Based on a 14-moment closure for nonresistive (general-) relativistic viscous plasmas, we describe a new numerical scheme that is able to handle all first-order dissipative effects (heat conduction, bulk and shear viscosities), as well the anisotropies induced by the presence of magnetic fields. The latter is parametrized in terms of a thermal gyrofrequency or, equivalently, a thermal Larmor radius and allows to correctly capture the thermal Hall effect. By solving an extended Israel-Stewart-like system for the dissipative quantities that enforces algebraic constraints via stiff-relaxation, we are able to cast all first-order dissipative terms in flux-divergence form. This allows us to apply traditional high-resolution shock capturing methods to the equations, making the system suitable for the numerical study of highly turbulent flows. We present several numerical tests to assess the robustness of our numerical scheme in flat spacetime. The 14-moment closure can seamlessly interpolate between the highly collisional limit found in neutron star mergers, and the highly anisotropic limit of relativistic Braginskii magnetohydrodynamics appropriate for weakly collisional plasmas in black-hole accretion problems. We believe that this new formulation and numerical scheme will be useful for a broad class of relativistic magnetized flows.

As the sensitivity and observing time of gravitational-wave detectors increase, a more diverse range of signals is expected to be observed from a variety of sources. Especially, long-lived gravitational-wave transients have received interest in the last decade. Because most long-duration signals are poorly modeled, detection must rely on generic search algorithms, which make few or no assumptions on the nature of the signal. However, the computational cost of those searches remains a limiting factor, which leads to suboptimal sensitivity. Several detection algorithms have been developed to cope with this issue. In this paper, we present a new data analysis pipeline to search for unmodeled long-lived transient gravitational-wave signals with duration between 10 and ${10}^3\mathrm{s}$, based on an excess cross-power statistic in a network of detectors. The pipeline implements several new features that are intended to reduce computational cost and increase detection sensitivity for a wide range of signal morphologies. The method is generalized to a network of an arbitrary number of detectors and aims to provide a stable interface for further improvements. Comparisons with a previous implementation of a similar method on simulated and real gravitational-wave data show an overall increase in detection efficiency for all but one signal morphologies tested and a computing time reduced by at least a factor 10.

We perform a global analysis of three-body charmless hadronic decays $B\to V{P}_3\to P_1{P}_2{P}_3$ in the perturbative QCD (PQCD) approach, where $V$ denotes an intermediate vector resonance, and $P_i$, $i=1$, 2, 3 denote final-state pseudoscalar mesons. Fitting the PQCD factorization formulas at leading order in the strong coupling ${\alpha }_s$ to measured branching ratios and direct $CP$ asymmetries, we determine the Gegenbauer moments in the two-meson distribution amplitudes (DAs) for the meson pairs $P_1{P}_2=\pi \pi ,K\pi ,KK$. The fitted Gegenbauer moments are then employed to make predictions for those observables, whose data are excluded in the fit due to larger experimental uncertainties. A general consistency between our predictions and data is achieved, which hints at the validity of the PQCD formalism for the above three-body $B$-meson decays and the universality of the nonperturbative two-meson DAs. The obtained two-meson DAs can be applied to PQCD studies of other multi-body $B$-meson decays involving the same meson pairs. We also attempt to determine the dependence of the Gegenbauer moments on the meson-pair invariant mass, and demonstrate that this determination is promising, when data become more precise.

We study an inevitable cosmological consequence in PeV-scale SUSY-breaking scenarios. We focus on the SUSY-breaking scale corresponding to the gravitino mass $m_{3/2}=100\mathrm{eV}–1\mathrm{keV}$. We argue that the presence of an early matter-dominated era and the resulting entropy production are requisite for the Universe with this gravitino mass. We infer the model-independent minimum amount of the entropy production $\mathrm{\Delta }$ by requiring that the number of dwarf satellite galaxies $N_{\mathrm{sat}}$ in the Milky Way exceed the currently observed value, i.e., $N_{\mathrm{sat}}\gtrsim 63$. This entropy production is inevitably imprinted on the primordial gravitational waves (PGWs) produced during the inflationary era. We study how the information on the value of $\mathrm{\Delta }$ and the time of entropy production are encoded in the PGW spectrum ${\mathrm{\Omega }}_{\mathrm{GW}}$. If the future GW surveys observe a suppression feature in the PGW spectrum for the frequency range $\mathcal{O}({10}^{-10})\mathrm{Hz}\lesssim f_{\mathrm{GW}}\lesssim \mathcal{O}({10}^{-5})\mathrm{Hz}$, it works as a smoking gun for PeV SUSY-breaking scenarios. Even if they do not, our study can be used to rule out all such scenarios.

