativistic dissipative fluid dynamics. The coefficients of the terms which are of the order of the product of Knudsen and inverse Reynolds numbers have been explicitly computed in the above reference, in the limit of a massless Boltzmann gas. Terms of second order in inverse Reynolds number arise from the collision term in the Boltzmann equation, upon expansion to second order in deviations from the single-particle distribution function in local thermodynamical equilibrium. In this work, we compute these second-order terms for a massless Boltzmann gas with constant scattering cross section. Consequently, we assess their relative importance in comparison to the terms which are of the order of the product of Knudsen and inverse Reynolds numbers.
Reynolds numberDissipationPermutationBoltzmann transport equationDissipative fluid dynamicsKnudsen numberBinary starProjection operatorRankingRelaxation time...
• #### Cosmology: from theory to data, from data to theory

Cosmology has come a long way from being based on a small number of observations to being a data-driven precision science. We discuss the questions "What is observable?", "What in the Universe is knowable?" and "What are the fundamental limits to cosmological knowledge?". We then describe the methodology for investigation: theoretical hypotheses are used to model, predict and anticipate results; data is used to infer theory. We illustrate with concrete examples of principled analysis approaches from the study of cosmic microwave background anisotropies and surveys of large-scale structure, culminating in a summary of the highest precision probe to date of the physical origin of cosmic structures: the Planck 2013 constraints on primordial non-Gaussianity.
Cosmic microwave backgroundCosmologyNon-GaussianityBispectrumPlanck missionStatisticsRandom FieldLight conesBayesianPrimordial Non-Gaussianities...
• #### Resonantly-Produced 7 keV Sterile Neutrino Dark Matter Models and the Properties of Milky Way Satellites

Sterile neutrinos produced through a resonant Shi-Fuller mechanism are arguably the simplest model for a dark matter interpretation origin of the recent unidentified X-ray line seen toward a number of objects harboring dark matter. Here, I calculate the exact parameters required in this mechanism to produce the signal. The suppression of small scale structure predicted by these models is consistent with Local Group and high-$z$ galaxy count constraints. Very significantly, the parameters necessary in these models to produce the full dark matter density fulfill previously determined requirements to successfully match the Milky Way Galaxy's total satellite abundance, the satellites' radial distribution and their mass density profile, or "too big to fail problem." I also discuss how further precision determinations of the detailed properties of the candidate sterile neutrino dark matter can probe the nature of the quark-hadron transition, which takes place during the dark matter production.
Dark matterLocal groupLepton numberSterile neutrinoSterile neutrino DMWarm dark matterAbundanceWDM particle massStructure formationAndromeda galaxy...
• #### Ya. B. Zeldovich (1914-1987): Chemist, Nuclear Physicist, Cosmologist

Ya.B. Zeldovich was a pre-eminent Soviet physicist whose seminal contributions spanned many fields ranging from physical chemistry to nuclear and particle physics, and finally astrophysics and cosmology. March 8, 2014 marks Zeldovich's birth centenary, and this article attempts to convey the zest with which Zeldovich did science, and the important role he played in fostering and mentoring a whole generation of talented Scientists.
GalaxyCosmologyBlack holeThe early UniverseCosmic microwave backgroundJeans instabilityPhase space causticNeutrinoEigenvalueGeneral relativity...
• #### Influence of small scale magnetic energy and helicity on the growth of large scale magnetic field

We have studied the influence of initially given small scale magnetic energy($E_M(0)$) and helicity($H_M(0)$) on the magnetohydrodynamics(MHD) dynamo using simulations and analytic methods. $E_M$(0) in small scale boosts the growth of the large scale magnetic field($\overline{{\bf B}}$). The rate is also proportional to $H_M(0)$; i.e., positive $H_M(0)$ is more effective than negative $H_M(0)$. $E_M$(0) and $H_M$(0) generate the additional electromotive force($EMF$) terms. The effect of initial conditions($IC$s) depends on magnetic diffusivity $\eta$, position of $IC$s $k_f$, and time($e^{-\eta k_f^2 t}$). Complete large scale $E_M$(t) and $H_M$(t) were derived using the mean field theory. It was discussed why large scale magnetic helicity should have the opposite sign of the injected kinetic helicity. The physical meaning of $H_M$ subject to $E_M$ was also briefly discussed.
HelicitySimulationsMagnetic helicityMHD dynamoMagnetohydrodynamicsMagnetic energyCurrent densityEddyMagnetic DiffusionFaraday's law of induction...
• #### Production of a sterile species: quantum kineticsver. 2

Production of a sterile species is studied within an effective model of active-sterile neutrino mixing in a medium in thermal equilibrium. The quantum kinetic equations for the distribution functions and coherences are obtained from two independent methods: the effective action and the quantum master equation. The decoherence time scale for active-sterile oscillations is $\tau_{dec} = 2/\Gamma_{aa}$, but the evolution of the distribution functions is determined by the two different time scales associated with the damping rates of the quasiparticle modes in the medium: $\Gamma_1=\Gamma_{aa}\cos^2\tm ; \Gamma_2=\Gamma_{aa}\sin^2\tm$ where $\Gamma_{aa}$ is the interaction rate of the active species in absence of mixing and $\tm$ the mixing angle in the medium. These two time scales are widely different away from MSW resonances and preclude the kinetic description of active-sterile production in terms of a simple rate equation. We give the complete set of quantum kinetic equations for the active and sterile populations and coherences and discuss in detail the various approximations. A generalization of the active-sterile transition probability \emph{in a medium} is provided via the quantum master equation. We derive explicitly the usual quantum kinetic equations in terms of the polarization vector'' and show their equivalence to those obtained from the quantum master equation and effective action.
Kinetic equationNeutrinoDensity matrixEffective actionMaster equationDegree of freedomSterile neutrinoMikheev-Smirnov-Wolfenstein effectMixing angleTwo-point correlation function...
• #### Bound states -- from QED to QCD

