In this work, we investigate the open-charm decay process $\psi \to {\mathrm{\Lambda }}_c{\overline{\mathrm{\Lambda }}}_c$ via the hadronic loop mechanism for vector charmonia above ${\mathrm{\Lambda }}_c{\overline{\mathrm{\Lambda }}}_c$ threshold. The branching ratios of these vector charmonium states to ${\mathrm{\Lambda }}_c{\overline{\mathrm{\Lambda }}}_c$ are estimated. The charmonium explanation of the $Y(4630)$ observed in $e^{+}{e}^{-}\to {\mathrm{\Lambda }}_c{\overline{\mathrm{\Lambda }}}_c$ is tested. Furthermore, for the predicted higher vector charmonia above 4.7 GeV, the branching ratios $\mathcal{B}[\psi (nS)\to {\mathrm{\Lambda }}_c{\overline{\mathrm{\Lambda }}}_c]$ with $n=7$, 8, 9 are found to be of the order of magnitude of ${10}^{-4}-{10}^{-3}$ while $\mathcal{B}[\psi (mD)\to {\mathrm{\Lambda }}_c{\overline{\mathrm{\Lambda }}}_c]$ with $m=6$, 7, 8 are of the order of magnitude of ${10}^{-3}-{10}^{-2}$. The experimental signals of these missing charmonium states are discussed. The search for them may be an interesting topic in the future BESIII and Belle II experiments.

We study four-dimensional gauge theories coupled to fermions in the fundamental and mesonlike scalars. All requisite beta functions are provided for general gauge group and fermion representation. In the regime where asymptotic freedom is absent, we determine all interacting fixed points using perturbation theory up to three loop in the gauge and two loop in the Yukawa and quartic couplings. We find that the conformal window of ultraviolet fixed points is narrowed down by finite-$N$ corrections beyond the Veneziano limit. We also find a new infrared fixed point whose main features, such as scaling exponents, UV-IR connecting trajectories, and phase diagram, are provided. Both fixed points collide upon varying the number of fermion flavors $N_{\mathrm{f}}$, and conformality is lost through a saddle-node bifurcation. We further revisit the prospect for ultraviolet fixed points in the large-$N_{\mathrm{f}}$ limit where matter field fluctuations dominate. Unlike at weak coupling, we do not find clear evidence for new scaling solutions even in the presence of scalar and Yukawa couplings.

We revisit the problem of building the Lagrangian of a large class of metric theories that respect spatial covariance, which propagate at most 2 degrees of freedom and in particular no scalar mode. The Lagrangians are polynomials built of the spatially covariant geometric quantities. By expanding the Lagrangian around a cosmological background and focusing on the scalar modes only, we find the conditions for the coefficients of the monomials in order to eliminate the scalar mode at the linear order in perturbations. We find the conditions up to $d=4$, with $d$ the total number of derivatives in the monomials, and determine the explicit Lagrangians for the cases of $d=2$, $d=3$ as well as the combination of $d=2$ and $d=3$. We also expand the Lagrangian of $d=2$ to the cubic order in perturbations, and find additional conditions for the coefficients such that the scalar mode is eliminated up to the cubic order. This perturbative analysis can be performed order by order, and one expects to determine the final Lagrangian at some finite order such that the scalar mode is fully eliminated. Our analysis provides an alternative and complimentary approach to building spatially covariant gravity with only tensorial degrees of freedom. The resulting theories can be used as alternatives to the general relativity to describe the tensorial gravitational waves in a cosmological setting.

During the early phase of inspiral of a binary system, the tidal heating of a compact object due to its companion plays a significant role in the determination of the orbital evolution of the binary. The phenomenon depends crucially on the “hairs,” as well as on the nature of the compact object. It turns out that the presence of extra dimension affects both these properties, by incorporating an extra tidal charge for braneworld black holes and also by introducing quantum effects, leading to possible existence of exotic compact objects. It turns out that the phasing information from tidal heating in the gravitational wave waveform can constrain the tidal charge inherited from extra dimension to a value $\sim {10}^{-6}$, the most stringent constraint, to date. Moreover, second order effects in tidal heating for exotic compact objects, also reveals an oscillatory behavior with respect to spin, which has unique signatures.

