Recently, a class of stationary black hole solutions with non-Killing horizon in the asymptotic AdS bulk space (i.e., nonequilibrium black funnel) was constructed to describe the far from equilibrium heat transport and particle transport between the boundary black holes via AdS/CFT correspondence. It is generally believed that the temperature of a black hole with non-Killing horizon can not be properly defined by the conventional methods used in the equilibrium black holes with Killing horizon. In this study, we calculate the spectrum of Hawking radiation of the nonequilibrium black funnel using the Damour-Ruffini method. Our results indicate that the spectrum and the temperatures as well as the chemical potentials of the nonequilibrium black funnel do depend on one of the spatial coordinates. This is different from the equilibrium black holes with Killing horizon, where the temperatures are uniform. Therefore, the black hole with non-Killing horizon can be overall in nonequilibrium steady state while the Hawking temperature of the black funnel can be viewed as the local temperature and the corresponding Hawking radiation can be regarded as being in the local equilibrium with the horizon of the black funnel. By AdS/CFT, we discuss some possible implications of our results of local Hawking temperature for the nonequilibrium thermodynamics of dual conformal field theory. We further discuss the nonequilibrium thermodynamics of the black funnel, where the first law can be formulated as the entropy production rate being equal to the sum of the changes of the entropies from the system (black funnel) and environments while the second law is given by the entropy production being larger than or equal to zero. We found the time arrow emerged from the nonequilibrium black hole heat and particle transport dissipation. We also discuss how the nonequilibrium dissipation may influence the evaporation process of the black funnel.

We argue that the equations of motion of quantum field theories in curved backgrounds encode new underlying black hole thermodynamic relations. We define new entropy variation relations. These “emerge” through the monodromies that capture the infinitesimal changes in the black hole background produced by the field excitations. This raises the possibility of new thermodynamic relations defined as independent sums involving entropies, temperatures, and angular velocities defined at every black hole horizon. We present explicit results for the sum of all horizon entropy variations for general rotating black holes, in both asymptotically flat and asymptotically anti–de Sitter spacetimes in four and higher dimensions. The expressions are universal and in most cases add up to zero. We also find that these thermodynamic summation relations apply in theories involving multicharge black holes.

In this paper, we study the pion leading-twist distribution amplitude (DA) ${\varphi }_{2;\pi }(x,\mu )$ by improving the traditional light-cone harmonic oscillator model within the reconstruction of the function ${\phi }_{2;\pi }(x)$. In order to constrain the model parameters, we calculate its moments $⟨{\xi }^n{⟩}_{2;\pi }{|}_{\mu }$ in the framework of the QCD background field theory sum rule up to tenth order. Considering the fact that the sum rule of the zeroth moment $⟨{\xi }^0{⟩}_{2;\pi }{|}_{\mu }$ cannot be normalized, we suggest a more reasonable sum rule formula for $⟨{\xi }^n{⟩}_{2;\pi }{|}_{\mu }$. Then, we obtain the values of $⟨{\xi }^n{⟩}_{2;\pi }{|}_{{\mu }_0}$ with $n=(2,4,6,8,10)$ at the initial scale ${\mu }_0=1\mathrm{GeV}$. The first two moments are $⟨{\xi }^2{⟩}_{2;\pi }{|}_{{\mu }_0}=0.271\pm 0.013$ and $⟨{\xi }^4{⟩}_{2;\pi }{|}_{{\mu }_0}=0.138\pm 0.010$, and the corresponding Gegenbauer moments are $a_2^{2;\pi }({\mu }_0)=0.206\pm 0.038$ and $a_4^{2;\pi }({\mu }_0)=0.047\pm 0.011$, respectively. After fitting the moments $⟨{\xi }^n{⟩}_{2;\pi }{|}_{\mu }$, we obtain the appropriate model parameters by using the least squares method. The resultant behavior for the twist-2 pion DA is closer to the AdS/QCD and lattice results, but narrower than that obtained using the Dyson-Schwinger equation. Furthermore, we calculate the pion-photon transition form factors (TFFs) and $B\to \pi$ TFFs within the light-cone sum rule approach, which conform with experimental and theoretical results.

We construct a theory of real scalar fields that interpolates between two different theories: a Lee-Wick theory with $N$ propagator poles, including $N-1$ Lee-Wick partners, and a nonlocal infinite-derivative theory with kinetic terms modified by an entire function of derivatives with only one propagator pole. Since the latter description arises when taking the $N\to \infty$ limit, we refer to the theory as “asymptotically nonlocal.” Introducing an auxiliary-field formulation of the theory allows one to recover either the higher-derivative form (for any $N$) or the Lee-Wick form of the Lagrangian, depending on which auxiliary fields are integrated out. The effective scale that regulates quadratic divergences in the large-$N$ theory is the would-be nonlocal scale, which can be hierarchically lower than the mass of the lightest Lee-Wick resonance. We comment on the possible utility of this construction in addressing the hierarchy problem.