These lectures are divided into two parts. In Part 1 I discuss bound state topics at the level of a basic course in field theory: The derivation of the Schr\"odinger and Dirac equations from the QED Lagrangian, by summing Feynman diagrams and in a Hamiltonian framework. Less well known topics include the equal-time wave function of Positronium in motion and the properties of the Dirac wave function for a linear potential. The presentation emphasizes physical aspects and provides the framework for Part 2, which discusses the derivation of relativistic bound states at Born level in QED and QCD. A central aspect is the maintenance of Poincar\'e invariance. The transformation of the wave function under boosts is studied in detail in D=1+1 dimensions, and its generalization to D=3+1 is indicated. Solving Gauss' law for $A^0$ with a non-vanishing boundary condition leads to a linear potential for QCD mesons, and an analogous confining potential for baryons.
Bound stateScalar electrodynamicsHamiltonianPositroniumC++Quantum chromodynamicsFeynman diagramsCovarianceForm factorHadronization...
• #### Primordial Magnetic Helicity from Stochastic Electric Currents

We study the possibility that primordial magnetic fields generated in the transition between inflation and reheating posses magnetic helicity, $H_M$. The fields are induced by stochastic currents of scalar charged particles created during the mentioned transition. We estimate the rms value of the induced magnetic helicity by computing different four-point SQED Feynman diagrams. For any considered volume, the magnetic flux across its boundaries is in principle non null, which means that the magnetic helicity in those regions is gauge dependent. We use the prescription given by Berger and Field and interpret our result as the difference between two magnetic configurations that coincide in the exterior volume. In this case the magnetic helicity gives only the number of magnetic links inside the considered volume. We calculate a concrete value of $H_M$ for large scales and analyze the distribution of magnetic defects as a function of the scale. Those defects correspond to regular as well as random fields in the considered volume. We find that the fractal dimension of the distribution of topological defects is $D = 1/2$. We also study if the regular fields induced on large scales are helical, finding that they are and that the associated number of magnetic defects is independent of the scale. In this case the fractal dimension is $D=0$. We finally estimate the intensity of fields induced at the horizon scale of reheating, and evolve them until the decoupling of matter and radiation under the hypothesis of inverse cascade of magnetic helicity. The resulting intensity is high enough and the coherence length long enough to have an impact on the subsequent process of structure formation.
• #### Massive Milky Way Satellites in Cold and Warm Dark Matter: Dependence on Cosmology

We investigate the claim that the largest subhaloes in high resolution dissipationless cold dark matter (CDM) simulations of the Milky Way are dynamically inconsistent with observations of its most luminous satellites. We find that the inconsistency is largely attributable to the large values of \sigma_8 and n_s adopted in the discrepant simulations producing satellites that form too early and therefore are too dense. We find the tension between observations and simulations adopting parameters consistent with WMAP9 is greatly diminished making the satellites a sensitive test of CDM. We find the Via Lactea II halo to be atypical for haloes in a WMAP3 cosmology, a discrepancy that we attribute to its earlier formation epoch than the mean for its mass. We also explore warm dark matter (WDM) cosmologies for 1--4 keV thermal relics. In 1 keV cosmologies subhaloes have circular velocities at kpc scales ~ 60% lower than their CDM counterparts, but are reduced by only 10% in 4 keV cosmologies. Since relic masses < 2-3 keV are ruled out by constraints from the number of Milky Way satellites and Lyman-\alpha\ forest, WDM has a minor effect in reducing the densities of massive satellites. Given the uncertainties on the mass and formation epoch of the Milky Way, the need for reducing the satellite densities with baryonic effects or WDM is alleviated.
Dark matter subhaloCosmologyWarm dark matterWilkinson Microwave Anisotropy ProbeMilky WayCold dark matterBolshoi N-body cosmological simulationVia Lactea 2 simulationA dwarfsMilky Way satellite...
• #### Cosmological Fluid Mechanics with Adaptively Refined Large Eddy Simulations

We investigate turbulence generated by cosmological structure formation by means of large eddy simulations (LES) using AMR. In contrast to the widely used implicit LES, which resolve a limited range of length scales and treat the effect of turbulent velocity fluctuations below the grid scale solely by numerical dissipation, we apply a subgrid-scale (SGS) model for the numerically unresolved fraction of the turbulence energy. For simulations with AMR, we utilize a new methodology that allows us to adjust the scale-dependent energy variables in such a way that the sum of resolved and unresolved energies is globally conserved. We test our approach in simulations of randomly forced turbulence. To treat inhomogeneous turbulence, we introduce an adaptive Kalman filtering technique that separates turbulent velocity fluctuations on resolved length scales from the non-turbulent bulk flow. The latter is produced by the accretion of gas into the potential wells of halos. From the magnitude of the fluctuating part and the SGS turbulence energy, the total turbulent velocity dispersion can be estimated. As a cosmological test case, we perform large eddy simulations of the Santa Barbara cluster. Our model predicts a turbulent velocity dispersion around 500 km/s in the ICM, driven on length scales of a few Mpc. The low-density gas outside the accretion shocks, on the other hand, is nearly devoid of turbulence. Based on the turbulent velocity dispersion, it follows that the magnetic field in the ICM is typically a few microgauss if the generation of the field by the turbulent dynamo has saturated at redshift zero. The turbulent energy flux and dissipation rate predicted by the SGS model correspond to dynamical time scales of several Gyr, independent of numerical resolution. LES also offer promising perspectives for more advanced cosmological simulations, including feedback. [abridged]
TurbulenceDissipationLarge eddy simulationAccretionCosmologyIntra-cluster mediumVorticityMach numberStatisticsKalman filter...
• #### Extending the scope of models for large-scale structure formation in the Universever. 2

