We compute the complete set of Higgs-mediated chargino-neutralino two-loop contributions to the electric dipole moments of the electron and neutron in the minimal supersymmetric standard model (MSSM). We study the dependence of these contributions on the parameters that govern $CP$-violation in the MSSM gauge-gaugino-Higgs-Higgsino sector. We find that contributions mediated by the exchange of $W{H}^{\pm }$ and $Z{A}^0$ pairs, where $H^{\pm }$ and $A^0$ are the charged and $CP$-odd Higgs scalars, respectively, are comparable to or dominate over those mediated by the exchange of neutral gauge bosons and $CP$-even Higgs scalars. We also emphasize that the result of this complete set of diagrams is essential for the full quantitative study of a number of phenomenological issues, such as electric dipole moment searches and their implications for electroweak baryogenesis.

We discuss the nature of the phase transition for lattice QCD at finite temperature and density. We propose a method to calculate the canonical partition function by fixing the total quark number introducing approximations allowed in the low density region. An effective potential as a function of the quark number density is discussed from the canonical partition function. We analyze data obtained in a simulation of two-flavor QCD using p4-improved staggered quarks with bare quark mass $m/T=0.4$ on a ${16}^3\times 4$ lattice. The results suggest that the finite density phase transition at low temperature is of first order.

In this work, we present more details of the calculation on the next-to-leading-order (NLO) QCD corrections to polarization of direct $J/\psi$ production via color singlet at the Tevatron and LHC, together with the results for ${\rm Y}$ for the first time. Our results show that the $J/\psi$ polarization status drastically changes from transverse polarization dominant at leading order into longitudinal polarization dominant in the whole range of the transverse momentum $p_t$ of $J/\psi$ when the NLO corrections are counted. For ${\rm Y}$ production, the $p_t$ distribution of the polarization status behaves almost the same as that for $J/\psi$ except that the NLO result is transverse polarization at small $p_t$ range. Although the theoretical evaluation predicts a larger longitudinal polarization than the measured value at the Tevatron, it may provide a solution towards the previous large discrepancy for $J/\psi$ and ${\rm Y}$ polarization between theoretical prediction and experimental measurement, and suggests that the next important step is to calculate the NLO corrections to hadronproduction of color-octet state $J/{\psi }^{(8)}$ and ${{\rm Y}}^{(8)}$. Our calculations are performed in two ways: namely, we do and do not analytically sum over the polarizations, and then check them with each other.

All the leading-twist parton distribution functions are calculated in a spectator model of the nucleon, using scalar and axial-vector diquarks. Single gluon rescattering is used to generate $T$-odd distribution functions. Different choices for the diquark polarization states are considered, as well as a few options for the form factor at the nucleon-quark-diquark vertex. The results are listed in analytic form and interpreted in terms of light-cone wave functions. The model parameters are fixed by reproducing the phenomenological parametrization of unpolarized and helicity parton distributions at the lowest available scale. Predictions for the other parton densities are given and, whenever possible, compared with available phenomenological parametrizations.

We report the first observation of two resonancelike structures in the ${\pi }^{+}{\chi }_{c1}$ invariant mass distribution near $4.1\mathrm{GeV}/c^2$ in exclusive ${\overline{B}}^0\to K^{-}{\pi }^{+}{\chi }_{c1}$ decays. From a Dalitz plot analysis in which the ${\pi }^{+}{\chi }_{c1}$ mass structures are represented by Breit-Wigner resonance amplitudes, we determine masses and widths of: $M_1=(4051\pm {14}_{-41}^{+20})\mathrm{MeV}/c^2$, ${\Gamma }_1=({82}_{-17-22}^{+21+47})\mathrm{MeV}$, $M_2=({4248}_{-29-35}^{+44+180})\mathrm{MeV}/c^2$, and ${\Gamma }_2=({177}_{-39-61}^{+54+316})\mathrm{MeV}$; and product branching fractions of $\mathcal{B}({\overline{B}}^0\to K^{-}{Z}_{1,2}^{+})\times \mathcal{B}(Z_{1,2}^{+}\to {\pi }^{+}{\chi }_{c1})=({3.0}_{-0.8-1.6}^{+1.5+3.7})\times {10}^{-5}$ and $({4.0}_{-0.9-0.5}^{+2.3+19.7})\times {10}^{-5}$, respectively. Here the first uncertainty is statistical, the second is systematic. The significance of each of the ${\pi }^{+}{\chi }_{c1}$ structures exceeds $5\sigma$, including the systematic uncertainty from various fit models. This analysis is based on $657\times {10}^6$ $B\overline{B}$ events collected at the ${\rm Y}(4S)$ resonance with the Belle detector at the KEKB asymmetric-energy $e^{+}{e}^{-}$ collider.

