We investigate the prospect of searching for new physics via the novel signature of same-sign $\mathrm{diboson}+{\cancel{E}}_T$ at the current and future LHC. We study three new physics models: (i) natural SUSY models, (ii) type-III seesaw model, and (iii) type-II seesaw/Georgi-Machacek model. In the first two class of models, this signature arises due to the presence of a singly-charged particle which has lifetime long enough to escape detection, while in the third model this signature originates resonantly from a doubly-charged particle produced along with two forward jets that, most likely, would escape detection. We analyze in great detail the discovery prospects of the signal in these three classes of models in the current as well as the upcoming runs of the LHC (such as HL-LHC, HE-LHC, and FCC-hh) by showing a distinction among these scenarios.

We explore if spacetime symmetric lattice field theory models with a finite Hilbert space per lattice site can reproduce asymptotic freedom in the two-dimensional $O(4)$ model. We focus on a simple class of such models with a five-dimensional local Hilbert space. We demonstrate how even the simplest model reproduces asymptotic freedom within the D-theory formalism but at the cost of increasing the size of the Hilbert space through coupling several layers of a two-dimensional lattice. We then argue that qubit regularization can be viewed as an effective field theory (EFT) even if the continuum limit cannot be reached, as long as we can tune the model close enough to the continuum limit where perturbation theory, or other analytical techniques, become viable. We construct a simple lattice model on a single layer with a four-dimensional local Hilbert space that acts like an excellent EFT of the original theory.

The differential cross section of coherent photoproduction of heavy quarkonia on nuclear targets is calculated within the QCD color dipole formalism. The higher-twist nuclear shadowing corresponding to the $\overline{Q}Q$ Fock component of the photon is calculated including the correlation between dipole orientation $\overrightarrow{r}$ and impact parameter of a collision $\overrightarrow{b}$, which is related to the transverse momentum transfer via the Fourier transform. We also included the leading-twist gluon shadowing corresponding to higher Fock components of the photon containing gluons, which have specifically short coherence time, especially for multigluon components, even at very high energies. The contribution of such fluctuating gluonic dipole is calculated employing the path-integral technique. Our results are in good agreement with recent ALICE data on charmonium production in ultraperipheral nuclear collisions.

We study the two-body decays of mesons using the covariant helicity formalism. In particular, we show how the partial wave analysis of decays constrains the interacting terms entering the Lagrangian describing the decays of mesons with $J=1$ and $J=2$. We use available information on partial wave analysis to study specific mesonic decays and to make predictions for not yet measured quantities as well as to investigate the isoscalar mixing angle in the axial-vector, pseudovector and pseudotensor sectors. In particular, in the axial-vector sector our result agrees with the LHCb one, and in the pseudotensor sector we confirm a quite large (and negative) angle in the nonstrange-strange basis, which is compatible with a large contribute of the axial anomaly.

Given the complexity and length of the several original formulas presented for the energy-momentum and helicity of gauge fields coupled to a pseudoscalar inflaton, typos and errors appear in the published version of [Phys. Rev. D 100, 123542 (2019)]. With this Erratum, we wish to rectify most of the formulas and all the plots presented. Note that these corrections do not alter the conclusions of the paper and further clarify our main results.

The goal of the present paper is to calculate the complex structure moduli space Kähler potentials for hypersurfaces in weighted projective spaces and compare with the partition functions of their mirror gauged linear sigma models. We explicitly perform the Kähler potential computation and show that the corresponding formula is well defined in the case of quasismooth hypersurfaces. We then construct the mirror gauged linear sigma models with an appropriate number of Kähler parameters and discuss the interpretation of its partition function in terms of mirror symmetry. Namely, it is shown that different contributions to the partition function are related to various charts of the complex structure moduli space.