We propose a phenomenological generalization of the models of large-scale structure formation in the Universe by gravitational instability in two ways: we include pressure forces to model multi-streaming, and noise to model fluctuations due to neglected short-scale physical processes. We show that pressure gives rise to a viscous-like force of the same character as that one introduced in the adhesion model'', while noise leads to a roughening of the density field yielding a scaling behavior of its correlations.
PolytropesCosmologyLarge scale structureAdhesionVelocity dispersionDynamical evolutionCoarse grainingZeldovich approximationEuler equationsRenormalization group...
• #### Stochastic fluctuations and structure formation in the Universe

It is shown that the evolution of the density perturbations during certain eras of substantial entropy generation in the universe can be described in the scheme of the KPZ equation. Therefore, the influence on cosmological structure formation by stochastic forces arising from various dissipations can be studied through the universal characteristics of surface growth in $d=3+1$ dimensions. We identify eras of strong stochastic fluctuations and describe dynamically how these other dissipative sources of noise, besides initial (inflationary) quantum fluctuations, generate seeds of density perturbation with power law spectrum, including the Harrison-Zeldovich spectrum.
DissipationStructure formationCosmologyReheatingTwo-point correlation functionPrimordial density perturbationEntropyStandard ModelQuantum fluctuationFractal...
• #### Cosmic Star Formation Historyver. 2

Over the last decade and a half, an avalanche of new data from multiwavelength imaging and spectroscopic surveys has revolutionized our view of galaxy formation and evolution. Making sense of it all and fitting it together into a coherent picture remains one of astronomy's great challenges. Here we review the range of complementary techniques and theoretical tools that are allowing astronomers to map the cosmic history of star formation, heavy element production, and reionization of the universe from the cosmic "dark ages" to the present epoch. A consistent picture is emerging from modern galaxy surveys, whereby the star formation rate density peaked about 3.5 Gyr after the Big Bang, at redshift 1.9, and declined exponentially at later times, with an e-folding timescale of 3.9 Gyr. Half of the stellar mass observed today was formed before redshift 1.3. Less than 1% of today's stars formed during the epoch of reionization, at redshift greater than 6. Under the simple assumption of a universal initial mass function, the global stellar mass density inferred at any epoch matches reasonably well the time integral of all the preceding star formation activity, although a mild disagreement may still point to unresolved issues with the measurements, or to deviations in the stellar initial mass function from conventional assumptions. The assembly histories of the stellar component of galaxies and their central black holes were quite similar, offering evidence for the co-evolution of black holes and their host galaxies. The rise of the mean metallicity of the universe to about 0.001 solar by redshift six, one Gyr after the Big Bang, appears to have been accompanied by the production of fewer than ten hydrogen Lyman-continuum photons per baryon, a rather tight budget for cosmological deionization.
GalaxyLuminosityStar formation rateStar formationStellar massStarLuminosity functionInitial mass functionStellar populationsExtinction...
• #### Fluid Dynamics and Viscosity in Strongly Correlated Fluids

We review the modern view of fluid dynamics as an effective low energy, long wavelength theory of many body systems at finite temperature. We introduce the notion of a nearly perfect fluid, defined by a ratio $\eta/s$ of shear viscosity to entropy density of order $\hbar/k_B$ or less. Nearly perfect fluids exhibit hydrodynamic behavior at all distances down to the microscopic length scale of the fluid. We summarize arguments that suggest that there is fundamental limit to fluidity, and review the current experimental situation with regard to measurements of $\eta/s$ in strongly coupled quantum fluids.
Fluid dynamicsKinetic theoryShear viscosityViscosityTwo-point correlation functionDissipationEntropyTransport coefficientAdS/CFT correspondenceQuark-gluon plasma...
• #### Introductory lectures to large-N QCD phenomenology and lattice resultsver. 2

An elementary, pedagogical introduction to the large-N limit of QCD and to its phenomenological implications is presented, and a survey of lattice results in the 't Hooft limit is briefly discussed.
Quantum chromodynamicsQuarkGauge theoryYang-Mills theoryString theorySimulationsDeconfinementGlueballDegree of freedomSuper Yang-Mills theory...
• #### The Interstellar Environment of our Galaxy

We review the current knowledge and understanding of the interstellar medium of our galaxy. We first present each of the three basic constituents - ordinary matter, cosmic rays, and magnetic fields - of the interstellar medium, laying emphasis on their physical and chemical properties inferred from a broad range of observations. We then position the different interstellar constituents, both with respect to each other and with respect to stars, within the general galactic ecosystem.
StarInterstellar mediumIonizationGalaxySunMilky WayPulsarAbsorptivitySupernovaScale height...
• #### Effective WIMPs