In this addendum to Phys. Rev. D 74, 023502 (2006), we present an update of cosmological constraints on single-field inflation in light of the Wilkinson Microwave Ansiotropy Probe satellite mission five-year results (WMAP5). We find that the cosmic microwave background data are quite consistent with a Harrison-Zel’dovich primordial spectrum with no running and zero tensor amplitude. We find that the three main conclusions of our analysis of the WMAP three-year data (WMAP3) are consistent with the WMAP5 data: (1) the Harrison-Zel’dovich model is within the 95% confidence level contours; (2) there is no evidence for running of the spectral index of scalar perturbations; (3) from the WMAP 5 data alone, potentials of the form $V\propto {\varphi }^p$ are consistent with the data for $p=2$ and are ruled out for $p=4$. Furthermore, consistent with our WMAP3 analysis, we find no evidence for primordial tensor perturbations, this time with a 95% confidence upper limit of $r<0.4$ for the WMAP5 data alone, and $r<0.35$ for the WMAP5 data taken in combination with the Arcminute Cosmology Bolometer Array (ACBAR).

We present a comparison of the noncommutative field theories built using two different star products: Moyal and Wick-Voros (or normally ordered). For the latter we discuss both the classical and the quantum field theory in the quartic potential case and calculate the Green’s functions up to one loop, for the two- and four-point cases. We compare the two theories in the context of the noncommutative geometry determined by a Drinfeld twist, and the comparison is made at the level of Green’s functions and $S$ matrix. We find that while the Green’s functions are different for the two theories, the $S$ matrix is the same in both cases and is different from the commutative case.

We introduce $SO(7{)}_{\mathrm{global}}$ symmetric mass terms into Bagger-Lambert theory in three dimensions. The scalar field $X_a{}^I$ and its fermionic partner ${\psi }_a$ are provided with the mass $m$, while a quartic interaction term is induced. These new terms explicitly break the original $SO(8{)}_{\mathrm{global}}$ symmetry down to $SO(7{)}_{\mathrm{global}}$ in terms of octonion structure constants. The original supersymmetry parameter in the ${\mathbf{8}}_{\mathrm{S}}$ is reduced to a singlet, implying that the original $N=8$ supersymmetry is reduced to $N=1$ supersymmetry. As illustrations, we present some nontrivial vacuum configurations with the breaking $SO(7{)}_{\mathrm{global}}\to SO(4{)}_{\mathrm{global}}$ or smaller symmetry groups. Interestingly, we also find that after a nontrivial vacuum expectation value $⟨X_a{}^I⟩$ is developed, the vector field $A_{\mu }{}^{ab}$ satisfies a “self-duality” condition, and starts propagating with a mass. These results are due to the special nature of the octonion structure constants.

We examine the motion and tidal dynamics of a nonrotating black hole placed within a post-Newtonian external spacetime. The black hole’s gravity is described accurately to all orders in $Gm/c^{2}r$, where $m$ is the black-hole mass and $r$ is the distance to the black hole. The tidal perturbation created by the external environment is treated as a small perturbation. At a large distance from the black hole, the gravitational field of the external distribution of matter is assumed to be sufficiently weak to be adequately described by the (first) post-Newtonian approximation to general relativity. There, the black hole is treated as a monopole contribution to the total gravitational field. There exists an overlap in the domains of validity of each description, and the black-hole and post-Newtonian metrics are matched in the overlap. The matching procedure produces (i) a justification of the statement that a nonrotating black hole is a post-Newtonian monopole; (ii) a complete characterization of the coordinate transformation between the inertial, barycentric frame and the accelerated, black-hole frame; (iii) the equations of motion for the black hole; and (iv) the gravito-electric and gravito-magnetic tidal fields acting on the black hole. We first calculate the equations of motion and tidal fields by making no assumptions regarding the nature of the post-Newtonian environment; this could contain a continuous distribution of matter (so as to model a galactic core) or any number of condensed bodies. We next specialize our discussion to a situation in which the black hole is a member of a post-Newtonian two-body system. As an application of our results, we examine the geometry of the deformed event horizon and calculate the tidal heating of the black hole, the rate at which it acquires mass as a result of its tidal interaction with the companion body.

The brane-world description of our universe entails a large extra dimension and a fundamental scale of gravity that might be lower by several orders of magnitude as compared to the Planck scale. An interesting consequence of the brane-world scenario is in the nature of the vacuum solutions of the brane gravitational field equations, with properties quite distinct as compared to the standard black-hole solutions of general relativity. One possibility of observationally discriminating between different types of black holes is the study of the emission properties of the accretion disks. In the present paper we obtain the energy flux, the emission spectrum and accretion efficiency from the accretion disks around several classes of static and rotating brane-world black holes, and we compare them to the general relativistic case. Particular signatures can appear in the electromagnetic spectrum, thus leading to the possibility of directly testing extra-dimensional physical models by using astrophysical observations of the emission spectra from accretion disks.

