We consider the dynamics of a particle of mass $M$ and spin $J$ in ${\mathrm{AdS}}_3$. The study reveals the presence of different dynamical sectors depending on the relative values of $M$, $J$ and the ${\mathrm{AdS}}_3$ radius $R$. For the subcritical $M^2{R}^2-J^2>0$ and supercritical $M^2{R}^2-J^2<0$ cases, it is seen that the equations of motion give the geodesics of ${\mathrm{AdS}}_3$. For the critical case $M^2{R}^2=J^2$ there exist extra gauge transformations which further reduce the physical degrees of freedom, and the motion corresponds to the geodesics of ${\mathrm{AdS}}_2$. This result should be useful in the holographic interpretation of the entanglement entropy for two-dimensional conformal field theories with gravitational anomalies.

We compute the correction to the muon magnetic moment in theories where the Higgs is a pseudo-Goldstone boson and leptons are partially composite. Using a general effective Lagrangian we show that in some regions of parameters a sizable new physics contribution to the magnetic moment can be obtained from composite fermions that could explain the $3.5\sigma$ experimental discrepancy from the standard model prediction. This effect depends on the derivative interactions of the Higgs that do not modify the coupling of the Higgs to leptons and it does not require extremely light fermions, allowing us to easily avoid LHC bounds. Our derivations can be in general applied to dipole operators in theories with Goldstone boson Higgs.

Shortly after its birth in a gravitational collapse, a protoneutron star enters in a phase of quasistationary evolution characterized by large gradients of the thermodynamical variables and intense neutrino emission. In a few tens of seconds, the gradients smooth out while the star contracts and cools down, until it becomes a neutron star. In this paper we study this phase of the protoneutron star life including rotation, and employing finite-temperature equations of state. We model the evolution of the rotation rate, and determine the relevant quantities characterizing the star. Our results show that an isolated neutron star cannot reach, at the end of the evolution, the maximum values of mass and rotation rate allowed by the zero-temperature equation of state. Moreover, a mature neutron star evolved in isolation cannot rotate too rapidly, even if it is born from a protoneutron star rotating at the mass-shedding limit. We also show that the I-Love-Q relations are violated in the first second of life, but they are satisfied as soon as the entropy gradients smooth out.

Classicalons are self-bound classical field configurations, which include black holes in general relativity. In quantum theory, they are described by condensates of many soft quanta. In this work, their decay properties are studied in arbitrary dimensions. It is found that generically the decays of other classicalons are enhanced compared to pure graviton condensates, i.e. black holes. The evaporation of higher dimensional graviton condensates turns out to match Hawking radiation solely due to nonlinearites captured by the classicalon picture. Although less stable than black holes, all self-bound condensates are shown to be stable in the limit of large mass. Like for black holes, the effective coupling always scales as the inverse of the number of constituents, indicating that these systems are at critical points of quantum phase transitions. Consequences for cosmology, astro-and collider physics are briefly discussed.

Lorentz invariant derivative interactions for a single spin-2 field are investigated, up to the cubic order. We start from the most general Lorentz invariant terms involving two spacetime derivatives, which are polynomials in the spin-2 field as well as its first derivatives. Using a perturbative Arnowitt-Deser-Misner analysis, we determined the parameters such that the corresponding Hamiltonian possesses a Lagrange multiplier, which would signify there are at most 5 degrees of freedom that are propagating. The resulting derivative terms are linear combinations of terms coming from the expansion of the Einstein-Hilbert Lagrangian around a Minkowski background, as well as the cubic “pseudolinear derivative term” identified in Hinterbichler [J. High Energy Phys. 10 (2013) 102]. We also derived the compatible potential terms, which are linear combinations of the expansions of the first two de Rham–Gabadadze–Tolley mass terms in unitary gauge.

It is known that a non-Abelian magnetic monopole cannot rotate globally (although it may possess a nonzero angular momentum density). At the same time, the total angular momentum of a magnetic dipole equals the electric charge. In this work we question the generality of these results by considering a number of generalizations of the Georgi-Glashow model. We study two different types of finite energy, regular configurations: solutions with net magnetic charge and monopole-antimonopole pairs with zero net magnetic charge. These configurations are endowed with an electric charge and carry also a nonvanishing angular momentum density. However, we argue that the qualitative results found in the Georgi-Glashow model are generic and thus a magnetic monopole cannot spin as long as the matter fields feature the usual “monopole” asymptotic behavior independently of the dynamics of the model. A study of the properties of the dyons and magnetic dipoles in some generalizations of the Georgi-Glashow model supplemented with higher order Skyrme-like terms in the gauge curvature and Higgs fields is given quantitatively.