The 'WIMP miracle' for the relic abundance of thermal dark matter motivates weak scale dark matter with renormalizable couplings to standard model particles. We study minimal models with such couplings that explain dark matter as a thermal relic. The models contain a singlet dark matter particle with cubic renormalizable couplings between standard model particles and 'partner' particles with the same gauge quantum numbers as the standard model particle. The dark matter has spin 0, 1/2, or 1, and may or may not be its own antiparticle. Each model has 3 parameters: the masses of the dark matter and standard model partners, and the cubic coupling. Requiring the correct relic abundance gives a 2-dimensional parameter space where collider and direct detection constraints can be directly compared. We focus on the case of dark matter interactions with colored particles. We find that collider and direct detection searches are remarkably complementary for these models. Direct detection limits for the cases where the dark matter is not its own antiparticle require dark matter masses to be in the multi-TeV range, where they are extremely difficult to probe in collider experiments. The models where dark matter is its own antiparticle are strongly constrained by collider searches for monojet and jets + MET signals. These models are constrained by direct detection mainly near the limit where the dark matter and partner masses are nearly degenerate, where collider searches become more difficult.
Dark matterQuarkRelic abundanceStandard ModelAntiparticleSupersymmetrySpin independentWeakly interacting massive particleDark matter particleChirality...
• #### Simplified Models for Dark Matter Interacting with Quarksver. 2

We investigate simplified models in which dark matter particles, taken to be either Dirac or Majorana fermions, couple to quarks via colored mediators. We determine bounds from colliders and direct detection experiments, and show how the interplay of the two leads to a complementary view of this class of dark matter models. Forecasts for future searches in light of the current constraints are presented.
Dark matterStandard ModelQuarkSpin independentMajorana dark matterElastic scatteringMajorana fermionDark matter particleComplete theoryEffective field theory...
• #### Isospin-Violating Dark Matter with Colored Mediators

In light of positive signals reported by the CDMS-II Si experiment and the recent results of the LUX and SuperCDMS experiments, we study isospin-violating dark matter scenarios assuming that the interaction of the dark matter is mediated by colored particles. We investigate the phenomenology of the model, including collider searches, flavor and CP phenomenology. A minimal possible scenario includes scalar dark matter and new vector-like colored fermions with masses of O(1) TeV as mediators. Such a scenario may be probed at the 14 TeV LHC, while flavor and CP constraints are stringent and severe tuning in the couplings is unavoidable. We also found that, as an explanation of the CDMS-II Si signal, isospin-violating fermionic dark matter models with colored scalar mediators are disfavored by the LHC constraints.
Dark matterStandard ModelQuarkYukawa couplingElectric dipole momentDown quarkDark matter modelCoupling constantEffective field theorySupersymmetry...
• #### Plasma Physics of Extreme Astrophysical Environments

Certain classes of astrophysical objects, namely magnetars and central engines of supernovae and gamma-ray bursts (GRBs), are characterized by extreme physical conditions not encountered elsewhere in the Universe. In particular, they possess magnetic fields that exceed the critical quantum field of 44 teragauss. Figuring out how these complex ultra-magnetized systems work requires understanding various plasma processes, both small-scale kinetic and large-scale magnetohydrodynamic (MHD). However, an ultra-strong magnetic field modifies the underlying physics to such an extent that many relevant plasma-physical problems call for building QED-based relativistic quantum plasma physics. In this review, after describing the extreme astrophysical systems of interest and identifying the key relevant plasma-physical problems, we survey the recent progress in the development of such a theory. We discuss how a super-critical field modifies the properties of vacuum and matter and outline the basic theoretical framework for describing both non-relativistic and relativistic quantum plasmas. We then turn to astrophysical applications of relativistic QED plasma physics relevant to magnetar magnetospheres and central engines of supernovae and long GRBs. Specifically, we discuss propagation of light through a magnetar magnetosphere; large-scale MHD processes driving magnetar activity and GRB jet launching and propagation; energy-transport processes governing the thermodynamics of extreme plasma environments; micro-scale kinetic plasma processes important in the interaction of intense magnetospheric electric currents with a magnetar's surface; and magnetic reconnection of ultra-strong magnetic fields. Finally, we point out that future progress will require the development of numerical modeling capabilities.
Neutron starMagnetarGamma ray burstMagnetosphere of a starPlasma physicsSupernovaStarMagnetohydrodynamicsSoft gamma repeaterNeutrino...
• #### Antimatter in the Universe : Constraints from Gamma-Ray Astronomy

We review gamma-ray observations that constrain antimatter - both baryonic and leptonic - in the Universe. Antimatter can be probed through ordinary matter, with the resulting annihilation gamma-rays providing indirect evidence for its presence. Although it is generally accepted that equal amounts of matter and antimatter have been produced in the Big Bang, gamma-rays have so far failed to detect substantial amounts of baryonic antimatter in the Universe. Conversely, positrons are abundantly observed through their annihilation in the central regions of our Galaxy and, although a wealth of astrophysical sources are plausible, their very origin is still unknown. As both antimatter questions - the source of the Galactic positrons and the baryon asymmetry in the Universe - can be investigated through the low energy gamma-ray channel, the mission concept of a dedicated space telescope is sketched out.
AntimatterPositronCosmologyCluster of galaxiesInterstellar mediumTelescopesBumpingGalactic CenterMilky WayCOMPTEL...
• #### Parallax Beyond a Kiloparsec from Spatially Scanning the Wide Field Camera 3 on the Hubble Space Telescope

We use a newly developed observing mode on the Hubble Space Telescope (HST) and Wide Field Camera 3 (WFC3), spatial scanning, to increase source sampling a thousand-fold and measure changes in source positions to a precision of 20--40 microarcseconds, more than an order of magnitude better than attainable in pointed observations. This observing mode can usefully measure the parallaxes of bright stars at distances of up to 5 kpc, a factor of ten farther than achieved thus far with HST. Long-period classical Cepheid variable stars in the Milky Way, nearly all of which reside beyond 1 kpc, are especially compelling targets for parallax measurements from scanning, as they may be used to anchor a determination of the Hubble constant to ~1%. We illustrate the method by measuring to high precision the parallax of a classical Cepheid, SY Aurigae, at a distance of more than 2 kpc, using 5 epochs of spatial-scan data obtained at intervals of 6 months. Rapid spatial scans also enable photometric measurements of bright Milky Way Cepheids---which would otherwise saturate even in the shortest possible pointed observations---on the same flux scale as extragalactic Cepheids, which is a necessity for reducing a leading source of systematic error in the Hubble constant. We demonstrate this capability with photometric measurements of SY Aur on the same system used for Cepheids in Type Ia supernova host galaxies. While the technique and results presented here are preliminary, an ongoing program with HST is collecting such parallax measurements for another 18 Cepheids to produce a better anchor for the distance scale.
StarParallaxCepheidTelescopesGeometric flatteningMilky WayPhotometryProper motionPoint spread functionOrientation...
• #### An unidentified line in X-ray spectra of the Andromeda galaxy and Perseus galaxy cluster