We point out that if the sector associated with the Standard Model degrees of freedom entered an open string Hagedorn phase in the early universe while the dark radiation sector was not part of this plasma, then this can lead to low values of the observable $\mathrm{\Delta }{N}_{\mathrm{eff}}$ (effective number of additional neutrinolike species). For explicit analysis, we focus on warped string compactifications with the Standard Model degrees of freedom at the bottom of a warped throat. If the Hubble scale during inflation is above the warped string scale associated with the throat, then the Standard Model sector will enter the Hagedorn phase. In this scenario, bulk axions are no longer dangerous from the point of view of dark radiation. While this article focuses on warped compactifications, the basic idea can be relevant to any scenario where the early universe entered a Hagedorn phase.

By using the free field worldsheet realization described by Gaberdiel and Gopakumar recently, we construct the nontrivial lowest generators of the higher spin superalgebra $hs(2,2|4)$. They consist of cubic terms between the bilinears of ambitwistorlike fields. We also obtain the worldsheet description for the findings of Sezgin and Sundell twenty years ago given by the familiar oscillator construction. The first order poles of the operator product expansions (OPEs), between the conformal weight-1 generators of Lie superalgebra $PSU(2,2|4)$ and the above conformal weight-3 generators of $hs(2,2|4)$, are determined explicitly and the additional generators appear in the worldsheet theory.

We define bulk/boundary maps corresponding to quantum gravity states in the tensorial group field theory formalism, for quantum geometric models sharing the same type of quantum states of loop quantum gravity. The maps are defined in terms of a partition of the quantum geometric data associated to an open graph into bulk and boundary ones, in the spin representation. We determine the general condition on the entanglement structure of the state that makes the bulk/boundary map isometric (a necessary condition for holographic behavior), and we analyze different types of quantum states, identifying those that define isometric bulk-to-boundary maps.

We study the instability of the charged Gauss–Bonnet–de Sitter black holes under gravito-electromagnetic perturbations. We adopt two criteria to search for an instability of the scalar type perturbations, including the local instability criterion based on the ${\mathrm{AdS}}_2$ Breitenlöhner-Freedman (BF) bound at extremality and the dynamical instability via quasinormal modes by full numerical analysis. We uncover the gravitational instability in five spacetime dimensions and above, and construct the complete parameter space in terms of the ratio of event and cosmological horizons and the Gauss-Bonnet coupling. We show that the BF bound violation is a sufficient but not necessary condition for the presence of dynamical instability. While the physical origin of the instability without the Gauss-Bonnet term has been argued to be from the ${\mathrm{AdS}}_2$ BF bound violation, our analysis suggests that the BF bound violation cannot account for all physical origin of the instability for the charged Gauss-Bonnet black holes.

The cosmic microwave background (CMB) serves as a backlight to large-scale structure during the epoch of reionization, where Thomson scattering gives rise to temperature anisotropies on small angular scales from the kinetic Sunyaev Zel’dovich (kSZ) effect. In this paper, we demonstrate that the technique of kSZ tomography (velocity reconstruction), based on cross-correlations between CMB temperature and 21-cm surveys, can significantly improve constraints on models of inhomogeneous reionization and provide information about large-scale modes that are poorly characterized by 21-cm measurements themselves due to foreground contamination.

Most of the phenomenology of loop quantum gravity in the cosmological sector is based on the so-called holonomy correction to the Hamiltonian constraint. It straightforwardly modifies the Friedmann equations. In this work, we investigate the influence of corrections generalizing the one usually used in loop quantum cosmology. We find that a long enough inflation phase can be generated by purely quantum geometrical effects but we also underline the limitations of this scenario. In addition, we study the effects of generalized holonomy corrections on an inflationary phase generated by a massive scalar field. At the level of perturbations, we investigate in detail the consequences on the primordial scalar power spectrum. The results are actually quite general and can be used beyond the “loop” framework.