In this paper charged black rings and black saturns are constructed in Einstein-Maxwell-dilaton theory in five dimensions. The neutral black ring and black saturn solutions are embedded in six dimensions and boosted with respect to the time coordinate and the added sixth dimension. Then the charged solutions are obtained by a Kaluza-Klein reduction. The influence of the charge is studied by analyzing the physical properties and the phase diagram. The different dilatonic solutions are compared and their thermodynamic stability is considered.

The Lemaître–Tolman model with $\mathrm{\Lambda }=0$ and constant bang time that imitates the luminosity distance–redshift relation of the $\mathrm{\Lambda }\mathrm{CDM}$ model using the energy function $E$ alone contains shell crossings. In this paper, the location in spacetime and the consequences of existence of the shell-crossing set (SCS) are investigated. The SCS would come into view of the central observer only at $t\approx 1064T$ to the future from now, where $T$ is the present age of the Universe, but would not leave any recognizable trace in her observations. Light rays emitted near to the SCS are blueshifted at the initial points, but the blueshift is finite, and is overcompensated by later-induced redshifts if the observer is sufficiently far. The local blueshifts cause that $z$ along a light ray is not a monotonic function of the comoving radial coordinate $r$. As a consequence, the angular diameter distance $D_A$ and the luminosity distance $D_L$ from the central observer fail to be functions of $z$; the relations $D_A(z)$ and $D_L(z)$ are multiple-valued in a vicinity of the SCS. The following quantities are calculated and displayed: (1) The distribution of mass density on a few characteristic hypersurfaces of constant time; some of them intersect the SCS. (2) The distribution of density along the past light cone of the present central observer. (3) A few light cones intersecting the SCS at characteristic instants. (4) The redshift profiles along several light cones. (5) The extremum-redshift hypersurface. (6) The $D_A(z)$ and $D_L(z)$ relations. (7) The last scattering time and its comparison with the $\mathrm{\Lambda }\mathrm{CDM}$ last scattering epoch.

Transformation of cosmic microwave background photons into light pseudoscalar particles at the post-big-bang-nucleosynthesis epoch is considered. Using the present day value of a large scale magnetic field to estimate it at earlier cosmological epochs, the oscillation probability of photons into light pseudoscalar particles with an account of coherence breaking in cosmological plasma is calculated. Demanding that the photon transformation does not lead to an exceedingly large cosmic microwave background spectral distortion and temperature anisotropy, the constraints on the coupling constant of axionlike particles to photons, $g_{\varphi \gamma }B\lesssim (10^{-15}–10^{-12})\mathrm{nG}\times {\mathrm{GeV}}^{-1}$, are found for the axionlike particle mass in the interval $10^{-25}\mathrm{eV}\lesssim m_{\varphi }\lesssim 10^{-5}\mathrm{eV}$, where $B$ is the strength of the large scale magnetic field at the present time. Our results update the previously obtained ones since we use the density matrix formalism which is more accurate than the wave function approximation for the description of oscillations with an essential coherence breaking. In the axionlike particle mass range $10^{-25}\mathrm{eV}\lesssim m_{\varphi }\lesssim 10^{-14}\mathrm{eV}$, weaker limits, by at least 2 orders of magnitude $g_{\varphi \gamma }B\lesssim 10^{-11}\mathrm{nG}\times {\mathrm{GeV}}^{-1}$, are obtained in comparison with the wave function approximation. In the mass range $10^{-14}\mathrm{eV}\lesssim m_{\varphi }\lesssim 10^{-5}\mathrm{eV}$, on the other hand, limits that are stronger, by more than an order of magnitude, are obtained. Our results are derived by using upper limits on spectral distortion parameter $\mu$ and temperature anisotropy $\mathrm{\Delta }T/T$ found by COBE and expected sensitivities found by PIXIE/PRISM.

The prospects for direct measurements of inflationary gravitational waves by next generation interferometric detectors inferred from the possible detection of $B$-mode polarization of the cosmic microwave background are studied. We compute the spectra of the gravitational wave background and the signal-to-noise ratios by two interferometric detectors (DECIGO and BBO) for large-field inflationary models in which the tensor-to-scalar ratio is greater than the order of 0.01. If the reheating temperature $T_{\mathrm{RH}}$ of chaotic inflation with the quadratic potential is high ($T_{\mathrm{RH}}>7.9\times 10^6\mathrm{GeV}$ for upgraded DECIGO and $T_{\mathrm{RH}}>1.8\times 10^6\mathrm{GeV}$ for BBO), it will be possible to reach the sensitivity of the gravitational background in future experiments at $3\sigma$ confidence level. The direct detection is also possible for natural inflation with the potential $V(\varphi )={\mathrm{\Lambda }}^4[1-\cos (\varphi /f)]$, provided that $f>4.2M_{\text{pl}}$ (upgraded DECIGO) and $f>3.6M_{\text{pl}}$ (BBO) with $T_{\mathrm{RH}}$ higher than $10^8\mathrm{GeV}$. The quartic potential $V(\varphi )=\lambda {\varphi }^4/4$ with a nonminimal coupling $\xi$ between the inflaton field $\varphi$ and the Ricci scalar $R$ gives rise to a detectable level of gravitational waves for $|\xi |$ smaller than the order of 0.01, irrespective of the reheating temperature.