We identify a weak line at $E \sim 3.5$ keV in X-ray spectra of the Andromeda galaxy and the Perseus galaxy cluster -- two dark matter-dominated objects, for which there exist deep exposures with the XMM-Newton X-ray observatory. Such a line was not previously known to be present in the spectra of galaxies or galaxy clusters. Although the line is weak, it has a clear tendency to become stronger towards the centers of the objects; it is stronger for the Perseus cluster than for the Andromeda galaxy and is absent in the spectrum of a very deep "blank sky" dataset. Although for individual objects it is hard to exclude the possibility that the feature is due to an instrumental effect or an atomic line of anomalous brightness, it is consistent with the behavior of a line originating from the decay of dark matter particles. Future detections or non-detections of this line in multiple astrophysical targets may help to reveal its nature.
Andromeda galaxyDark matterPerseus ClusterXMM-NewtonDark matter decayEPIC PN cameraDM decay lineNGC 1275Effective areaInstrumental line...
• #### Relic neutrino decoupling including flavour oscillations

In the early universe, neutrinos are slightly coupled when electron-positron pairs annihilate transferring their entropy to photons. This process originates non-thermal distortions on the neutrino spectra which depend on neutrino flavour, larger for nu_e than for nu_mu or nu_tau. We study the effect of three-neutrino flavour oscillations on the process of neutrino decoupling by solving the momentum-dependent kinetic equations for the neutrino spectra. We find that oscillations do not essentially modify the total change in the neutrino energy density, giving N_eff=3.046 in terms of the effective number of neutrinos, while the small effect over the production of primordial 4He is increased by O(20%), up to 2.1 x 10^{-4}. These results are stable within the presently favoured region of neutrino mixing parameters.
NeutrinoNeutrino oscillationsFlavourNeutrino decouplingBig bang nucleosynthesisFlavour oscillationKinetic equationDensity matrixCosmic neutrino backgroundReheating...
• #### Magnetic Field Instabilities in Neutron Starsver. 2

Magnetic fields represent a crucial aspect of the physics and astrophysics of neutron stars. Despite its great relevance, the internal magnetic field configuration of neutron stars is very poorly constrained by the observations, and understanding its properties is a long-standing theoretical challenge. The investigation on the subject is focused on the search for those magnetic field geometries which are stable on several Alfv\en timescales, thus constituting a viable description of neutron star interiors. Assesing the stability of a given magnetic field geometry is therefore an important part of this research. So far only simple configurations, such as the purely poloidal or purely toroidal ones, have been studied in detail in perturbation theory and, most recently, by means of nonlinear magnetohydrodynamic simulations. Here we review the basic results of the state-of-the-art general relativistic nonlinear studies, discussing the present status of the field and its future directions.
InstabilityNeutron starSimulationsMagnetohydrodynamicsGravitational waveMagnetized neutron starMagnetic energyMagnetar Giant FlareStarMagnetic field strength...
• #### Angular fluctuations in the CXB: Is Fe 6.4 keV line tomography of the large-scale structure feasible?ver. 2

AGN are known to account for a major fraction, if not all, of the Cosmic X-ray background radiation. The dominant sharp spectral feature in their spectra is the 6.4 keV fluorescent line of iron, which may contribute as much as ~ 5-10 % to the CXB spectral intensity at ~ 2-6 keV. Due to cosmological redshift, the line photons detected at the energy E carry information about objects located at the redshift z=6.4/E-1. In particular, imprinted in their angular fluctuations is the information about the large-scale structure at redshift z. This opens a possibility to perform the Fe K_alpha line tomography of the cosmic large-scale structure. We show that detection of the tomographic signal at a ~100 sigma confidence requires an all-sky survey by an instrument with effective area of ~10 m^2 and field of view of ~1 deg^2. The signal is strongest for objects located at the redshift z~1, and at the angular scales corresponding to l ~ 100-300, therefore an optimal detection can be achieved with an instrument having a rather modest angular resolution of ~ 0.1-0.5 deg. For such an instrument, the CCD-type energy resolution of ~ 100-200 eV FWHM is entirely sufficient for the optimal separation of the signals originating at different redshifts. The gain in the signal strength which could potentially be achieved with energy resolution comparable to the line width, is nullified by the photon counting and AGN discreteness noise. Among the currently planned and proposed missions, these requirements are best satisfied by LOFT, despite the fact that it was proposed for entirely different purpose. Among others, clear detection should be achieved by WFXT (~ 20-35 sigma) and ATHENA (~ 10-20 sigma). eROSITA, in the course of its 4 years all-sky survey, will detect the tomographic signal only marginally.
Active Galactic NucleiCosmic X-ray backgroundSignal to noise ratioLuminosity functionLuminosityLarge scale structureLOFTFull width at half maximumStatisticsEffective area...
• #### Fe K emission from active galaxies in the COSMOS field

