All purely bosonic supersymmetric solutions of minimal gauged supergravity in five dimensions are classified. The solutions fall into two classes depending on whether the Killing vector constructed from the Killing spinor is timelike or null. When it is timelike, the solutions are determined by a four-dimensional Kähler base manifold, up to an antiholomorphic function, are necessarily not static, and generically preserve 1/2 of the supersymmetry. When it is null we provide a precise prescription for constructing the solutions and we show that they generically preserve 1/4 of the supersymmetry. We show that five-dimensional anti-de Sitter space $\left({\mathrm{AdS}}_5\right)$ is the unique maximally supersymmetric configuration. The formalism is used to construct some new solutions, including a nonsingular deformation of ${\mathrm{AdS}}_5,$ which can be uplifted to obtain new solutions of type IIB supergravity.

We study monopole and dyon solutions to the equations of motion of the bosonic sector of $\mathcal{N}=4\mathrm{}$ gauged supergravity in four dimensional space-time. A static, spherically symmetric ansatz for the metric, gauge fields, dilaton, and axion leads to soliton solutions which, in the electrically charged case, have compact spatial sections. Both analytical and numerical results for the solutions are presented.

We show that topological 3D gravity with torsion can be formulated as a Chern-Simons gauge theory, provided a specific parameter, known as the effective cosmological constant, is negative. In that case, the boundary dynamics of the theory corresponding to anti–de Sitter boundary conditions is described by a conformal field theory with two different central charges.

In this paper the problem of finding exact solutions of the combined system of the Einstein-Maxwell-Weyl equations for cylindrical waves is reduced to the solution of two complete singular integral equations in the complex plane of the auxiliary analytical parameter. In the case of the nonsingular symmetry axis the problem further simplifies and requires solving the only integral equation, the expressions for the Ernst potentials on the symmetry axis then defining the group transformations of internal symmetries during the solution generation process. A large class of exact solutions for neutrino electrovacuum is obtained, and the Cauchy problem related to some particular initial data is considered.

We present a method for generating exact diagonal cosmological solutions with two spacelike commuting Killing vectors ${(G}_2$ cosmologies) in dilaton gravity coupled to a radiation perfect fluid and with a cosmological potential of a special type. The method is based on the symmetry group of the system of $G_2$ field equations. Several new classes of explicit exact inhomogeneous perfect fluid scalar-tensor cosmologies are presented.

In a toy model we derive the gravitational equation on a self-gravitating curved D-brane. The effective theory on the brane is drastically changed from the ordinal Einstein equation. The net cosmological constant on the brane depends on a tuning between the brane tension and the brane charges. Moreover, the nonzero matter stress tensor exists if the net cosmological constant is not zero. This fact indicates a direct connection between matter on the brane and dark energy.

We construct a model where cosmological perturbations are analytically solved based on dilatonic brane worlds. A bulk scalar field has an exponential potential in the bulk and an exponential coupling to the brane tension. The bulk scalar field yields a power-law inflation on the brane. The exact background metric can be found including the back reaction of the scalar field. Then exact solutions for cosmological perturbations which properly satisfy the junction conditions on the brane are derived. These solutions provide us an interesting model to understand the connection between the behavior of cosmological perturbations on the brane and the geometry of the bulk. Using these solutions, the behavior of an anisotropic stress induced on the inflationary brane by bulk gravitational fields is investigated.

Recent fits of cosmological parameters by a Wilkinson Microwave Anisotropy Probe (WMAP) measurement favor a primordial scalar spectrum with a varying index. This result, if it stands, could severely constrain inflation model building. Most extant slow-roll inflation models allow for only a tiny amount of scale variations in the spectrum. We propose in this paper an extra-dimensional inflation model which is natural theoretically and can generate the required variations of the spectral index as implied by the WMAP for suitable choices of parameters.

We develop a search method for gravitational ringing of black holes. The gravitational ringing is due to complex frequency modes called the quasinormal modes that are excited when a black hole geometry is perturbed. The detection of it will be a direct confirmation of the existence of a black hole. Assuming that the ringdown waves are dominated by the least-damped (fundamental) mode with the least imaginary part, we consider matched filtering and develop an optimal method to search for the ringdown waves that have damped sinusoidal wave forms. When we use the matched filtering method, a data analysis with a lot of templates is required. Here we have to ensure a proper match between the filter as a template and the real wave. It is necessary to keep the detection efficiency as high as possible under limited computational costs. First, we consider the white noise case for which the matched filtering can be studied analytically. We construct an efficient method for tiling the template space. Then, using a fitting curve of the TAMA300 DT7 noise spectrum, we numerically consider the case of colored noise. We find our tiling method developed for the white noise case is still valid even if the noise is colored.

