We show that the relativistic gravity theory can offer a framework to formulate the nonrelativistic effective field theory in a general coordinate invariant way. We focus on the parity violating case in $2+1$ dimensions which is particularly appropriate for the study on quantum Hall effects and chiral superfluids. We discuss how the nonrelativistic spacetime structure emerges from relativistic gravity. We present covariant maps and constraints that relate the field contents in the two theories, which also serve as the holographic dictionary in the context of gauge/gravity duality. A low energy effective action for fractional quantum Hall states is constructed, which captures universal geometric properties and generates nonuniversal corrections systematically. We give another holographic example with dyonic black brane background to calculate thermodynamic and transport properties of strongly coupled nonrelativistic fluids in magnetic field. In particular, by identifying the shift function in the gravity as a minus of guiding center velocity, we obtain the Hall viscosity with its relation to Landau orbital angular momentum density proportional to Wen-Zee shift. Our formalism has a good projection to lowest Landau level.

We investigate holographically the entanglement entropy of a nonconformal medium whose dual geometry is described by an Einstein-Maxwell-dilaton theory. Because of an additional conserved charge corresponding to the number operator, its thermodynamics can be represented in a grand canonical or canonical ensemble. We study thermodynamics in both ensembles by using the holographic renormalization and the entanglement entropy of a nonconformal medium. After defining the entanglement chemical potential, which unlike the entanglement temperature has a nontrivial size dependence, we find that the entanglement entropy of a small subsystem satisfies the relation resembling the first law of thermodynamics in a medium. Furthermore, we study the entanglement entropy change in the nonconformal medium caused by the excitation of the ground state and by the global quench corresponding to the insertion of particles.

The recent excess in the CMS measurements of $eejj$ and $e\nu jj$ channels and the emergence of PeV cosmic neutrino events at the IceCube experiment share an intriguing implication for a leptoquark with a 600–650 GeV mass. We investigate the CMS constraints on the flavor structure of a scenario with the minimal leptoquark Yukawa couplings and correlate such a scenario to the resonant enhancement in the very high energy shower event rates at the IceCube. We find for a single leptoquark, the CMS signals require large couplings to the third generation leptons. This leads to an enhancement in the ${\nu }_{\tau }$-nucleon scattering cross section and subsequently more ${\nu }_{\tau }$ events at PeV energies. However, a visible enhancement above the Standard Model scattering would require a leptoquark Yukawa coupling larger than one that can be easily tested at the upcoming LHC runs.

We study collective excitations in systems described by chiral kinetic theory in an external magnetic field, such as quark-gluon plasma or Fermi liquids near Dirac/Weyl points of a semimetal. We consider high-temperature weak-coupling plasma, as well as high-density Landau Fermi liquid, without restricting to weak interactions. We show that the chiral magnetic wave (CMW) emerges in the hydrodynamic regime (at frequencies smaller than the collision relaxation rate), and the CMW velocity is determined by thermodynamic properties only. We find that in a plasma of opposite chiralities, at frequencies smaller than the chirality-flipping rate, the CMW excitation turns into a vectorlike diffusion mode. In the interacting Fermi liquid, the CMW turns into the Landau zero sound mode in the high-frequency collisionless regime.

The noncommutative (NC) massive quantum electrodynamics in $2+1$ dimensions is considered. We show explicitly that the one-loop effective action arising from integrating out the fermionic fields leads to the ordinary NC Chern-Simons and NC Maxwell action at the long wavelength limit (large fermion mass). In the next to leading order, the higher-derivative contributions to NC Chern-Simons are obtained. Moreover, the gauge invariance of the outcome action is carefully discussed. We then consider the higher-derivative modification into the pure NC Chern-Simons Lagrangian density and evaluate the one-loop correction to the pole of the photon propagator.

The aim of this paper is to propose a generalized Cardy formula for three-dimensional hyperscaling violation black holes. We first note that for the hyperscaling violation metrics, the scaling of the entropy in terms of the temperature (defined as the effective spatial dimensionality divided by the dynamical exponent) depends explicitly on the gravity theory. Starting from this observation, we first explore the case of quadratic curvature gravity theories for which we derive four classes of asymptotically hyperscaling violation black holes. For each solution, we compute the mass as well as the mass of the soliton counterpart obtained through a double Wick rotation. Assuming that the partition function has a certain invariance involving the effective spatial dimensionality, a generalized Cardy formula is derived. This latter is shown to correctly reproduce the entropy where the ground state is identified with the soliton. Comparing our formula with the one derived in the standard Einstein gravity case with source, we stress the role played by the effective spatial dimensionality. From this observation, we speculate the general form of the Cardy formula for hyperscaling violation metric with an arbitrary value of the effective spatial dimensionality. Finally, we test the viability of this formula in the case of a cubic gravity theory.