We present a rest-frame spectral stacking analysis of ~1000 X-ray sources detected in the XMM-COSMOS field in order to investigate the iron K line properties of active galaxies beyond redshift z~1. In Type I AGN that have a typical X-ray luminosity of Lx~1.5e44 erg/s and z~1.6, the cold Fe K at 6.4 keV is weak (EW~0.05keV), in agreement with the known trend. In contrast, high-ionization lines of Fe XXV and Fe XXVI are pronounced. These high-ionization Fe K lines appear to have a connection with high accretion rates. While no broad Fe emission is detected in the total spectrum, it might be present, albeit at low significance, when the X-ray luminosity is restricted to the range below 3e44 erg/s, or when an intermediate range of Eddington ratio around 0.1 is selected. In Type II AGN, both cold and high-ionzation lines become weak with increasing X-ray luminosity. However, strong high-ionization Fe K (EW~0.3 keV) is detected in the spectrum of objects at z>2, while no 6.4 keV line is found. It is then found that the primary source of the high-ionization Fe K emission is those objects detected with Spitzer-MIPS at 24 micron. Given their median redshift of z=2.5, their bolometric luminosity is likely to reach 10^13 Lsun and the MIPS-detected emission most likely originates from hot dust heated by embedded AGN, probably accreting at high Eddington ratio. These properties match those of rapidly growing black holes in ultra-luminous infrared galaxies at the interesting epoch (z=2-3) of galaxy formation.
Active Galactic NucleiLuminosityK-lineX-ray luminosityPhotometric redshiftXMM-COSMOS surveyAbsorptivityBlack holeIonizationAccretion...
• #### The Hubble flow around the Local Group

We use updated data on distances and velocities of galaxies in the proximity of the Local Group (LG) in order to establish properties of the local Hubble flow. For 30 neighbouring galaxies with distances 0.7 < D_LG < 3.0 Mpc, the Local flow is characterized by the Hubble parameter H_loc = (78+/-2) km/(s*Mpc), the mean-square peculiar velocity sigma_v = 25 km/s, corrected for errors of radial velocity measurements (~4 km/s) and distance measurements (~10 km/s), as well as the radius of the zero-velocity surface R_0 = (0.96+/-0.03) Mpc. The minimum value for sigma_v is achieved when the barycenter of the LG is located at the distance D_c = (0.55+/-0.05) D_M31 towards M31 corresponding to the Milky Way-to-M31 mass ratio M_MW / M_M31 ~ 4/5. In the reference frame of the 30 galaxies at 0.7 - 3.0 Mpc, the LG barycenter has a small peculiar velocity ~(24+/-4) km/s towards the Sculptor constellation. The derived value of R_0 corresponds to the total mass M_T(LG) = (1.9+/-0.2) 10^12 M_sun with Omega_m = 0.24 and a topologically flat universe, a value in good agreement with the sum of virial mass estimates for the Milky Way and M31.
Local groupGalaxyHubble flowAndromeda galaxyBarycenterPeculiar velocityConstellationsMass ratioRadial velocityVirial mass...
• #### Dark matter distributions around massive black holes: A general relativistic analysis

The cold dark matter at the center of a galaxy will be redistributed by the presence of a massive black hole. The redistribution may be determined using an approach pioneered by Gondolo and Silk: begin with a model distribution function for the dark matter, and `grow'' the black hole adiabatically, holding the adiabatic invariants of the motion constant. Unlike the approach of Gondolo and Silk, which adopted Newtonian theory together with ad hoc correction factors to mimic general relativistic effects, we carry out the calculation fully relativistically, using the exact Schwarzschild geometry of the black hole. We find that the density of dark matter generically vanishes at r=2R_S, not 4R_S as found by Gondolo and Silk, where R_S is the Schwarzschild radius, and that the spike very close to the black hole reaches significantly higher densities. We apply the relativistic adiabatic growth framework to obtain the final dark matter density for both cored and cusped initial distributions. Besides the implications of these results for indirect detection estimates, we show that the gravitational effects of such a dark matter spike are significantly smaller than the relativistic effects of the black hole, including frame dragging and quadrupolar effects, for stars orbiting close to the black hole that might be candidates for testing the black hole no-hair theorems.
Black holeDark matterStarDark matter particlePeriapsisAdiabatic invariantNo-hair theoremGalactic CenterPhase spaceCritical value...
• #### Helicity-Flux-Driven Alpha Effect in Laboratory and Astrophysical Plasmas

The constraint imposed by magnetic helicity conservation on the alpha effect is considered for both magnetically and flow dominated self-organizing plasmas. Direct numerical simulations are presented for a dominant contribution to the alpha effect, which can be cast in the functional form of a total divergence of an averaged helicity flux, called the helicity-flux-driven alpha ( H$\alpha$) effect. Direct numerical simulations of the H$\alpha$ effect are prese nted for two examples---the magnetically dominated toroidal plasma unstable to tearing modes, and the flow-dominated accretion disk.
Alpha-effectMagnetorotational instabilityDirect numerical simulationMagnetic helicitySimulationsAccretion diskSelf-organizationMagnetohydrodynamicsInstabilityAzimuth...
• #### Distribution of Faraday Rotation Measure in Jets from Active Galactic Nuclei II. Prediction from our Sweeping Magnetic Twist Model for the Wiggled Parts of AGN Jets and Tails