Since the advent of the accelerated expanding homogeneous universe model, some other explanations for the type Ia supernova dimming have been explored, among which there are inhomogeneous models constructed with exact $\mathrm{\Lambda }=0$ solutions of Einstein’s equations. They have been used either to be a one patch or to build Swiss-cheese models. The most studied ones have been the Lemaître-Tolman-Bondi (LTB) models. However, these models being spatially spherical, they are not well designed to reproduce the large scale structures which exhibit clusters, filaments, and nonspherical voids. This is the reason why Szekeres models, which are devoid of any symmetry, have recently come into play. In this paper, we give the equations and an algorithm to compute the redshift drift for the most general quasispherical Szekeres (QSS) models with no dark energy. We apply it to a QSS model recently proposed by Bolejko and Sussman (BSQSS model) who averaged their model to reproduce the density distribution of the Alexander and collaborators’ LTB model which is able to fit a large set of cosmological data without dark energy. They concluded that their model represents a significant improvement over the observed cosmic structure description by spherical LTB models. We show here that this QSS model is ruled out by a negative cosmological redshift, i.e., a blueshift, which is not observed in the universe. We also compute a positive redshift and the redshift drift for the model of Alexander et al. and compare this redshift drift to that of the $\mathrm{\Lambda }\mathrm{CDM}$ model. We conclude that the process of averaging an unphysical QSS model can lead to obtain a physical model able to reproduce our observed local universe with no dark energy need and that the redshift drift can discriminate between this model and the $\mathrm{\Lambda }\mathrm{CDM}$ model. For completeness, we also compute the blueshift drift of the BSQSS model.

We present the first observation by the Telescope Array Surface Detector (TASD) of the effect of thunderstorms on the development of cosmic ray single count rate intensity over a $700{\mathrm{km}}^2$ area. Observations of variations in the secondary low-energy cosmic ray counting rate, using the TASD, allow us to study the electric field inside thunderstorms, on a large scale, as it progresses on top of the $700{\mathrm{km}}^2$ detector, without dealing with the limitation of narrow exposure in time and space using balloons and aircraft detectors. In this work, variations in the cosmic ray intensity (single count rate) using the TASD, were studied and found to be on average at the $\sim (0.5–1)\%$ and up to 2% level. These observations were found to be both in excess and in deficit. They were also found to be correlated with lightning in addition to thunderstorms. These variations lasted for tens of minutes; their footprint on the ground ranged from 6 km to 24 km in diameter and moved in the same direction as the thunderstorm. With the use of simple electric field models inside the cloud and between cloud to ground, the observed variations in the cosmic ray single count rate were recreated using CORSIKA simulations. Depending on the electric field model used and the direction of the electric field in that model, the electric field magnitude that reproduces the observed low-energy cosmic ray single count rate variations was found to be approximately between 0.2 GV–0.4 GV. This in turn allows us to get a reasonable insight on the electric field and its effect on cosmic ray air showers inside thunderstorms.

The High-Energy Particle Detector (HEPD) on board the China Seismo-Electromagnetic Satellite (CSES-01) was launched in February 2018, with a foreseen mission lifetime of over 5 years. It is providing crucial new insight in the physical dynamics of the radiation belts in the Earth’s magnetosphere, in particular in the South Atlantic Anomaly (SAA). In this work, proton data from HEPD in the 40 MeV–250 MeV energy range, collected inside the SAA during the period between August 2018 and December 2020, are presented and compared with the up-to-date AP9 model by NASA. These are the first results on SAA protons at Low-Earth Orbit during the minimum activity phase between the 24th and the 25th solar cycles below 250 MeV. They enable an extensive testing and validation of current theoretical and empirical models aimed at predictions of temporal changes in this critical region of space. HEPD is advancing the observations collected by the PAMELA space experiment and NASA Van Allen Probe during the last 15 years through the 23rd and 24th solar cycles.

