Within the basis light-front quantization framework, we compute the masses and light-front wave functions of the ${\mathrm{\Lambda }}_b$ baryon and its isospin triplet counterparts ${\mathrm{\Sigma }}_b^{+}$, ${\mathrm{\Sigma }}_b^0$, and ${\mathrm{\Sigma }}_b^{-}$ using a light-front effective Hamiltonian in the leading Fock sector. These wave functions are obtained as eigenstates of the effective Hamiltonian, which incorporates the one-gluon exchange interaction with fixed coupling and a three-dimensional confinement potential. With the quark masses and the couplings as adjustable parameters, the computed masses are set within the experimental range. The resulting predictions for their electromagnetic properties align well with other theoretical calculations. Additionally, the parton distribution functions (PDFs) of these baryons are obtained for the first time, with gluon and sea quark distributions dynamically generated through QCD evolution of the valence quark PDFs.

We have studied the deep inelastic scattering (DIS) of polarized charged leptons from polarized nucleon targets and evaluated the polarized nucleon structure functions $g_{1N,2N}(x,Q^2)$, as well as the nucleon asymmetries $A_{1N,2N}(x,Q^2)$ for protons and neutrons. The higher-order perturbative corrections up to the next-to-next-to-leading order (NNLO), using the parametrization of polarized parton distribution functions (PPDFs) given by Borsa, Stratmann, Vogelsang, de Florian, and Sassot (BDSSV24) in the three-flavor $\overline{\mathrm{MS}}$ scheme, along with the nonperturbative corrections—namely, the twist-3 corrections and the target mass corrections (TMCs)—have been included in the calculations. The numerical results for the polarized nucleon structure functions, the nucleon asymmetries, and the sum rule integrals of the nucleon structure functions—corresponding to the Ellis-Jaffe, Bjorken, and Burkhardt-Cottingham sum rules—have been evaluated numerically and are found to be in agreement with the experimental results from SLAC, CERN, DESY, and JLab. The benchmarking of the PPDFs of BDSSV24 at NNLO using the present data on polarized nucleon structure functions and other observables will be useful in studying the nuclear medium effects in the scattering of the charged leptons from nuclei at JLab, EIC, DESY, etc., and the scattering of the (anti)neutrinos from polarized nucleons and nuclei at the proposed neutrino factories.

The Cabibbo-favored hadronic weak decay of the ${\mathrm{\Xi }}_c^{+}\to {\mathrm{\Xi }}^0{\pi }^{+}$, ${\mathrm{\Xi }}_c^0\to {\mathrm{\Xi }}^{-}{\pi }^{+}$, ${\mathrm{\Xi }}_c^0\to {\mathrm{\Xi }}^0{\pi }^0$, ${\mathrm{\Xi }}_c^0\to {\mathrm{\Xi }}^0{\eta }^{{(}^{\prime })}$, and ${\mathrm{\Xi }}_c^0\to {\mathrm{\Xi }}^{+}{K}^{-}$ are studied in the nonrelativistic constituent quark model. By analyzing their decay mechanisms at the quark level we show that the pole terms are essential for understanding the transition dynamics in addition to the usually considered direct meson emission process and color suppressed process in the charmed baryon hadronic weak decays. The experimentally measurable asymmetry parameters are also predicted in order to further pin down the decay mechanism.

Using a dataset of $(27.12\pm 0.14)\times {10}^8\psi (3686)$ events collected by the BESIII detector operating at the BEPCII collider, we report the first observation of the decay $\psi (3686)\to {\mathrm{\Sigma }}^0{\overline{\mathrm{\Sigma }}}^0\omega$ with a statistical significance of $8.9\sigma$. The measured branching fraction is $(1.24\pm 0.16_{\mathrm{stat}}\pm 0.11_{\mathrm{sys}})\times {10}^{-5}$, where the first uncertainty is statistical and the second is systematic. Additionally, we investigate potential intermediate states in the invariant mass distributions of ${\mathrm{\Sigma }}^0\omega$, ${\overline{\mathrm{\Sigma }}}^0\omega$ and ${\mathrm{\Sigma }}^0{\overline{\mathrm{\Sigma }}}^0$. A hint of a resonance is observed in the invariant mass distribution of $M_{{\mathrm{\Sigma }}^0({\overline{\mathrm{\Sigma }}}^0)\omega }$, located around $2.06\mathrm{GeV}/c^2$, with a significance of $2.5\sigma$.