Distributions of Faraday rotation measure (FRM) and the projected magnetic field derived by a 3-dimensional simulation of MHD jets are investigated based on our "sweeping magnetic twist model". FRM and Stokes parameters were calculated to be compared with radio observations of large scale wiggled AGN jets on kpc scales. We propose that the FRM distribution can be used to discuss the 3-dimensional structure of magnetic field around jets and the validity of existing theoretical models, together with the projected magnetic field derived from Stokes parameters. In the previous paper, we investigated the basic straight part of AGN jets by using the result of a 2-dimensional axisymmetric simulation. The derived FRM distribution has a general tendency to have a gradient across the jet axis, which is due to the toroidal component of the magnetic field generated by the rotation of the accretion disk. In this paper, we consider the wiggled structure of the AGN jets by using the result of a 3-dimensional simulation. Our numerical results show that the distributions of FRM and the projected magnetic field have a clear correlation with the large scale structure of the jet itself, namely, 3-dimensional helix. Distributions, seeing the jet from a certain direction, show a good matching with those in a part of 3C449 jet. This suggests that the jet has a helical structure and that the magnetic field (especially the toroidal component) plays an important role in the dynamics of the wiggle formation because it is due to a current-driven helical kink instability in our model.
Astrophysical jetRotation measure of the plasmaSimulationsActive Galactic NucleiMagnetohydrodynamicsIntensityHelicityLine of sightKink instabilityAccretion disk...
• #### Inflationary Cosmology after Planck 2013

I give a general review of inflationary cosmology and of its present status, in view of the 2013 data release by the Planck satellite. A specific emphasis is given to the new broad class of theories, the cosmological attractors, which have nearly model-independent predictions converging at the sweet spot of the Planck data in the (n_s,r) plane. I also discuss the problem of initial conditions for the theories favored by the Planck data.
Planck missionChaotic Inflation theoryScalar fieldHomogenizationModel of inflationCosmologyInflatonSupergravitySlow-roll inflationAttractor...
• #### Black Hole-Neutron Star Mergers with a Hot Nuclear Equation of State: Outflow and Neutrino-Cooled Disk for a Low-Mass, High-Spin Casever. 2

Neutrino emission significantly affects the evolution of the accretion tori formed in black hole-neutron star mergers. It removes energy from the disk, alters its composition, and provides a potential power source for a gamma-ray burst. To study these effects, simulations in general relativity with a hot microphysical equation of state and neutrino feedback are needed. We present the first such simulation, using a neutrino leakage scheme for cooling to capture the most essential effects and considering a moderate mass (1.4 M_{\odot} neutron star, 5.6 M_{\odot} black hole), high spin (black hole J/M^2=0.9) system with the K_0=220 MeV Lattimer-Swesty equation of state. We find that about 0.08 M_{\odot} of nuclear matter is ejected from the system, while another 0.3 M_{\odot} forms a hot, compact accretion disk. The primary effects of the escaping neutrinos are (i) to make the disk much denser and more compact, (ii) to cause the average electron fraction Y_e of the disk to rise to about 0.2 and then gradually decrease again, and (iii) to gradually cool the disk. The disk is initially hot (T~6 MeV) and luminous in neutrinos (L_{\nu}~10^{54} erg s^{-1}), but the neutrino luminosity decreases by an order of magnitude over 50 ms of post-merger evolution.
NeutrinoBlack holeAccretionStarLuminosityEntropyEjectaAccretion diskTidal tailBlack hole spin...
• #### Non-relativistic Nambu-Goldstone modes associated with spontaneously broken space-time and internal symmetries

We show that a momentum operator of a translational symmetry may not commute with an internal symmetry operator in the presence of a topological soliton in non-relativistic theories. As a striking consequence, there appears a coupled Nambu-Goldstone mode with a quadratic dispersion consisting of translational and internal zero modes in the vicinity of a domain wall in an O(3) sigma model, a magnetic domain wall in ferromagnets with an easy axis.
Domain wallFerromagnetismPhononZero modeSigma modelSolitonSupersymmetry algebraMagnetic domain wallSuperfluid vortexEuler-Lagrange equation...
• #### Scale versus Conformal Invariance Revisited

For a scale invariant theory with gauge-invariant local virial current we argue that the existence of a well defined ground state implies the vanishing of all conformal dilaton scattering amplitudes.
Scale invarianceConformal invarianceDilatonGauge invarianceUnitarityScattering amplitudeS-matrixAmplitudeGauge fieldUnitary representation...
• #### Sterile neutrinos in leptonic and semileptonic decaysver. 2

We address the impact of a modified $W \ell \nu$ coupling on a wide range of observables, such as $\tau$ leptonic and mesonic decays, leptonic decays of pseudoscalar mesons, as well as semileptonic meson decays. In particular, we concentrate on deviations from lepton flavour universality, focusing on the ratios $R_{P} = \Gamma (P \to \ell \nu) / \Gamma (P \to \ell' \nu)$, with $P=K, \pi, D, D_s$, $R(D)={\Gamma (B^+ \to D \tau^+ \nu)}/{\Gamma (B^+ \to D\ell^+ \nu)}$, $R \tau={\Gamma (\tau\to \mu\nu\nu)}/{\Gamma (\tau\to e\nu\nu)}$, $R^{\ell \tau}_P=\Gamma(\tau\to P\nu)/\Gamma(P\to \ell \nu)$, and $\text{BR}(B \to \tau \nu)$. We further consider leptonic gauge boson decays, such as $W\to \ell \nu$ and $Z \to \nu \nu$. For all the above observables, we provide the corresponding complete analytical expressions, derived for the case of massive neutrinos. Working in the framework of the Standard Model extended by additional sterile fermions, which mix with the active (left-handed) neutrinos, we numerically study the impact of active-sterile mixings on the above mentioned observables.
Standard ModelSterile neutrinoNeutrinoUnitarityActive-sterile neutrino mixingMeson decaysKinematicsLepton flavour universalityHadronizationCosmology...
• #### Non-strictly black body spectrum from the tunnelling mechanism