Loop diagram calculations typically rely on reduction to a finite set of master integrals in $4-2\epsilon$ dimensions. It has been shown that for any problem, the masters can be chosen so that their coefficients are finite as $\epsilon \to 0$. I propose a definition of renormalized $\epsilon$-finite master integrals, which incorporate ultraviolet divergence subtractions in a specific way. A key advantage of this choice is that in expressions for physical observables, expansions to positive powers in $\epsilon$ are never needed. As an example, I provide the subtractions for general three-loop self-energy integrals. The differential equations method is used to compute numerically the renormalized $\epsilon$-finite master integrals for the arbitrary external momentum invariant, in special cases with internal masses equal to a single scale or zero. These include the ones necessary for the three-loop QCD corrections to the self-energies of the $W$, $Z$, and Higgs bosons. In principle, the same method should provide for the numerical computation of general three-loop self energies with any masses.

Recent theoretical work has explored dark matter accumulation in the Earth and its drift toward the center of the Earth that, for the current age of the Earth, does not necessarily result in a concentration of dark matter ($\chi$) in the Earth’s core. We consider a scenario of long-lived (${\tau }_{\chi }\sim {10}^{28}\mathrm{s}$), superheavy ($m_{\chi }={10}^7–{10}^{10}\mathrm{GeV}$) dark matter that decays via $\chi \to {\nu }_{\tau }{\overline{\nu }}_{\tau }$ or $\chi \to {\nu }_{\mu }{\overline{\nu }}_{\mu }$. We show that an IceCube-like detector over 10 years can constrain a dark matter density that mirrors the Earth’s density or has a uniform density with density fraction ${\epsilon }_{\rho }$ combined with the partial decay width $B_{\chi \to {\nu }_{\tau }{\overline{\nu }}_{\tau }}{\mathrm{\Gamma }}_{\chi }$ in the range of $({\epsilon }_{\rho }/{10}^{-10})B_{\chi \to {\nu }_{\tau }}{\mathrm{\Gamma }}_{\chi }\lesssim 1.5\times {10}^{-29}–1.5\times {10}^{-28}{\mathrm{s}}^{-1}$. For $\chi \to {\nu }_{\mu }{\overline{\nu }}_{\mu }$, $m_{\chi }={10}^8–{10}^{10}\mathrm{GeV}$, and $E_{\mu }>{10}^7\mathrm{GeV}$, the range of constraints is $({\epsilon }_{\rho }/{10}^{-10})B_{\chi \to {\nu }_{\mu }}{\mathrm{\Gamma }}_{\chi }\lesssim 3\times {10}^{-29}–7\times {10}^{-28}{\mathrm{s}}^{-1}$.

The gravitational form factors (GFFs) of hadrons encode the matrix elements of the energy-momentum tensor of QCD. These quantities describe how energy, spin, and various mechanical properties of hadrons are carried by their quark and gluon constituents. We present the gluon GFFs of the pion, nucleon, $\rho$ meson, and $\mathrm{\Delta }$ baryon as functions of the squared momentum transfer $t$ in the region $0\le -t<2{\mathrm{GeV}}^2$, as determined in a lattice QCD study with pion mass $m_{\pi }=450(5)\mathrm{MeV}$. By fitting the extracted GFFs using multipole and z-parameter expansion functional forms, we extract various gluon contributions to the energy, pressure, and shear force distributions of the hadrons in the 3D and 2D Breit frames as well as in the infinite momentum frame. We also obtain estimates for the corresponding gluon mechanical and mass radii, as well as the forward-limit gluon contributions to the momentum fraction and angular momentum of the hadrons.

We describe a heavy and exotic tetraquark state as a holographic molecule, by binding the lightest heavy-light meson $(0^{-},1^{-})$ multiplet to a flavored sphaleron, in the bulk of the Witten-Sakai-Sugimoto model. Bound tetraquark states emerge as Efimov states in the heavy quark limit, with a binding energy for a charm tetraquark comparable to the $T_{cc}^{+}$ recently reported by the LHCb collaboration, but with a substantially smaller width, for a large but finite ’t Hooft coupling. Fixing the parameters of the model at the empirical mass of $T_{cc}^{+}$, allows for a prediction of the bindings of the undiscovered bottom-charm and bottom tetraquarks.