Numerous extended sources around Galactic pulsars have shown significant $\gamma$-ray emission from GeV to TeV energies, revealing hundreds of TeV energy electrons scattering off of the underlying photon fields through inverse Compton scattering (ICS). HAWC TeV gamma-ray observations of few-degree extended emission around the pulsars Geminga and Monogem, and LAT GeV emission around Geminga, suggest that systems older than 100 kyr have multi-TeV $e^{\pm }$ propagating beyond the SNR-PWN system into the interstellar medium. Following the discovery of few $\gamma$-ray sources by HAWC at energies $\mathrm{E}>100\mathrm{TeV}$, we investigate the presence of an extended $\gamma$-ray emission in Fermi-LAT data around the three brightest sources detected by HAWC up to 100 TeV. We find an extended emission of ${\theta }_{68}=1.00_{-0.07}^{+0.05}\mathrm{deg}$ around eHWC J1825-134 and ${\theta }_{68}=0.71\pm 0.10\mathrm{deg}$ eHWC $\mathrm{J}1907+063$. The analysis with ICS templates on Fermi-LAT data point to diffusion coefficient values which are significantly lower than the average Galactic one. When studied along with HAWC data, the $\gamma$-ray Fermi-LAT data provide invaluable insight into the very high-energy electron and positron parent populations.

Dense relativistic matter has attracted a lot of attention over many decades now, with a focus on an understanding of the phase structure and thermodynamics of dense strong-interaction matter. The analysis of dense strong-interaction matter is complicated by the fact that the system is expected to undergo a transition from a regime governed by spontaneous chiral symmetry breaking at low densities to a regime governed by the presence of a Cooper instability at intermediate and high densities. Renormalization group (RG) approaches have played and still play a prominent role in studies of dense matter, in general. In the present work, we study RG flows of dense relativistic systems in the presence of a Cooper instability and analyze the role of the Silver-Blaze property. In particular, we critically assess how to apply the derivative expansion to study dense-matter systems in a systematic fashion. This also involves a detailed discussion of regularization schemes. Guided by these formal developments, we introduce a new class of regulator functions for functional RG studies which is suitable to deal with the presence of a Cooper instability in relativistic theories. We close by demonstrating its application with the aid of a simple quark-diquark model.

We propose a pseudo-Goldstone boson dark matter (pGDM) particle in $SO(10)$ grand unified theory (GUT). Due to its Goldstone nature, this pGDM evades the direct DM detection experiments which, otherwise, severely constrain the parameter space of DM models. In $SO(10)$, the pGDM is embedded as a linear combination of the Standard Model (SM) singlet scalars in ${\mathbf{16}}_{\mathbf{H}}$ and ${\overline{\mathbf{126}}}_{\mathbf{H}}$ representations. We consider two scenarios for the intermediate route of $SO(10)$ symmetry breaking (SB) to the SM: $SU(5)\times U(1{)}_X$ and Pati-Salam the $SU(4{)}_c\times SU(2{)}_L\times SU(2{)}_R$ ($4\text{−}2\text{−}2$) gauge groups. The vacuum expectation value of ${\overline{\mathbf{126}}}_{\mathbf{H}}$, which triggers the breaking of $U(1{)}_X$ and $4\text{−}2\text{−}2$ symmetry in the two scenarios, respectively, determines the pGDM lifetime whose astrophysical lower bound provides one of the most stringent constraints. For the $4\text{−}2\text{−}2$ route to $SO(10)$, the successful SM gauge coupling unification requires the $4\text{−}2\text{−}2$ breaking scale to be $\mathcal{O}({10}^{11})\mathrm{GeV}$, and most of the parameter space is excluded. For the $SU(5)\times U(1{)}_X$ route, on the other hand, the $U(1{)}_X$ breaking scale can be significantly higher, and a wide range of the parameter space is allowed. Furthermore, the proton lifetime in the $SU(5)$ case is predicted to be $4.53\times {10}^{34}\mathrm{years}$, which lies well within the sensitivity reach of the Hyper-Kamiokande experiment. We also examine the constraints on the model parameter space from the Large Hadron Collider and the indirect DM search by Fermi-LAT and MAGIC experiments.