A modern and largely used approach to obtain Hawking radiation is the tunnelling mechanism. However, in various papers in the literature, the analysis concerned almost only to obtain the Hawking temperature through a comparison of the probability of emission of an outgoing particle with the Boltzmann factor. In a interesting and well written paper, Banerjee and Majhi improved the approach, by explicitly finding a black body spectrum associated with black holes. On the other hand, this result, which has been obtained by using a reformulation of the tunnelling mechanism, is in contrast which the remarkable result by Parikh and Wilczek, that, indeed, found a probability of emission which is compatible with a non-strictly thermal spectrum. By using our recent introduction of an effective state for a black hole, here we solve such a contradiction, through a slight modification of the analysis by Banerjee and Majhi. The final result will be a non-strictly black body spectrum from the tunnelling mechanism. We also show that, for an effective temperature, we can write the corresponding effective metric by Hawking's periodicity arguments. Potential important implications for the black hole information puzzle are also discussed
Black holeHawking temperatureEffective temperatureHawking radiationBlack hole evaporationHorizonUnitarityQuantum gravityQuantum mechanicsVirtual particle...
• #### Acronym recognition and processing in 22 languages

We are presenting work on recognising acronyms of the form Long-Form (Short-Form) such as "International Monetary Fund (IMF)" in millions of news articles in twenty-two languages, as part of our more general effort to recognise entities and their variants in news text and to use them for the automatic analysis of the news, including the linking of related news across languages. We show how the acronym recognition patterns, initially developed for medical terms, needed to be adapted to the more general news domain and we present evaluation results. We describe our effort to automatically merge the numerous long-form variants referring to the same short-form, while keeping non-related long-forms separate. Finally, we provide extensive statistics on the frequency and the distribution of short-form/long-form pairs across languages.
StatisticsLanguageFrequency
• #### Mining the Web for Lexical Knowledge to Improve Keyphrase Extraction: Learning from Labeled and Unlabeled Data

Keyphrases are useful for a variety of purposes, including summarizing, indexing, labeling, categorizing, clustering, highlighting, browsing, and searching. The task of automatic keyphrase extraction is to select keyphrases from within the text of a given document. Automatic keyphrase extraction makes it feasible to generate keyphrases for the huge number of documents that do not have manually assigned keyphrases. Good performance on this task has been obtained by approaching it as a supervised learning problem. An input document is treated as a set of candidate phrases that must be classified as either keyphrases or non-keyphrases. To classify a candidate phrase as a keyphrase, the most important features (attributes) appear to be the frequency and location of the candidate phrase in the document. Recent work has demonstrated that it is also useful to know the frequency of the candidate phrase as a manually assigned keyphrase for other documents in the same domain as the given document (e.g., the domain of computer science). Unfortunately, this keyphrase-frequency feature is domain-specific (the learning process must be repeated for each new domain) and training-intensive (good performance requires a relatively large number of training documents in the given domain, with manually assigned keyphrases). The aim of the work described here is to remove these limitations. In this paper, I introduce new features that are derived by mining lexical knowledge from a very large collection of unlabeled data, consisting of approximately 350 million Web pages without manually assigned keyphrases. I present experiments that show that the new features result in improved keyphrase extraction, although they are neither domain-specific nor training-intensive.
Supervised learningFrequencyComputer science (under construction)
• #### Multiplicative functions in arithmetic progressions

We develop a theory of multiplicative functions (with values inside or on the unit circle) in arithmetic progressions analogous to the well-known theory of primes in arithmetic progressions.
Arithmetic progressionUnits
• #### Pedagogic notes on Thomas-Fermi theory (and on some improvements) : atoms, stars, and the stability of bulk matter

StarThomas-Fermi modelAtom
• #### Anomalies without an action

Modern on-shell methods allow us to construct both the classical and quantum S-matrix for a large class of theories, without utilizing knowledge of the interacting Lagrangian. It was recently shown that the same applies for chiral gauge theories, where the constraints from anomaly cancelation can be recast into the tension between unitarity and locality, without any reference to gauge symmetry. In this paper, we give a more detailed exploration, for chiral QED and QCD. We study the rational terms that are mandated by locality, and show that the factorization poles of such terms reveal a new particle in the spectrum, the Green-Schwarz two-from. We further extend the analysis to six-dimensional gravity coupled to chiral matter, including self-dual two-forms for which covariant actions generically do not exist. Despite this, the on-shell methods define the correct quantum S-matrix by demonstrating that locality of the one-loop amplitude requires combination of chiral matter that is consistent with that of anomaly cancelation.
AmplitudeC++UnitarityChiralityTwo-formGauge invarianceChiral fermionAnomaly cancellationGreen-Schwarz mechanismS-matrix...
• #### Adler-Bardeen theorem and manifest anomaly cancellation to all orders in gauge theories

We reconsider the Adler-Bardeen theorem for the cancellation of gauge anomalies to all orders, when they vanish at one loop. Using the Batalin-Vilkovisky formalism and combining the dimensional-regularization technique with the higher-derivative gauge-invariant regularization, we prove the theorem in the most general perturbatively unitary renormalizable gauge theories coupled to matter in four dimensions, and identify the subtraction scheme where anomaly cancellation to all orders is manifest, namely no subtractions of finite local counterterms are required from two loops onwards. Our approach is based on an order-by-order analysis of renormalization, and, differently from most derivations existing in the literature, does not make use of arguments based on the properties of the renormalization group. As a consequence, the proof we give also applies to conformal field theories and finite theories.
RegularizationQuantum anomalyRenormalizationGauge anomalyDimensional regularizationPower countingGauge fixingGauge fieldGauge invarianceRenormalization group...