Based on the Dyson-Schwinger equation, we compute the resummed gluon propagator in a holonomous plasma that is described by introducing a constant background field for the vector potential $A_0$. Because of the transversality of the holonomous hard thermal loop in gluon self-energy, the resummed propagator has a similar Lorentz structure as that in the perturbative quark-gluon plasma where the holonomy vanishes. As for the color structures, since diagonal gluons are mixed in the overcomplete double-line basis, only the propagators for off-diagonal gluons can be obtained unambiguously. On the other hand, multiplied by a projection operator, the propagators for diagonal gluons, which exhibit a highly nontrivial dependence on the background field, are uniquely determined after summing over the color indices. As an application of these results, we consider the Debye screening effect on the in-medium binding of quarkonium states by analyzing the static limit of the resummed gluon propagator. In general, introducing nonzero holonomy merely amounts to modifications on the perturbative screening mass $m_D$ and the resulting heavy-quark potential, which remains the standard Debye screened form, is always deeper than the screened potential in the perturbative quark-gluon plasma. Therefore, a weaker screening and, thus, a more tightly bounded quarkonium state can be expected in a holonomous plasma. In addition, both the diagonal and off-diagonal gluons become distinguishable by their modified screening masses ${\mathcal{M}}_D$, and the temperature dependence of the ratio ${\mathcal{M}}_D/T$ shows a very similar behavior as that found in lattice simulations.

We study $U(N{)}_k$ Chern-Simons theory on lens space in Seifert framing and write down the partition function as a unitary matrix model. In the large $k$ and large $N$ limit the eigenvalue density satisfies an upper cap $\frac{1}{2\pi \lambda }$ where $\lambda =N/(k+N)=\text{fixed}$. The eigenvalue density of the standard gapped phase saturates the upper cap at a critical value of $\lambda$ and ceases to exist beyond that. We find a new phase (cap-gap phase) in this theory for $\lambda$ beyond the critical value and see that the on-shell free energy for the cap-gap phase is less than that of the gapped phase.

We analyze the canonical quantum dynamics of the isotropic universe, as emerging from the Hamiltonian formulation of a metric $f(R)$ gravity, viewed in the Jordan frame. The canonical method of quantization is performed by solving the Hamiltonian constraint before quantizing and adopting like a relational time the nonminimally coupled scalar field emerging in the Jordan frame. The resulting Schrödinger evolution is then investigated both in the vacuum and in the presence of a massless scalar field, though as the kinetic component of an inflaton. We show that, in vacuum, the morphology of localized wave packets is that of a nonspreading profile up to the cosmological singularity. When the external scalar field is included into the dynamics, we see that the wave packets acquire the surprising feature of increasing localization of the universe volume, as it expands. This result suggests that, in the metric $f(R)$ formulation of gravity, a spontaneous mechanism arises for the Universe classicalization. Actually, when the phase space of the scalar field is fully explored, such an increasing localization in the Universe volume is valid up to a given value of the time, i.e., of the nonminimally coupled mode after which the wave packets spread again. We conclude our analysis by inferring that before this critical transition age is reached, the inflationary phase could take place, here modeled via a cosmological constant. This point of view provides an interesting scenario for the transition from a Planckian Universe to a classical de-Sitter phase, which in the $f(R)$ gravity appears more natural than in the Einsteinian picture.

The measurement of the epicyclic frequencies is a widely used astrophysical technique to infer information on a given self-gravitating system and on the related gravity background. We derive their explicit expressions in static and spherically symmetric wormhole spacetimes. We discuss how these theoretical results can be applied to: (1) detect the presence of a wormhole, distinguishing it by a black hole; (2) reconstruct wormhole solutions through the fit of the observational data, once we have them. Finally, we discuss the physical implications of our proposed epicyclic method.

We investigate the clustering property of primordial black holes (PBHs) in a scenario where PBHs can explain the existence of supermassive black holes (SMBHs) at high redshifts. We analyze the angular correlation function of PBHs originating from fluctuations of a spectator field which can be regarded as a representative model to explain SMBHs without conflicting with the constraint from the spectral distortion of cosmic microwave background. We argue that the clustering property of PBHs can give a critical test for models with PBHs as the origin of SMBHs and indeed show that the spatial distribution of PBHs in such a scenario is highly clustered, which suggests that those models may be disfavored from observations of SMBHs although a careful comparison with observational data would be necessary.