We extract constraints on the transition redshift $z_{\text{tr}}$, determining the onset of cosmic acceleration, predicted by an effective cosmographic construction, in the framework of $f(T)$ gravity. In particular, employing cosmography we obtain bounds on the viable $f(T)$ forms and their derivatives. Since this procedure is model independent, as long as the scalar curvature is fixed, we are able to determine intervals for $z_{\text{tr}}$. In this way we guarantee that the Solar-System constraints are preserved and, moreover, we extract bounds on the transition time and the free parameters of the scenario. We find that the transition redshifts predicted by $f(T)$ cosmology, although compatible with the standard $\mathrm{\Lambda }\mathrm{CDM}$ predictions, are slightly smaller. Finally, in order to obtain observational constraints on $f(T)$ cosmology, we perform a Monte Carlo fitting using supernova data, involving the most recent Union 2.1 data set.

We apply the methods of transformation optics to theoretical descriptions of spacetimes that support closed null geodesic curves. The metric used is based on frame dragging spacetimes, such as the van Stockum dust or the Kerr black hole. Through transformation optics, this metric is analogous to a material that in theory should allow for communication between past and future. Presented herein is a derivation and description of the spacetime and the resulting permeability, permittivity, and magnetoelectric couplings that a material would need in order for light in the material to follow closed null geodesics. We also address the paradoxical implications of such a material and demonstrate why such a material would not actually result in a violation of causality. A full derivation of the Plebanski equations is also included.

We present a first simulation of the post-merger evolution of a black hole-neutron star binary in full general relativity using an energy-integrated general-relativistic truncated moment formalism for neutrino transport. We describe our implementation of the moment formalism and important tests of our code, before studying the formation phase of an accretion disk after a black hole-neutron star merger. We use as initial data an existing general-relativistic simulation of the merger of a neutron star of mass $1.4M_{\odot }$ with a black hole of mass $7M_{\odot }$ and dimensionless spin ${\chi }_{\mathrm{BH}}=0.8$. Comparing with a simpler leakage scheme for the treatment of the neutrinos, we find noticeable differences in the neutron-to-proton ratio in and around the disk, and in the neutrino luminosity. We find that the electron neutrino luminosity is much lower in the transport simulations, and that both the disk and the disk outflows are less neutron rich. The spatial distribution of the neutrinos is significantly affected by relativistic effects, due to large velocities and curvature in the regions of strongest emission. Over the short time scale evolved, we do not observe purely neutrino-driven outflows. However, a small amount of material ($3\times {10}^{-4}{M}_{\odot }$) is ejected in the polar region during the circularization of the disk. Most of that material is ejected early in the formation of the disk, and is fairly neutron rich (electron fraction $Y_e\sim 0.15–0.25$). Through r-process nucleosynthesis, that material should produce high-opacity lanthanides in the polar region, and could thus affect the light curve of radioactively powered electromagnetic transients. We also show that by the end of the simulation, while the bulk of the disk remains neutron rich ($Y_e\sim 0.15–0.2$ and decreasing), its outer layers have a higher electron fraction: 10% of the remaining mass has $Y_e>0.3$. As that material would be the first to be unbound by disk outflows on longer time scales, and as composition evolution is slower at later times, the changes in $Y_e$ experienced during the formation phase of the disk could have an impact on nucleosynthesis outputs from neutrino-driven and viscously driven outflows. Finally, we find that the effective viscosity due to momentum transport by neutrinos is unlikely to have a strong effect on the growth of the magnetorotational instability in the post-merger accretion disk.

The warm Chaplygin inflationary universe model in the context of the effective field theory of loop quantum cosmology (LQC) is studied. In the slow-roll phase of inflation primordial perturbation spectrums, tensor-to-scalar ratio and spectral indices of our model are presented. Using chaotic potential, we present the main characteristics of this model in great detail. The parameters of the model are restricted by recent observational results i.e. WMAP9 and Planck data.

Perturbation theory for dark matter clustering has received a lot of attention in recent years, but its convergence properties remain poorly justified and there is no successful model that works both for correlation functions and for power spectra. Here we present the halo Zel’dovich approach combined with perturbation theory, in which we use standard perturbation theory at one-loop order (SPT) at very low $k$, and connect it to a version of the halo model, for which we adopt the Zel’dovich approximation plus a Padé expansion of a compensated one-halo term. This low-$k$ matching allows us to determine the one-halo term amplitude and redshift evolution, both of which are in an excellent agreement with simulations, and approximately agree with the expected value from the halo model. Our Padé expansion approach of the one-halo term added to the Zel’dovich approximation identifies a typical halo scale averaged over the halo mass function, the halo radius scale of order of $1\mathrm{Mpc}/\mathrm{h}$, and a much larger halo mass compensation scale, which can be determined from SPT. The model gives better than one-percent-accurate predictions for the correlation function above $5\mathrm{Mpc}/\mathrm{h}$ at all redshifts, without any free parameters. With three fitted Padé expansion coefficients the agreement in the power spectrum is good to a percent up to $k\sim 1\mathrm{h}/\mathrm{Mpc}$, which can be improved to arbitrary $k$ by adding higher-order terms in the Padé expansion.