We show how current LIGO data is able to probe interesting theories beyond the Standard Model, particularly dark sectors where a dark Higgs boson triggers symmetry breaking via a first-order phase transition. We use publicly available LIGO O2 data to illustrate how these sectors, even if disconnected from the Standard Model, can be probed by gravitational wave detectors. We link the LIGO measurements with the model content and mass scale of the dark sector, finding that current O2 data are testing a broad set of scenarios that can be mapped into many different types of dark-sector models where the breaking of $SU(N)$ theories with $N_f$ fermions is triggered by a dark Higgs boson at scales $\mathrm{\Lambda }\simeq {10}^8–{10}^9\mathrm{GeV}$ with reasonable parameters for the scalar potential.

We investigate the renormalon ambiguity from bubble-chain diagrams in the isovector unpolarized quasiparton distribution function (PDF) of a hadron. We confirm the assertion by Braun, Vladimirov, and Zhang [Phys. Rev. D 99, 014013 (2019)] that the leading IR renormalon ambiguity is an $\mathcal{O}({\mathrm{\Lambda }}_{\mathrm{QCD}}^2/x^2{P}_z^2)$ effect, with $x$ the parton momentum fraction and $P_z$ the hadron momentum, together with a new $\mathcal{O}(\delta (x){\mathrm{\Lambda }}_{\mathrm{QCD}}^2/P_z^2)$ contribution such that the quark number is conserved. This implies the convergence of the perturbative matching kernel between a quasi-PDF and a PDF would eventually fail for small $x$. However, in both the $R$-scheme designed to cancel the leading IR renormalon and the typically used regularization-independent momentum subtraction scheme in lattice QCD for the same quasi-PDF, we find good convergence in the kernel based on three-loop bubble-chain diagram analyses. These results are encouraging for the quasi-PDF program. However, firm conclusions can only be drawn after the complete higher loop QCD calculations are carried out.

We analyze all available experimental data on the ${\nu }_{\mu }$ and ${\overline{\nu }}_{\mu }$ total and differential cross sections of charged-current single pion production through the decay of intermediate nucleon and baryon resonances measured on hydrogen and deuterium targets in the accelerator experiments at ANL, BNL, FNAL, and CERN. These data are used to determine the current “resonance” axial-vector mass of the nucleon and to fine tune the nonresonance noninterfering background contribution which described within the Rein-Sehgal approach. For this analysis, we revise the phenomenological model and the experimental dataset for the fits, modify the method of likelihood analysis compared to the previous study. The obtained model parameters coming in combination with a revised strategy for the normalization of the Breit-Wigner distributions are slightly different from the values used by default.

We study the concomitant breaking of spatial translations and dilatations in Ginzburg-Landau-like models, where the dynamics responsible for the symmetry breaking is described by an effective Mexican hat potential for spatial gradients. We show that there are fractonic modes with either subdimensional propagation or no propagation altogether, namely, immobility. Such a class of effective field theories encompasses instances of helical superfluids and metafluids, where fractons can be connected to an emergent symmetry under higher-moment charges, leading in turns to the trivialization of some elastic coefficients. The introduction of a finite-charge density alters the mobility properties of fractons and leads to a competition between the chemical potential and the superfluid velocity in determining the gap of the dilaton. The mobility of fractons can also be altered at zero density upon considering additional higher-derivative terms.