Thermal relic dark matter particles with a mass of 31–40 GeV that dominantly annihilate to bottom quarks have been shown to provide an excellent description of the excess gamma rays observed from the center of the Milky Way. Flavored dark matter provides a well-motivated framework in which the dark matter can dominantly couple to bottom quarks in a flavor-safe manner. We propose a phenomenologically viable model of bottom flavored dark matter that can account for the spectral shape and normalization of the gamma-ray excess while naturally suppressing the elastic scattering cross sections probed by direct detection experiments. This model will be definitively tested with increased exposure at LUX and with data from the upcoming high-energy run of the Large Hadron Collider (LHC).

While dust contamination now appears as a likely explanation of the apparent tension between the recent BICEP2 data and the Planck data, we will here explore the consequences of a large running in the spectral index as suggested by the BICEP2 Collaboration as an alternative explanation of the apparent tension, but which would be in conflict with prediction of the simplest model of chaotic inflation. The large field chaotic model is sensitive to UV physics, and the nontrivial running of the spectral index suggested by the BICEP2 Collaboration could therefore, if true, be telling us some additional new information about the UV completion of inflation. However, before we would be able to draw such strong conclusions with confidence, we would first have to also carefully exclude all the alternatives. Assuming monomial chaotic inflation is the right theory of inflation, we therefore explore the possibility that the running could be due to some other less UV sensitive degree of freedom. As an example, we ask if it is possible that the curvature perturbation spectrum has a contribution from a curvaton, which makes up for the large running in the spectrum. We find that this effect could mask the information we can extract about the UV physics. We also study different models, which might lead to a large negative intrinsic running of the curvaton.

The contribution of positronium to the electron $g\text{−}2$ ($a_e$) has been computed in G. Mishima, arXiv:1311.7109, and found to be of the same order of $\alpha$ as that of five-loop perturbative QED. We confirm this result and correct a few errors in its first derivation. As recently calculated in K. Melnikov, A. Vainshtein, and M. Voloshin, arXiv:1402.5690, a continuum nonperturbative contribution to $a_e$ cancels one-half of the positronium one. We show by explicit calculation that the remaining half is already included in the five-loop perturbative result. We also show that it arises from the class I(i) of five-loop diagrams containing only one closed electron loop.

The distinguishing feature of the Dine–Fischler–Srednicki–Zhitnitsky (DFSZ) axion is that it couples to the electroweak Higgs fields. There is thus an immediate connection between the Peccei–Quinn (PQ) scale and the weak scale. We wish to incorporate the DFSZ axion in a complete supersymmetric model, valid at all scales, and then to implement it in a numerical code connecting the high scale and the low scale physics on a quantitative level. We find that the simplest supersymmetric DFSZ model, as proposed by Rajagopal et al. in 1990, is inconsistent when we consider the minimization of the scalar potential. The problem is that we obtain a negative squared mass for the saxion, the scalar partner of the axion, at the minimum. We then consider the minimal extension in order to get a consistent model for all scales: one has to include an additional explicit sector to spontaneously break the PQ symmetry. In the complete model we can determine the mass of the axino, the fermionic partner of the axion. It is useful to distinguish two cases: 1) the supersymmetry (SUSY)-breaking scale is lower than the PQ-breaking scale, and 2) the scales are comparable. We find that the axino is very light in case 1, while its mass is generically of the order of the other soft SUSY-breaking masses in case 2. We have implemented SUSY breaking via generic soft-breaking terms, and thus make no explicit statement about the form and mediation of SUSY breaking. This complete model can then be incorporated in a numerical code connecting the two scales. We briefly discuss the renormalization group equations and the couplings of the axion to gluons and photons.

We obtained retarded Green’s functions for massless scalar fields in the background of near-extreme, near-horizon rotating charged black hole of five-dimensional minimal gauged supergravity in Phys. Rev. D 84, 044018 (2011). For general nonextreme black holes, we also derived the radial part of the massless Klein-Gordon equation with zero azimuthal-angle eigenvalues, and showed that it is a general Heun’s equation with a regular singularity at each horizon $u_k$ ($k=1,2,3$) and at infinity. We derived explicitly that the residuum of a pole at each $u_k$ is associated with the surface gravity there. In this addendum, probing regular singularities at each $u_k$ we complete the derivation of the full radial equation with nonzero azimuthal-angle eigenvalues. The residua now include modifications by the angular velocities at respective horizons. This result completes the analysis of the wave equation for the massless Klein-Gordon equation for the general rotating charged black hole of five-dimensional minimal gauged supergravity.