Planck-2015 data seem to favor a large value of the lensing amplitude parameter, $A_{\mathrm{L}}=1.22\pm 0.10$, in CMB spectra. This result is in $2\sigma$ tension with the lensing reconstruction result, $A_{\mathrm{L}}^{\varphi \varphi }=0.95\pm 0.04$. In this paper, we simulate several CMB anisotropy and CMB lensing spectra based on Planck-2015 best-fit cosmological parameter values and Planck bluebook beam and noise specifications. We analyze several modified gravity models within the effective field theory framework against these simulations and find that models whose effective Newton constant is enhanced can modulate the CMB anisotropy spectra in a way similar to that of the $A_{\mathrm{L}}$ parameter. However, in order to lens the CMB anisotropies sufficiently, like in the Planck-2015 results, the growth of matter perturbations is substantially enhanced and gives a high ${\sigma }_8$ value. This in turn proves to be problematic when combining CMB anisotropy data from Planck with other data, such as weak lensing from CFHTLenS which favor a smaller amplitude of matter fluctuations.

Searches in final states with two leptons plus missing transverse energy, targeting supersymmetric particles or invisible decays of the Higgs boson, were performed during Run 1 of the LHC. Recasting the results of these analyses in the context of the inert doublet model (IDM) using MadAnalysis 5, we show that they provide constraints on inert scalars that significantly extend previous limits from LEP. Moreover, these LHC constraints allow us to test the IDM in the limit of very small Higgs–inert scalar coupling, where the constraints from direct detection of dark matter and the invisible Higgs width vanish.

Tentative evidence for excess GeV-scale gamma rays from the Galactic Center has been corroborated by several groups, including the Fermi collaboration, on whose data the observation is based. Dark matter annihilation into standard model particles has been shown to give a good fit to the signal for a variety of final state particles, but models with heavy mediators are typically inconsistent with constraints from direct detection or monojets. Models where the dark matter annihilates to mediators that subsequently decay are less constrained. We perform global fits of such models to recent data, allowing branching fractions to all possible fermionic final states to vary. The best fit models, including constraints from the AMS-02 experiment (and also antiproton ratio), require branching primarily to muons, with a $\sim 10–20\%$ admixture of $b$ quarks, and no other species. This suggests models in which there are two scalar mediators that mix with the Higgs, and have masses consistent with such a decay pattern. The scalar that decays to ${\mu }^{+}{\mu }^{-}$ must therefore be lighter than $2m_{\tau }\cong 3.6\mathrm{GeV}$. Such a small mass can cause Sommerfeld enhancement, which is useful to explain why the best-fit annihilation cross section is larger than the value needed for a thermal relic density. For light mediator masses (0.2–2) GeV, it can also naturally lead to elastic dark matter self-interactions at the right level for addressing discrepancies in small structure formation as predicted by collisionless cold dark matter.

We construct an energy-momentum tensor on the lattice which satisfies the appropriate Ward identities (WIs) and has the right trace anomaly in the continuum limit. It is defined by imposing suitable WIs associated to the Poincaré invariance of the continuum theory. These relations come forth when the length of the box in the temporal direction is finite, and they take a particularly simple form if the coordinate and the periodicity axes are not aligned. We implement the method for the SU(3) Yang-Mills theory discretized with the standard Wilson action in the presence of shifted boundary conditions in the (short) temporal direction. By carrying out extensive numerical simulations, the renormalization constants of the traceless components of the tensor are determined with a precision of roughly half a percent for values of the bare coupling constant in the range $0\le g_0^2\le 1$.

Quarkonium-nucleus systems are composed of two interacting hadronic states without common valence quarks, which interact primarily through multigluon exchanges, realizing a color van der Waals force. We present lattice QCD calculations of the interactions of strange and charm quarkonia with light nuclei. Both the strangeonium-nucleus and charmonium-nucleus systems are found to be relatively deeply bound when the masses of the three light quarks are set equal to that of the physical strange quark. Extrapolation of these results to the physical light-quark masses suggests that the binding energy of charmonium to nuclear matter is $B_{\text{phys}}^{\mathrm{NM}}\lesssim 40\mathrm{MeV}$.

The color connection of the parton system is an important bridge to connect the perturbative process and the hadronization one. The special color connection of the four-heavy-quark system in $e^{+}{e}^{-}$ annihilation, which is the necessary one for the doubly heavy baryon and tetraquark productions is revisited. The hadronization effects, investigated with the help of the quark combination model are compared with the corresponding results employing the Lund string model in our previous work. The global properties related to a certain color connection are not sensitive to various hadronization models.

The inclusive production of a $\mathrm{\Upsilon }J/\psi$ pair in proton-proton interactions at the LHCb is considered. This process is forbidden at the leading order of perturbation theory, so channels such as double parton scattering, ${\chi }_b{\chi }_c$ pair production with subsequent radiative decays of $P$-wave quarkonia, contributions of color-octet states, and next-to-leading-order corrections are studied in detail. For all these channels we present theoretical predictions of the total cross sections at the LHCb and distributions over different kinematical variables. According to the results presented in the paper, the double parton interaction gives the main contribution to the cross section of the considered reaction.