Black hole perturbation theory for Kerr black holes is best studied in the Newman-Penrose formalism, in which gravitational waves are described as perturbations in the Weyl scalars ${\psi }_0$ and ${\psi }_4$, with the governing equation being the well-known Teukolsky equation. Near infinity and near the horizon, ${\psi }_4$ is dominated by the component that corresponds to waves propagating towards the positive radial direction, while ${\psi }_0$ is dominated by the component that corresponds to waves that propagate towards the negative radial direction. Since gravitational-wave detectors measure outgoing waves at infinity, research has been mainly focused on ${\psi }_4$, leaving ${\psi }_0$ less studied. But the scenario is reversed in the near horizon region where the ingoing wave boundary condition needs to be imposed. For ingoing waves, the components of the tidal tensor measured by observers near the future horizon depend mainly on ${\psi }_0$. Thus, studying the near horizon phenomena, e.g., tidal heating and gravitational-wave echoes from extremely compact objects (ECOs), requires computing ${\psi }_0$. In this work, we explicitly calculate the source term for the ${\psi }_0$ Teukolsky equation due to a point particle plunging into a Kerr black hole. We highlight the need to regularize the solution of the ${\psi }_0$ Teukolsky equation obtained using the usual Green’s function techniques. We suggest a regularization scheme for this purpose and go on to compute the ${\psi }_0$ waveform close to a Schwarzschild horizon for two types of trajectories of the in-falling particle. We compare the ${\psi }_0$ waveform calculated directly from the Teukolsky equation with the ${\psi }_0$ waveform obtained by using the Starobinsky-Teukolsky identity on ${\psi }_4$. We also compute the first outgoing gravitational-wave echo waveform near infinity, using the near-horizon ${\psi }_0$ computed directly from the Teukolsky equation, and the Boltzmann boundary condition on the ECO surface. We show that this outgoing echo is quantitatively very different (stronger) than the echo obtained using previous prescriptions that did not compute the near-horizon ${\psi }_0$ directly using the Teukolsky equation.

We present numerical waveforms of gravitational-wave echoes from spinning exotic compact objects (ECOs) that result from binary black hole coalescence. We obtain these echoes by solving the Teukolsky equation for the ${\psi }_4$ associated with gravitational waves that propagate toward the horizon of a Kerr spacetime, and process the subsequent reflections of the horizon-going wave by the surface of the ECO, which lies right above the Kerr horizon. The trajectories of the infalling objects are modified from Kerr geodesics, such that the gravitational waves propagating toward future null infinity match those from merging black holes with comparable masses. In this way, the corresponding echoes can be used to approximate to those from nonspinning comparable-mass mergers. For boundary conditions at the ECO surface, we adopt recent work using the membrane paradigm, which relates ${\psi }_0$ associated with the horizon-going wave and ${\psi }_4$ of the wave that leaves the ECO surface. We obtain ${\psi }_0$ of the horizon-going wave from ${\psi }_4$ using the Teukolsky-Starobinsky relation. The echoes we obtain turn out to be significantly weaker than those from previous studies that generate echo waveforms by modeling the ringdown part of binary black hole coalescence waveforms as originating from the past horizon.

We explore the performance of an updated effective one-body (EOB) model for spin-aligned coalescing black hole binaries designed to deal with any orbital configuration. The model stems from previous work involving the TEOBResumS waveform model, but incorporates recently computed analytical information up to fifth post-Newtonian (PN) order in the EOB potentials. The dynamics is then informed by numerical relativity (NR) quasicircular simulations (incorporating also recently computed 4PN spin-spin and, optionally, 4.5PN spin-orbit terms). The so-constructed model(s) are then compared to various kind of NR simulations, covering either quasicircular inspirals, eccentric inspirals and scattering configurations. For quasicircular (534 datasets) and eccentric (28 datasets) inspirals up to coalescence, the EOB/NR unfaithfulness is well below 1% except for a few outliers in the high, positive, spin corner of the parameter space, where however it does not exceed the 3% level. The EOB values of the scattering angle are found to agree ($\lesssim 1\%$) with the NR predictions for most configurations, with the largest disagreement of only $\sim 4\%$ for the most relativistic one. The inclusion of some high-order analytical information in the orbital sector is useful to improve the EOB/NR agreement with respect to previous work, although the use of NR-informed functions is still crucial to accurately describe the strong-field dynamics and waveform.