In a recent work, it has been pointed out that certain observables of the massless scalar field theory in a static spherically symmetric background exhibit a universal behavior at large distances. More precisely, it was shown that, unlike what happens in the case where the coupling to the curvature $\xi$ is generic, for the special cases $\xi =0$ and $\xi =1/6$ the large distance behavior of the expectation value $⟨T^{\mu }{}_{\nu }⟩$ turns out to be independent of the internal structure of the gravitational source. Here, we address a higher dimensional generalization of this result: We first compute the difference between a black hole and a static spherically symmetric star for the observables $⟨{\varphi }^2⟩$ and $⟨T^{\mu }{}_{\nu }⟩$ in the far field limit. Thus, we show that the conformally invariant massless scalar field theory in a static spherically symmetric background exhibits such a universality phenomenon in $D\ge 4$ dimensions. Also, using the one-loop effective action, we compute $⟨T^{\mu }{}_{\nu }⟩$ for a weakly gravitating object. These results lead to the explicit expression of the expectation value $⟨T^{\mu }{}_{\nu }⟩$ for a Schwarzschild-Tangherlini black hole in the far field limit. As an application, we obtain quantum corrections to the gravitational potential in $D$ dimensions, which for $D=4$ are shown to agree with the one-loop correction to the graviton propagator previously found in the literature.

Analogue models for gravity intend to provide a framework where matter and gravity, as well as their intertwined dynamics, emerge from degrees of freedom that have a priori nothing to do with what we call gravity or matter. Bose-Einstein condensates (BEC) are a natural example of an analogue model since one can identify matter propagating on a (pseudo-Riemannian) metric with collective excitations above the condensate of atoms. However, until now, a description of the “analogue gravitational dynamics” for such model was missing. We show here that in a BEC system with massive quasiparticles, the gravitational dynamics can be encoded in a modified (semiclassical) Poisson equation. In particular, gravity is of extreme short range (characterized by the healing length) and the cosmological constant appears from the noncondensed fraction of atoms in the quasiparticle vacuum. While some of these features make the analogue gravitational dynamics of our BEC system quite different from standard Newtonian gravity, we nonetheless show that it can be used to draw some interesting lessons about “emergent gravity” scenarios.

The advent of explicit Dirac-Born-Infeld inflationary models within string theory has drawn renewed interest to the cosmological role of unusual scalar field dynamics, usually referred to as $k$-inflation. In this situation, the standard method used to determine the behavior of cosmological perturbations breaks down. We present a generic method, based on the uniform approximation, to analytically derive the power spectra of scalar and tensor perturbations. For this purpose, a simple hierarchy of parameters, related to the sound speed of the cosmological fluctuations and its successive derivatives, is introduced in a $k$-inflation analogue of the Hubble flow functions. The scalar spectral index and its running are obtained up to next-to-next-to-leading order for all $k$-inflationary models. This result relies on the existence of a well-motivated initial state, which is not trivial in the present context: having the wavelength of the Fourier mode smaller than the sonic horizon is indeed not enough and some conditions on the dynamics of the sound speed are also required. Our method is then applied to various models encountered in the literature. After deriving a generic slow-roll trajectory valid for any Dirac-Born-Infeld model, simple formulae for the cosmological observables are obtained. In particular, the running, as the spectral index, for the so-called UV and IR brane inflationary models is found to be uniquely determined by the ’t Hooft coupling. Finally, the accuracy of these cosmological predictions is assessed by comparing the analytical approximations with exact numerical integrations.

Oscillating scalar fields, with an oscillation frequency much greater than the expansion rate, have been proposed as models for dark energy. We examine these models, with particular emphasis on the evolution of the ratio of the oscillation frequency to the expansion rate. We show that this ratio always increases with time if the dark energy density declines less rapidly than the background energy density. This allows us to classify oscillating dark energy models in terms of the epoch at which the oscillation frequency exceeds the expansion rate, which is effectively the time at which rapid oscillations begin. There are three basic types of behavior: early oscillation models, in which oscillations begin during the matter-dominated era; late oscillation models, in which oscillations begin after scalar-field domination; and nonoscillating models. We examine a representative set of models (those with power-law potentials) and determine the parameter range giving acceptable agreement with the supernova observations. We show that a subset of all three classes of models can be consistent with the observational data.