The determination of the direction of a stellar core collapse via its neutrino emission is crucial for the identification of the progenitor for a multimessenger follow-up. A highly effective method of reconstructing supernova directions within the Deep Underground Neutrino Experiment (DUNE) is introduced. The supernova neutrino pointing resolution is studied by simulating and reconstructing electron-neutrino charged-current absorption on ${}^{40}\mathrm{Ar}$ and elastic scattering of neutrinos on electrons. Procedures to reconstruct individual interactions, including a newly developed technique called “brems flipping,” as well as the burst direction from an ensemble of interactions are described. Performance of the burst direction reconstruction is evaluated for supernovae happening at a distance of 10 kpc for a specific supernova burst flux model. The pointing resolution is found to be 3.4 degrees at 68% coverage for a perfect interaction-channel classification and a fiducial mass of 40 kton, and 6.6 degrees for a 10 kton fiducial mass respectively. Assuming a 4% rate of charged-current interactions being misidentified as elastic scattering, DUNE’s burst pointing resolution is found to be 4.3 degrees (8.7 degrees) at 68% coverage.

Using $20.3{\mathrm{fb}}^{-1}$ of $e^{+}{e}^{-}$ collision data collected at a center-of-mass energy of 3.773 GeV with the BESIII detector operating at the BEPCII collider, the branching fractions of three hadronic charm meson decays, $D^{+}\to \varphi {\pi }^{+}{\pi }^{+}{\pi }^{-}$, $D^{+}\to K_S^0{K}^{+}{\pi }^{+}{\pi }^{-}{\pi }^0$, and $D^{+}\to K_S^0{K}^{+}\omega$, are measured for the first time to be $(0.54\pm 0.19\pm 0.02)\times {10}^{-4}$, $(2.51\pm 0.34\pm 0.14)\times {10}^{-4}$, and $(2.02\pm 0.35\pm 0.10)\times {10}^{-4}$, respectively. Futhermore, the branching fractions of $D^{+}\to K^{+}{K}^{-}{\pi }^{+}{\pi }^{+}{\pi }^{-}$ and $D^{+}\to K_S^0{K}^{+}\eta$ are measured with improved precision, yielding values of $(0.66\pm 0.11\pm 0.03)\times {10}^{-4}$ and $(2.27\pm 0.22\pm 0.05)\times {10}^{-4}$, respectively.

We exhibit an exclusive process, namely the photoproduction of a ${\pi }^0\gamma$ pair with large invariant mass, which violates collinear factorization. We explicitly demonstrate that this is due to the fact that there exists diagrams with gluon exchange in $t$ channel, contributing at the leading power, for which Glauber gluons are trapped. This is caused by the pinching of the contour integration of both the plus and minus light-cone components of the Glauber gluon momentum. We argue that this leads to the observed “end pointlike” divergence of the convolution integral at leading order and leading power when collinear factorization is naïvely assumed.

We study holographic subregion complexity in a moving strongly coupled plasma in dimensions $d=2$, 3, 4, which is holographically dual to a boosted black brane metric in a higher dimensional geometry. The proposal we employ is the one that identifies the complexity of a mixed state by the volume of codimensional-one hypersurface enclosed by Hubeny-Rangamani-Takayanagi surface. Using the finite difference method, the numerical calculations reveal that temperature, velocity, and subregion length all have an increasing effect on holographic subregion complexity. For arbitrary values of temperature and subregion length, as velocity approaches its relativistic upper limit, holographic subregion complexity exhibits a divergence. This divergence behavior observed in $d=2$, 3, 4 seems to demonstrate a universal behavior and is characterized by the Lorentz factor squared, ${\gamma }^2$.

We consider a class of two dimensional conformal $\mathcal{N}=2$ supersymmetric $U(1)$ gauge linear sigma models with $N$ fields of charges $+1$ and $N$ fields of charges $-1$, whose Higgs branches are noncompact toric Calabi-Yau manifolds of complex dimension $2N-1$. We show, starting from large-$N$ approximation, that the Coulomb branch of these models, which opens up at strong coupling, is described by $\mathcal{N}=2$ Liouville theory and then extrapolate it to exact equivalence demanding the central charge of the Liouville theory to be $\widehat{c}=2N-1$. Next, we concentrate on mostly physically attractive $N=2$ and $N\ge 3$ cases and find there a perfect agreement of the set of complex moduli on the Calabi-Yau side with the marginal deformations in $\mathcal{N}=2$ Liouville theory, supporting proposed exact equivalence.