Most cosmological data analysis today relies on the Friedmann-Lemaître-Robertson-Walker (FLRW) metric, providing the basis of the current standard cosmological model. Within this framework, interesting tensions between our increasingly precise data and theoretical predictions are coming to light. It is therefore reasonable to explore the potential for cosmological analysis outside of the exact FLRW cosmological framework. In this work we adopt the general luminosity-distance series expansion in redshift with no assumptions of homogeneity or isotropy. This framework will allow for a full model-independent analysis of near-future low-redshift cosmological surveys. We calculate the effective observational ‘Hubble’, ‘deceleration’, ‘curvature’ and ‘jerk’ parameters of the luminosity-distance series expansion in numerical relativity simulations of realistic structure formation, for observers located in different environments and with different levels of sky-coverage. With a ‘fairly-sampled’ sky, we find 2% and 15% cosmic variance in the ‘Hubble’ and ‘deceleration’ parameters for scales of $200\mathrm{Mpc}/h$ (corresponding to density contrasts of $\sim 0.1$ in the simulated model universe), respectively. On top of this, we find that typical observers measure maximal sky-variance of 7% and 550% in the same parameters, as compared to their analogies in the large scale FLRW model. Our work suggests the inclusion of low-redshift anisotropy in cosmological analysis could be important for drawing correct conclusions about our Universe.

We investigate the capability of the DUNE near detector (ND) to constrain nonstandard interaction parameters (NSIs) describing the production of neutrinos $({ϵ}_{\alpha \beta }^s)$ and their detection $({ϵ}_{\alpha \beta }^d)$. We show that the DUNE ND is able to reject a large portion of the parameter space allowed by DUNE far detector analyses and to set the most stringent bounds from accelerator neutrino experiments on $|{ϵ}_{\mu e}^{s,d}|$ for wide intervals of the related phases. We also provide simple analytic understanding of our results as well as a numerical study of their dependence on the systematic errors, showing that the DUNE ND offers a clean environment to study source and detector NSIs.

We present predictions for the distribution of rapidity gaps in realistic kinematics of future electron-ion colliders, based on numerical solutions of the original Kovchegov-Levin equation and of its next-to-leading extension taking into account the running of the strong coupling. We find that for the rapidities we have considered, the fixed and the running coupling equations lead to different distributions whose general shape is rather insensitive to the chosen prescription in the running coupling case. The obtained distributions for the fixed coupling framework exhibit a shape characteristic of a recently proposed partonic picture of diffractive dissociation already at rapidities accessible at future electron-ion colliders. The modification of this shape in the running coupling case can also be understood qualitatively from that picture. Our results confirm the relevance of measurements of such observables for the microscopic understanding of diffractive dissociation in the framework of quantum chromodynamics.

We examine the radiation emitted by high-energy positrons channeled into silicon crystal samples. The positrons are modeled as semiclassical vector currents coupled to an Unruh-DeWitt detector to incorporate any local change in the energy of the positron. In the subsequent accelerated QED analysis, we discover a Larmor formula and power spectrum that are both thermalized by the acceleration. Thus, these systems explicitly exhibit thermalization of the detector energy gap at the celebrated Fulling-Davies-Unruh (FDU) temperature. Our derived power spectrum, with a nonzero energy gap, is then shown to have an excellent statistical agreement with high-energy channeling experiments and also provides a method to directly measure the FDU temperature. We also investigate the Rindler horizon dynamics and confirm that the Bekenstein-Hawking area-entropy law is satisfied in these experiments. As such, we present the evidence for the first observation of acceleration-induced thermality in a nonanalog system.

In $f(R)$ gravity, the metric, presented in the form of the multipole expansion, for the external gravitational field of a spatially compact supported source up to $1/c^3$ order is provided, where $c$ is the velocity of light in vacuum. The metric consists of general relativity-like part and $f(R)$ part, where the latter is the correction to the former in $f(R)$ gravity. At the leading pole order, the metric can reduce to that for a pointlike or ball-like source. For the gyroscope moving around the source without experiencing any torque, the multipole expansions of its spin’s angular velocities of gravitoelectric-type precession, gravitomagnetic-type precession, $f(R)$ precession, and Thomas precession are all derived. The first two types of precession are collectively called general relativity-like precession, and the $f(R)$ precession is the correction in $f(R)$ gravity. At the leading pole order, these expansions can recover the results for the gyroscope moving around a pointlike or ball-like source. If the gyroscope has a nonzero four-acceleration, its spin’s total angular velocity of precession up to $1/c^3$ order in $f(R)$ gravity is the same as that in general relativity.