In this paper I present a detailed QCD analysis of twist-3 effects in the Wandzura-Wilczek (WW) approximation in deeply virtual Compton scattering (DVCS) observables for various kinematical settings, representing the DESY HERA, HERMES, CLAS and the planned EIC (electron-ion-collider) experiments. I find that the twist-3 effects in the WW approximation are almost always negligible at collider energies but can be large for low $Q^2$ and smaller $x_{\mathrm{bj}}$ in observables for the lower energy, fixed target experiments directly sensitive to the real part of DVCS amplitudes like the charge asymmetry. Conclusions are then drawn about the reliability of extracting twist-2 generalized parton distributions (GPDs) from experimental data and a first, phenomenological, parametrization of the LO and NLO twist-2 GPD H, describing all the currently available DVCS data within the experimental errors is given.

We perform a model independent analysis of the chargino contributions to the CP asymmetry in the $\overrightarrow{B}\phi K_S$ process. We use the mass insertion approximation method generalized by including the possibility of a light right stop. We find that the dominant effect is given by the contributions of the mass insertions $({\delta }_{\mathrm{LL}}^u{)}_{32}$ and $({\delta }_{\mathrm{RL}}^u{)}_{32}$ to the Wilson coefficient of the chromomagnetic operator. By considering both these contributions simultaneously, the CP asymmetry in the $\overrightarrow{B}\phi K_S$ process is significantly reduced, and negative values, which are within the $1\sigma$ experimental range and satisfy the $\overrightarrow{b}s\gamma$ constraints, can be obtained.

We investigate the negative-parity baryon spectra in quenched lattice QCD. We employ the anisotropic lattice with a standard Wilson gauge and $O\left(a\right)\mathrm{}$ improved Wilson quark actions at three values of lattice spacings with a renormalized anisotropy $\xi {=a}_{\sigma }{/a}_{\tau }=4,$ where $a_{\sigma }$ and $a_{\tau }$ are spatial and temporal lattice spacings, respectively. The negative-parity baryons are measured with the parity projection. In particular, we pay much attention to the lowest SU(3) flavor-singlet negative-parity baryon, which is assigned as the $\Lambda \mathrm{}\left(1405\right)\mathrm{}$ in the quark model. For the flavor octet and decuplet negative-parity baryons, the calculated masses are close to the experimental values of corresponding lowest-lying negative-parity baryons. In contrast, the flavor-singlet baryon is found to be about 1.7 GeV, which is much heavier than the $\Lambda \mathrm{}\left(1405\right).$ Therefore it is difficult to identify the $\Lambda \mathrm{}\left(1405\right)\mathrm{}$ to be the flavor-singlet three-quark state, which seems to support an interesting picture of the pentaquark $\left(udsq\overline{q}\right)$ state or the $N\overline{K}$ molecule for the $\Lambda \mathrm{}\left(1405\right).$

A future galactic SN can be located several hours before the optical explosion through the MeV-neutrino burst, exploiting the directionality of $\nu -e$ scattering in a water Cherenkov detector such as Super-Kamiokande. We study the statistical efficiency of different methods for extracting the SN direction and identify a simple approach that is nearly optimal, yet independent of the exact SN neutrino spectra. We use this method to quantify the increase in the pointing accuracy by the addition of gadolinium to water, which tags neutrons from the inverse beta decay background. We also study the dependence of the pointing accuracy on neutrino mixing scenarios and initial spectra. We find that in the “worst case” scenario the pointing accuracy is $8°$ at 95% C.L. in the absence of tagging, which improves to $3°$ with a tagging efficiency of 95%. At a megaton detector, this accuracy can be as good as $0.6°.$ A TeV-neutrino burst is also expected to be emitted contemporaneously with the SN optical explosion, which may locate the SN to within a few tenths of a degree at a future ${\mathrm{km}}^2$ high-energy neutrino telescope. If the SN is not seen in the electromagnetic spectrum, locating it in the sky through neutrinos is crucial for identifying the Earth matter effects on SN neutrino oscillations.