Particle production in cosmology is often efficiently computed in terms of Bogoliubov transforms. Restricting to a particular class of dispersion relationships, we identify a map between the number of particles produced in a special kinematic limit and a Stokes phenomena related topology of analytic continuation of the Bogoliubov coefficient functions. Intuitively, this kinematic limit corresponds to the long wavelength limit although a more precise description depends on the nature of the curved spacetime. To identify the topology, we reformulate the usual Bogoliubov computations as a type of SU(1, 1) gauged differential equation and utilize a special gauge together with a discrete symmetry that naturally characterizes the dispersion relationship. Using a dark matter model and a nonzero constant spatial curvature model, we estimate how such topological contributions will arise in physical applications.

We show that the moduli space metric of a single vortex gets corrections because of the excitation of the radially symmetric shape mode. It leads to a nonzero amount of the shape mode carried by the vortex when moving with a constant velocity. However, due to the radial symmetry, this effect does not reproduce the Lorentz contraction of the moving vortex. We apply the Derrick mode approximation in order to recover the Lorentz contraction on the level of the collective model.

We present a new perturbative/nonperturbative (P/NP) relation that applies to a broader class of genus-1 potentials, including those that possess real and complex instantons parametrized by a deformation parameter, such as polynomial and elliptic potentials. Our findings significantly extend the scope of quantum mechanical systems for which perturbation theory suffices to calculate the contributions of nonperturbative effects to energy levels, with or without the need for a boundary condition, depending on the potential. We further provide evidence for our results by predicting the corrections to the large-order behavior of the perturbative expansion for the Jacobi SD elliptic potential using the early terms of the instanton fluctuations that satisfy the P/NP relation.

We study the application of the background field method in the framework of the exact renormalization group (ERG). By considering the case of a scalar field theory, we provide a detailed discussion of the properties satisfied by a background dependent Wilson action. We show how the Ward identity associated with background field shifts for the Wilson action is related to that for the 1PI Wilson action, or effective average action. Moreover, we discuss the ERG equations in the dimensionless framework and emphasize the role of the Ward identity in this setting. We give two examples: the Gaussian fixed point for the real scalar theory and the large $N$ limit of the linear sigma model.

Recently, the “bootstrap” technique was applied in quantum mechanics to solve the eigenspectra of Hermitian Hamiltonians and extended to non-Hermitian parity-time (PT)-symmetric systems. However, its application has been limited to real spectra. In this work, we establish bootstrap conditions for the non-Hermitian system and generate eigenspectra for a generic complex polynomial potential, which includes PT-symmetric Hamiltonians as a special case. Additionally, we demonstrate the method’s ability to obtain eigenspectra under various boundary conditions imposed on the eigenfunction, including the notable application of capturing the PT-symmetric phase transition.

Strong-field gravity simulators are laboratory experiments that can investigate a wide range of both classical and quantum phenomena occurring in nature. In this work, we introduce an effective geometry that captures most of the characteristics of the strong-field regime of astrophysical, rotating black holes. This geometry can represent a vortex made from a variety of fluid and superfluid profiles with zero viscosity, making it a promising finite-temperature quantum-field-theory simulator for rotating curved spacetimes. Our geometry includes not only the typical radial flow which gives rise to an acoustic horizon, but also azimuthal circulation of the fluid. We compute the quasinormal modes, semianalytically, and the exact quasibound states of acoustic excitations interacting with this effective geometry. The resulting spectra can be identified for both corotating and counterrotating surface acoustic waves. In particular, the behavior of our acoustic geometry with circulation aligns with the phenomenology observed in recent experiments that include superfluids.

We prove the uniqueness theorem for static spherically symmetric traversable wormholes with two asymptotically flat ends constituting the solutions of the Einstein-phantom-electric-magnetic equations of motion. For the completeness of the results, we also consider the case of the phantom $U(1)$-gauge field. The key role in the proof is bounded with the conformal positive energy theorem.