We consider a scalar field with a kinetic term nonminimally coupled to gravity in an anisotropic background. Various potentials for the scalar field are considered. By explicit examples, we show how the anisotropy can change the dynamics of the scalar field compared with the isotropic background.

We present the description of the exponentiated diagrams in terms of generating function within the universal diagrammatic technique. In particular, we show the exponentiation of the gauge theory amplitudes involving products of an arbitrary number of Wilson lines of arbitrary shapes, which generalizes the concept of web diagrams. The presented method gives a new viewpoint on the web diagrams and proves the non-Abelian exponentiation theorem.

The emergent gauge theories are reconsidered in light of supersymmetry and an appropriate emergence conjecture is formulated. Accordingly, it might be expected that only global symmetries are fundamental symmetries of nature, whereas local symmetries and associated massless gauge fields could solely emerge due to spontaneous breaking of the underlying spacetime symmetries involved, such as relativistic invariance and supersymmetry. We further argue that this breaking, taken in the form of the nonlinear $\sigma$-model-type pattern for vector fields or superfields, puts essential restrictions on geometrical degrees of freedom of a physical field system that makes it adjust itself in such a way that its global internal symmetry $G$ turns into the local symmetry $G_{\text{loc}}$. Otherwise, a given field system could lose too many degrees of freedom, thus getting unphysical, which would make it impossible to set the required initial conditions in an appropriate Cauchy problem, or to choose self-consistent equal-time commutation relations in quantum theory. Remarkably, this emergence process may naturally be triggered by supersymmetry, as is illustrated in detail by an example of a general supersymmetric QED model which is then extended to the Standard Model and GUTs. The requirement of vacuum stability in such a class of models makes both Lorentz invariance and supersymmetry become spontaneously broken in the visible sector. As a consequence, the massless photon and other gauge bosons appear as the corresponding Goldstone and pseudo-Goldstone zero modes and special local invariance is simultaneously generated. Due to this invariance, all possible Lorentz violations turn out to be completely canceled out among themselves. However, broken supersymmetry effects related to the existence of a light pseudo-Goldstino (being essentially a photino) are still left in the theory. It typically appears in the low-energy particle spectrum as the eV-scale stable lightest supersymmetric particle or the electroweak-scale long-lived next-to-lightest supersymmetric particle, and in both cases it is accompanied by a very light gravitino that could be considered as some observational signature in favor of emergent supersymmetric theories.

We study a deformation of $\mathcal{N}=2$ supersymmetric QCD with a $U(N)$ gauge group and $N_f$ number of quark flavors induced by the mass term $\mu$ for the adjoint matter which breaks supersymmetry down to $\mathcal{N}=1$ QCD. Recently this deformation was shown to lead to a weakly coupled dual theory only in two particular sets of vacua: the $r=N$ vacuum and the so-called zero vacua which can be found at $r<N_f-N$, where $r$ is the number of condensed quarks. For small quark masses and intermediate values of $\mu$, the gauge group of the dual theory is $U(N_f-N)\times U(1{)}^{2N-N_f}$, where the Abelian sector is heavy and can be integrated out. However, at larger values of $\mu$, the Abelian sector enters the strong coupling regime. We show that the ’t Hooft matching conditions in the chiral limit require the Seiberg neutral meson field $M$ from this sector to become light. In the $r=N$ vacuum, $M$ is constructed of a monopole and an antimonopole connected by confining magnetic strings, while in the zero vacua, it is built of a quark and antiquark connected by confining electric strings.

Motivated by an improved multiwavelength observational coverage of the transient sky, we investigate the importance of relativistic effects in disruptions of stars by nonspinning black holes (BHs). This paper focuses on calculating the ballistic rate of return of debris to the BH as this rate is commonly assumed to be proportional to the light curve of the event. We simulate the disruption of a low mass main sequence star by BHs of varying masses ($10^5,10^6,10^7{M}_{\odot }$) and of a white dwarf by a $10^5{M}_{\odot }$ BH. Based on the orbital energy as well as angular momentum of the debris, we infer the orbital distribution and estimate the return rate of the debris following the disruption. We find two signatures of relativistic disruptions: a gradual rise as well as a delayed peak in the return rate curves relative to their Newtonian analogs. Assuming that the return rates are proportional to the light curves, we find that relativistic effects are in principle measurable given the cadence and sensitivity of the current transient sky surveys. Accordingly, using a simple model of a relativistic encounter with a Newtonian parametric fit of the peak leads to an overestimate in the BH mass by a factor of $\sim \text{few}\times 0.1$ and $\sim \text{few}$ in the case of the main sequence star and white dwarf tidal disruptions, respectively.