Understanding the Bondi-Metzner-Sachs (BMS) frame of the gravitational waves produced by numerical relativity is crucial for ensuring that analyses on such waveforms are performed properly. It is also important that models are built from waveforms in the same BMS frame. Up until now, however, the BMS frame of numerical waveforms has not been thoroughly examined, largely because the necessary tools have not existed. In this paper, we show how to analyze and map to a suitable BMS frame for numerical waveforms calculated with the Spectral Einstein Code (SpEC). However, the methods and tools that we present are general and can be applied to any numerical waveforms. We present an extensive study of 13 binary black hole systems that broadly span parameter space. From these simulations, we extract the strain and also the Weyl scalars using both SpECTRE’s Cauchy-characteristic extraction module and also the standard extrapolation procedure with a displacement memory correction applied during postprocessing. First, we show that the current center-of-mass correction used to map these waveforms to the center-of-mass frame is not as effective as previously thought. Consequently, we also develop an improved correction that utilizes asymptotic Poincaré charges instead of a Newtonian center-of-mass trajectory. Next, we map our waveforms to the post-Newtonian (PN) BMS frame using a PN strain waveform. This helps us find the unique BMS transformation that minimizes the $L^2$ norm of the difference between the numerical and PN strain waveforms during the early inspiral phase. We find that once the waveforms are mapped to the PN BMS frame, they can be hybridized with a PN strain waveform much more effectively than if one used any of the previous alignment schemes, which only utilize the Poincaré transformations.

In the framework of classical scale invariance, we consider quadratic gravity in the Palatini formalism and investigate the inflationary predictions of the theory. Our model corresponds to a two-field scalar-tensor theory, which involves the Higgs field and an extra scalar field stemming from a gauge $U(1{)}_X$ extension of the Standard Model, which contains an extra gauge boson and three right-handed neutrinos. Both scalar fields couple nonminimally to gravity and induce the Planck scale dynamically, once they develop vacuum expectation values. By means of the Gildener-Weinberg approach, we describe the inflationary dynamics in terms of a single scalar degree of freedom along the flat direction of the tree-level potential. The one-loop effective potential in the Einstein frame exhibits plateaus on both sides of the minimum and thus the model can accommodate both small and large field inflation. The inflationary predictions of the model are found to comply with the latest bounds set by the Planck collaboration for a wide range of parameters and the effect of the quadratic in curvature terms is to reduce the value of the tensor-to-scalar ratio.

In this article we extend a previous discussion about the influence of an external magnetic field on renormalons in a self-interacting scalar theory by including now temperature effects, in the imaginary formalism, together with an external weak external magnetic field. We show that the position of renormalons, which are poles in the Borel plane, does not change, getting their residues, however, a dependence on temperature and on the magnetic field. The effects of temperature and the magnetic field strength on the residues turn out to be opposite. We present a detailed discussion about the evolution of these residues, showing technical details involved in the calculation.

The Keldysh formalism is capable of describing driven-dissipative dynamics of open quantum systems as nonunitary effective field theories that are not necessarily thermodynamical, thus often exhibiting new physics. Here, we introduce a general Keldysh action that maximally obeys Weinbergian constraints, including locality, Poincaré invariance, and two “$CPT$” constraints: complete positivity and trace preserving as well as charge, parity, and time reversal symmetry. We find that the perturbative Lindblad term responsible for driven-dissipative dynamics introduced therein has the natural form of a double-trace deformation ${\mathcal{O}}^2$, which, in the large $N$ limit, possibly leads to a new nonthermal conformal fixed point. This fixed point is IR when $\mathrm{\Delta }<d/2$ or UV when $\mathrm{\Delta }>d/2$ given $d$ the dimensions of spacetime and $\mathrm{\Delta }$ the scaling dimension of $\mathcal{O}$. Such a UV fixed point being not forbidden by Weinbergian constraints may suggest its existence and even completion of itself, in contrast to the common sense that dissipation effects are always IR relevant. This observation implies that driven-dissipative dynamics is much richer than thermodynamics, differing in not only its noncompliance with thermodynamic symmetry (e.g., the fluctuation-dissipation relation) but its UV/IR relevance as well. Examples including a $(0+1)\text{−}d$ harmonic oscillator under continuous measurement and a $(4-\epsilon )\text{−}d$ classic $O(N)$ vector model with quartic interactions are studied.