The standard cosmological model, rooted in general relativity (GR), has achieved remarkable success, yet it still faces unresolved issues like the nature of dark matter, dark energy, and the Hubble tension. These challenges might imply the need for alternative gravitational theories. Teleparallel gravity offers a compelling framework by reformulating the gravitational interaction using torsion, rather than curvature, as its fundamental geometrical property. This paper delves into $f(T)$ gravity, an extension of the teleparallel equivalent of general relativity (TEGR), which introduces nonlinear modifications of the torsion scalar $T$. We focus on the role of spacetime-dependent Lorentz transformations in the vierbein formalism, examining their impact on both background solutions and perturbation dynamics. Special attention is given to the homogeneous and isotropic Friedmann-Lemaître-Robertson-Walker (FLRW) spacetime, as well as the anisotropic Bianchi I spacetime. Furthermore, the analysis of the propagating degrees of freedom on these spacetimes is performed. While it is well established that TEGR reproduces the same results as GR, the propagating degrees of freedom in its nonlinear extension, $f(T)$ gravity, is still debated in the literature. In this work, we find that only two fields propagate in the gravity sector, independent of the background spacetime considered, either FLRW or Bianchi I. Although not definitive, this paper provides fresh insights into the issue of the propagating degrees of freedom in $f(T)$ gravity, opening the door to intriguing new directions for further investigation.

It is commonly assumed that low-mass primordial black holes cannot constitute a significant fraction of the dark matter in our universe due to their predicted short lifetimes from the conventional Hawking radiation and evaporation process. Assuming physical black holes are nonsingular—likely due to quantum gravity or other high-energy physics—we demonstrate that a large class of nonsingular black holes have finite evaporation temperatures. This can lead to slowly evaporating low-mass black holes or to remnant mass states that circumvent traditional evaporation constraints. As a proof of concept, we explore the limiting curvature hypothesis and the evaporation process of a nonsingular black hole solution in two-dimensional dilaton gravity. We identify generic features of the radiation profile and compare them with known regular black holes, such as the Bardeen solution in four dimensions. Remnant masses are proportional to the fundamental length scale, and we argue that slowly evaporating low-mass nonsingular black holes, or remnants, are viable dark matter candidates.

Predicting the flavor composition of neutrinos from supernovae is a challenging task, primarily due to the high neutrino densities at their core. In such an environment, neutrino self-interactions give rise to collective effects that have dramatic yet poorly understood consequences for their flavor evolution. In this paper, however, we show that standard matter effects in the outer layers of supernovae can significantly constrain the flavor composition of the neutrino flux. We assume that, since a large number of neutrinos undergo different evolutions within the core, their state upon entering the Mikheyev–Smirnov–Wolfenstein-dominated region is affected by decoherence. This assumption simplifies the problem and suggests that the fraction of neutrinos with electron flavor reaching Earth, denoted as $f_{{\nu }_e}$, is constrained to be less than 0.5 for all energies throughout the emission phase in the case of normal mass ordering. In contrast, for inverted mass ordering, we anticipate neutrinos arriving in near flavor equipartition ($f_{{\nu }_e}\approx 1/3$). These predictions, and consequently their underlying assumptions, could be tested by future observations and may provide valuable insights into the properties of neutrino fluxes emerging from supernovae.

The direct observation of intermediate-mass black holes (IMBH) populations would not only strengthen the possible evolutionary link between stellar and supermassive black holes, but unveil the details of the pair-instability mechanism and elucidate their influence in galaxy formation. Conclusive observation of IMBHs remained elusive until the detection of gravitational-wave (GW) signal GW190521, which lies with high confidence in the mass gap predicted by the pair-instability mechanism. Despite falling in the sensitivity band of current GW detectors, IMBH searches are challenging due to their similarity to transient bursts of detector noise, known as glitches. In this proof-of-concept work, we combine a matched-filter algorithm with a machine learning (ML) method to differentiate IMBH signals from nontransient burst noise, known as glitches. In particular, we build a multilayer perceptron network to perform a multiclass classification of the output triggers of matched filter. In this way we are able to distinguish simulated GW IMBH signals from different classes of glitches that occurred during the third observing run (O3) in single detector data. We train, validate, and test our model on O3a data, reaching a true positive rate of over 90% for simulated IMBH signals. To test the generalization ability over the evolutionary observing run, we test on the unseen data of O3b, which yields a true positive rate of over 70%. We also combine data from multiple detectors to search for simulated IMBH signals in real detector noise, providing a significance measure for the output of our ML method.