In this paper, we first analyze the horizon structure of the acoustic charged black hole in curved spacetime and then study its acoustic shadow as well as the near-horizon characteristics including the quasinormal mode (QNM) frequencies and analog Hawking radiation. We find that the radius of the acoustic shadow for an acoustic charged black hole is larger than that for a Reissner-Nordström (RN) black hole, and both of them are suppressed by increasing the black hole charge because their related outer horizons become smaller. Then the QNM frequencies under scalar field perturbation and its eikonal limit are computed via numeric method and acoustic shadow, respectively. We find that the acoustic charged black hole is stable under the perturbation and the QNM frequencies are much weaker than that for the astrophysical black hole. Moreover, as the tuning parameter increases, the perturbation oscillates more mildly and its damping time becomes longer, while as the charge increases, the oscillation is enhanced slightly and the perturbation decays a little faster which is different from that in a RN black hole. Finally, we numerically study the analog Hawking radiation. We find that the gray-body factor and energy emission rate are suppressed by the angular number and the charge, but they do not monotonically depend on the tuning parameter in the acoustic charged black hole. The behavior of the energy emission rate affected by the parameters could be explained by the dependent behavior of the Hawking temperature. We expect that our results could shed light to the study of black holes in both theoretical and experimental perspectives.

Nonspherical rapid acceleration of mass (or energy) to a relativistic velocity is a natural source of gravitational radiation. Such conditions arise in both long and short gamma-ray bursts whose central engine ejects relativistic jets. The resulting gravitational wave signal is of a memory type, rising to a finite level (of order $4G\mathcal{E}/r$) over a duration that corresponds to the longer of either the injection time or the acceleration time of the jet. We explore the properties of such signals and their potential detectability. Unfortunately, the expected signals are below the frequency band of Advanced LIGO-Virgo-Kagra and above LISA. However, they fall within the range of the planned BBO and DECIGO. While current sensitivity is marginal for the detection of jet gravitational wave signals from gamma-ray bursts, hidden relativistic jets that exist within some core collapse supernove could be detected. Such a detection would reveal the acceleration mechanism and the activity of the central engine, which cannot be explored directly in any other way.

Light axionlike particles (ALPs) are expected to be abundantly produced in core-collapse supernovae (CCSNe), resulting in a $\sim 10$-second long burst of ALPs. These particles subsequently undergo conversion into gamma rays in external magnetic fields to produce a long gamma-ray burst (GRB) with a characteristic spectrum peaking in the 30–100-MeV energy range. At the same time, CCSNe are invoked as progenitors of ordinary long GRBs, rendering it relevant to conduct a comprehensive search for ALP spectral signatures using the observations of long GRBs with the Fermi Large Area Telescope (LAT). We perform a data-driven sensitivity analysis to determine CCSN distances for which a detection of an ALP signal is possible with the LAT’s low-energy technique which, in contrast to the standard LAT analysis, allows for a a larger effective area for energies down to 30 MeV. Assuming an ALP mass $m_a\lesssim {10}^{-10}\mathrm{eV}$ and ALP-photon coupling $g_{a\gamma }=5.3\times {10}^{-12}{\mathrm{GeV}}^{-1}$, values considered and deduced in ALP searches from SN1987A, we find that the distance limit ranges from $\sim 0.5$ to $\sim 10\mathrm{Mpc}$, depending on the sky location and the CCSN progenitor mass. Furthermore, we select a candidate sample of 24 GRBs and carry out a model comparison analysis in which we consider different GRB spectral models with and without an ALP signal component. We find that the inclusion of an ALP contribution does not result in any statistically significant improvement of the fits to the data. We discuss the statistical method used in our analysis and the underlying physical assumptions, the feasibility of setting upper limits on the ALP-photon coupling, and give an outlook on future telescopes in the context of ALP searches.