We report on a search for the flavor-changing neutral current decay $D^0\to {\mu }^{+}{\mu }^{-}$ in $p\overline{p}$ collisions at $\sqrt{s}=1.96\mathrm{}\mathrm{TeV}$ using $65{\mathrm{pb}}^{-1}$ of data collected by the CDF II experiment at the Fermilab Tevatron Collider. A displaced-track trigger selects long-lived $D^0$ candidates in the $D^0\to {\mu }^{+}{\mu }^{-}$ search channel, the kinematically similar $D^0\to {\pi }^{+}{\pi }^{-}$ channel used for normalization, the Cabibbo-favored $D^0\to K^{-}{\pi }^{+}$ channel used to optimize the selection criteria in an unbiased manner, and their charge conjugates. Finding no signal events in the $D^0\to {\mu }^{+}{\mu }^{-}$ search window, we set an upper limit on the branching fraction $\mathcal{B}{(D}^0\to {\mu }^{+}{\mu }^{-})<~2.5\times {10}^{-6}$ $(3.3\mathrm{}\times {10}^{-6})$ at the $90\%$ (95%) confidence level.

A covariant quantization method is developed for the off-shell superparticle in 10 dimensions. On shell it is consistent with light cone quantization, while off shell it gives a noncommutative superspace that realizes nonlinearly a hidden 11-dimensional super Poincaré symmetry. The nonlinear commutation rules are then used to construct the supersymmetric generalization of the covariant Moyal star product in noncommutative superspace. As one of the possible applications, we propose this new product as the star product in supersymmetric string field theory. Furthermore, the formalism introduces new techniques and concepts in noncommutative (super)geometry.

Large-volume, high-temperature Bose-Einstein condensation is illustrated for a relativistic $O\left(2\right)\mathrm{}$-invariant scalar field with a fixed charge using the canonical ensemble. The standard, grand canonical results are reproduced for the infinite-volume limit. Finite-volume corrections are calculated in the canonical ensemble and the results are found to differ from the finite-volume grand canonical approximation in a consistent qualitative way.

Gravitational waves from oscillating neutron stars in axial symmetry are studied performing numerical simulations in full general relativity. Neutron stars are modeled by a polytropic equation of state for simplicity. A gauge-invariant wave extraction method as well as a quadrupole formula are adopted for computation of gravitational waves. It is found that the gauge-invariant variables systematically contain numerical errors generated near the outer boundaries in the present axisymmetric computation. We clarify their origin, and illustrate that it is possible to eliminate the dominant part of the systematic errors. The best corrected waveforms for oscillating and rotating stars currently contain errors of magnitude $\sim {10}^{-3}$ in the local wave zone. Comparing the waveforms obtained by the gauge-invariant technique with those by the quadrupole formula, it is shown that the quadrupole formula yields approximate gravitational waveforms in addition to a systematic underestimation of the amplitude of $O(M/R)\mathrm{}$ where M and R denote the mass and the radius of neutron stars. However, the wave phase and modulation of the amplitude can be computed accurately. This indicates that the quadrupole formula is a useful tool for studying gravitational waves from rotating stellar core collapse to a neutron star in fully general relativistic simulations. The properties of the gravitational waveforms from the oscillating and rigidly rotating neutron stars are also addressed paying attention to the oscillation associated with fundamental modes.

We consider an Unruh-DeWitt type monopole detector theory for the massless scalar field in (3+1)-dimensional space-time. In this model the detector is accelerated via the interaction at a point with the massless scalar field only. The consistency between the uniform acceleration and the vacuum background as well as the potential for the monopole moment is examined at the classical level. Then we calculate the radiation from the accelerated detector. We find that the Unruh effect on the monopole moment reflects the quantum uncertainty of the detector to the radiation in a way consistent with the fact that the radiation vanishes in the static limit.

Black hole perturbation theory, or more generally, perturbation theory on a Schwarzschild background, has been applied in several contexts, but usually under the simplifying assumption that the Arnowitt-Deser-Misner (ADM) momentum vanishes, namely, that the evolution is carried out and observed in the “center of momentum frame.” In this paper we consider some consequences of the inclusion of a nonvanishing ADM momentum in the initial data. We first provide a justification for the validity of the transformation of the initial data to the “center of momentum frame,” and then analyze the effect of this transformation on the gravitational wave amplitude. The most significant result is the possibility of a type of gravitational memory effect that appears to have no simple relation to the well known Christodoulou effect.