A missing energy discovery is possible at the LHC with the first $100{\mathrm{pb}}^{-1}$ of understood data. We present a realistic strategy to rapidly narrow the list of candidate theories at, or close to, the moment of discovery. The strategy is based on robust ratios of inclusive counts of simple physics objects. We study specific cases showing discrimination of look-alike models in simulated data sets that are at least 10 to 100 times smaller than used in previous studies. We discriminate supersymmetry models from nonsupersymmetric look-alikes with only $100{\mathrm{pb}}^{-1}$ of simulated data, using combinations of observables that trace back to differences in spin.

Volume dependence of the spectral weight is usually used as a simple criteria to distinguish single-particle states from multiparticle states in lattice QCD calculations. Within a solvable model, the Lee model, we show that this criteria is in principle only valid for a stable particle or a narrow resonance. If the resonance being studied is broad, then the volume dependence of the corresponding spectral weight resembles that of a multiparticle state instead of a single-particle one. For an unstable $V$ particle in the Lee model, the transition from single-particle to multiparticle volume dependence is governed by the ratio of its physical width to the typical level spacing in the finite volume. We estimate this ratio for practical lattice QCD simulations and find that, for most cases, the resonance studied in lattice QCD simulations still resembles the single-particle behavior.

Electroweak Sudakov logarithms at high energy, of the form $(\alpha /{sin}^2{\theta }_W{)}^n{log}^{m}s/M_{Z,W}^2$, are summed using effective theory (EFT) methods. The exponentiation of Sudakov logarithms and factorization is discussed in the EFT formalism. Radiative corrections are computed to scattering processes in the standard model involving an arbitrary number of external particles. The computations include nonzero particle masses such as the $t$-quark mass, electroweak mixing effects which lead to unequal $W$ and $Z$ masses and a massless photon, and Higgs corrections proportional to the top-quark Yukawa coupling. The structure of the radiative corrections, and which terms are summed by the EFT renormalization group is discussed in detail. The omitted terms are smaller than 1%. We give numerical results for the corrections to dijet production, dilepton production, $t\overline{t}$ production, and squark pair production. The purely electroweak corrections are significant—about 15% at 1 TeV, increasing to 30% at 5 TeV, and they change both the scattering rate and angular distribution. The QCD corrections (which are well-known) are also computed with the EFT. They are much larger—about a factor of 4 at 1 TeV, increasing to a factor of 30 at 5 TeV. Mass effects are also significant; the $q\overline{q}\to t\overline{t}$ rate is enhanced relative to the light-quark production rate by 40%.

We report on a search for $CP$ asymmetry in the singly Cabibbo-suppressed decay $D^{+}\to K^{+}{K}^{-}{\pi }^{+}$ using a data sample of $818{\mathrm{pb}}^{-1}$ accumulated with the CLEO-c detector on the $\psi (3770)$ resonance. A Dalitz-plot analysis is used to determine the amplitudes of the intermediate states. We find no evidence for $CP$ violation either in specific two-body amplitudes or integrated over the entire phase space. The $CP$ asymmetry in the latter case is measured to be $(-0.03\pm 0.84\pm 0.29)\%$.

We consider the impact of a large phase of $B_s\mathrm{\text{−}}{\overline{B}}_s$ mixing in supersymmetric SU(5) and SO(10) models. In the models, the magnitude of this phase is correlated with the branching ratio of $\tau \to \mu \gamma$, and we find that in the SU(5) model, the phase is bound to be small. In the case of SO(10) models, this correlation can be relaxed and a large phase can be obtained. We predict the sparticle mass ranges for the LHC for these models once the recent result which shows evidence of large phase is accommodated and discuss the dark matter and the anomalous magnetic moment constraints on this analysis. We show that the upcoming results of Fermilab will be very useful to decipher these important grand unified theory symmetries.

We describe a method for determining the hierarchy of the neutrino mass spectrum and ${\theta }_{13}$ through remote detection of electron antineutrinos from a nuclear reactor. This method utilizing a single, 10-kiloton scintillating liquid detector at a distance of 49–63 kilometers from the reactor complex measures mass-squared differences involving ${\nu }_3$ with a one(ten)-year exposure provided ${sin}^2(2{\theta }_{13})>0.05(0.02)$. Our technique applies the Fourier transform to the event rate as a function of neutrino flight distance over neutrino energy. Sweeping a relevant range of $\delta m^2$ resolves separate spectral peaks for $\delta m^2{}_{31}$ and $\delta m^2{}_{32}$. For normal (inverted) hierarchy $|\delta m^2{}_{31}|$ is greater (lesser) than $|\delta m^2{}_{32}|$. This robust determination requires a detector energy resolution of $3.5\%/\sqrt{E}$.