Recently, the importance of the electronic many-body effect in the dark matter (DM) detection has been recognized, and a coherent formulation of the DM-electron scattering in terms of the dielectric response of the target material has been well established in literatures. In this paper, we put relevant formulas into practical density functional theory (DFT) estimation of the excitation event rates for the diamond and silicon semiconductor targets. Moreover, we compare the event rates calculated from the energy loss functions with and without the local field effects. For a consistency check of this numerical method, we also compare the differential spectrum and detection reach of the silicon target with those computed with the $\mathtt{GPAW}$ code. It turns out that these DFT approaches are quite consistent and robust. As an interesting extension, we also investigate the in-medium effect on the detection of the solar-reflected DM flux in silicon-based detectors, where the screening effect is found to be less remarkable than on detection of the Galactic DM, due to the high energies of the reflected DM particles.

The $e^{+}{e}^{-}\to \gamma {\chi }_{cJ}$ ($J=0$, 1, 2) processes are studied at center-of-mass energies ranging from 3.773 to 4.600 GeV, using a total integrated luminosity of $19.3{\mathrm{fb}}^{-1}$ $e^{+}{e}^{-}$ annihilation data accumulated with the BESIII detector at BEPCII. We observe for the first time $e^{+}{e}^{-}\to \gamma {\chi }_{c1,c2}$ signals at $\sqrt{s}=4.180\mathrm{GeV}$ with statistical significances of $7.6\sigma$ and $6.0\sigma$, respectively. The production cross section of $e^{+}{e}^{-}\to \gamma {\chi }_{c1,c2}$ at each center-of-mass energy is also measured. We find that the line shape of the $e^{+}{e}^{-}\to \gamma {\chi }_{c1}$ cross section can be described with conventional charmonium states $\psi (3686)$, $\psi (3770)$, $\psi (4040)$, $\psi (4160)$. Compared with this, for the $e^{+}{e}^{-}\to \gamma {\chi }_{c2}$ channel, one more additional resonance is added to describe the cross section line shape. Its mass and width are measured to be $M=4371.7\pm 7.5\pm 1.8\mathrm{MeV}/c^2$ and ${\mathrm{\Gamma }}^{\mathrm{tot}}=51.1\pm 17.6\pm 1.9\mathrm{MeV}$, where the first uncertainties are statistical and the second systematic. The significance of this resonance is estimated to be $5.8\sigma$, and its parameters agree with the $Y(4360)$ resonance previously reported in $e^{+}{e}^{-}\to {\pi }^{+}{\pi }^{-}\psi (3686)$, and the $Y(4390)$ in $e^{+}{e}^{-}\to {\pi }^{+}{\pi }^{-}{h}_c$ within uncertainties. No significant signal for the $e^{+}{e}^{-}\to \gamma {\chi }_{c0}$ process is observed, and the upper limits of Born cross sections ${\sigma }_B(e^{+}{e}^{-}\to \gamma {\chi }_{c0})$ at 90% confidence level are reported.

Advances in upcoming weak lensing surveys pose new challenges for an accurate modeling of the lensing observables. The wide sky coverage of Euclid makes angular scales down to $l_{\min }=10$ accessible. At such large angular scales, general relativistic effects manifest themselves, and the lensing magnification cannot be correctly described by the standard lensing convergence only. The impact of line-of-sight velocities on the magnification angular power spectrum, referred to as the Doppler magnification, is already well recognized in literature. In particular, it was suggested that the Doppler magnification could be extracted by measurements of both cosmic shear and magnification. In this work, we point out two previously neglected aspects with respect to this method. First, the impact of the Doppler magnification is reduced through nonvanishing cross terms with the standard lensing convergence. This is particularly relevant when the sources are averaged over a bin of width $\mathrm{\Delta }z\approx 0.1$, such as in Euclid’s tomographic weak lensing survey. Second, general relativistic potential terms slightly enhance the signal. We present numerical calculations of all relativistic effects in the weak lensing angular power spectra on large scales.