The observation of coherent elastic neutrino-nucleus scattering ($\mathrm{CE}\nu \mathrm{NS}$) provides us opportunities to explore a wide class of new physics. In the Standard Model (SM), the $\mathrm{CE}\nu \mathrm{NS}$ process arises from the vector and axial-vector neutral currents through the exchange of $Z$ bosons, and the axial-vector current contribution turns out to be subdominant. It is, thus, natural to consider the extra contributions to $\mathrm{CE}\nu \mathrm{NS}$ from more generic new physics beyond the SM with (axial-)vector interactions associated with a new vector mediator $Z^{\prime }$. Besides ordinary $\mathrm{CE}\nu \mathrm{NS}$, the active neutrinos can convert into a new exotic fermion $\chi$ through the process $\nu N\to \chi N$ mediated by $Z^{\prime }$ without violating coherence. It would be interesting to consider the implication of this conversion for the new fermion sector beyond the SM. We consider the framework of a simplified neutrino model in which a new Dirac fermion $\chi$ interacts with active neutrinos and a leptophobic vector mediator $Z^{\prime }$. We evaluate both the tree-level and loop-level contributions to $\mathrm{CE}\nu \mathrm{NS}$, and, in particular, the loop diagrams produce active neutrino elastic scattering process $\nu N\to \nu N$ with the fermion $\chi$ inside the loops. When the interaction between $Z^{\prime }$ and the SM quarks is vector type and axial-vector type, the $\mathrm{CE}\nu \mathrm{NS}$ processes are, respectively, dominated by the tree-level and loop-level contributions. We investigate the constraints on the model parameters by fitting to the COHERENT data, assuming a wide range of $m_{\chi }$. The parameter space with $m_{\chi }$ larger than the maximal energy of incoming neutrinos can be constrained by including the loop-level contribution. More importantly, the inclusion of loop diagrams can place a constraint on axial-vector interaction whose tree-level process is absent in the coherent neutrino-nucleus scattering.

We propose a factorized approach to QED radiative corrections for inclusive and semi-inclusive deep-inelastic scattering to systematically account for QED and QCD radiation contributions to both processes on equal footing. This is achieved by utilizing factorization to resum logarithmically enhanced QED radiation into universal lepton distribution and fragmentation (or jet) functions. Numerical simulations suggest that the QED effects induced by the rotational distortion of the hadron transverse momentum, arising from the mismatch between the experimental Breit frame and the true photon-hadron frame, can be as large as 50% for moderate $Q$, and become increasingly important for large transverse momenta. Our framework provides a uniform treatment of radiative effects for extracting three-dimensional hadron structure from high-energy lepton-hadron scattering at current and future facilities, such as the Electron-Ion Collider.

Motivated by the recent discovery of the first hidden charm pentaquark state with strangeness $P_{cs}(4459)$ by the LHCb Collaboration, we study the likely existence of a three-body ${\mathrm{\Sigma }}_c\overline{D}\overline{K}$ bound state, which shares the same minimal quark content as $P_{cs}(4459)$. The ${\mathrm{\Sigma }}_c\overline{D}$ and $DK$ interactions are determined by reproducing $P_c(4312)$ and $D_{s0}^{*}(2317)$ as ${\mathrm{\Sigma }}_c\overline{D}$ and $\overline{D}\overline{K}$ molecules, respectively, while the ${\mathrm{\Sigma }}_c\overline{K}$ interaction is constrained by chiral effective theory. We indeed find a three-body bound state by solving the Schrödinger equation using the Gaussian expansion method, which can be viewed as an excited hidden charm exotic state with strangeness, $P_{cs}^{*}(4739)$, with $I(J^P)=1(1/2^{+})$ and a binding energy of ${77.8}_{-10.3}^{+25}\mathrm{MeV}$. We further study its strong decays via triangle diagrams and show that its partial decay widths into $D{\mathrm{\Xi }}_c^{\prime }$ and $D_s^{*}{\mathrm{\Sigma }}_c$ are of a few tens of MeV, with the former being dominant.

In this work we present the results from numerical simulations of an interacting ensemble of instanton dyons in the $SU(3)$ gauge group with $N_f=2$ flavors of massless quarks. Dynamical quarks are included via the effective interactions induced by the fermionic determinant evaluated in the subspace of topological zero modes. The eigenvalue spectrum of the Dirac operator is studied at different volumes to extract the chiral condensate and eigenvalue gap, with both observables providing consistent values of the chiral transition temperature $T_c$. We find that a sufficient density of dyons is responsible for generating the confining potential and breaking the chiral symmetry, both of which are compatible with second-order transitions.

Stimulated by the newly reported doubly charmed tetraquark state $T_{cc}^{+}$ by LHCb, we carry out a systematic investigation of the $S$-wave interactions between the charmed meson ($D$, $D^{*}$) in $H$-doublets and the charmed meson ($D_1$, $D_2^{*}$) in $T$-doublets by adopting the one-boson exchange model. Both the $S$-$D$ wave mixing effect and the coupled channel effect are taken into account. By performing a quantitative calculation, we suggest that the $S$-wave $D^{*}{D}_1$ states with $I(J^P)=0(0^{-},1^{-})$ and the $S$-wave $D^{*}{D}_2^{*}$ states with $I(J^P)=0(1^{-},2^{-})$ should be viewed as the most promising candidates of the doubly charmed molecular tetraquark states, and the $S$-wave $D{D}_1$ state with $I(J^P)=0(1^{-})$ and the $S$-wave $D{D}_2^{*}$ state with $I(J^P)=0(2^{-})$ are the possible doubly charmed molecular tetraquark candidates. With the accumulation of experimental data at Run III and after a High-Luminosity LHC upgrade, these predicted doubly charmed molecular tetraquark states can be accessible at LHCb in the near future.

MINERvA presents a new analysis of inclusive charged-current neutrino interactions on a hydrocarbon target. We report single and double-differential cross sections in muon transverse and longitudinal momentum. These measurements are compared to neutrino interaction generator predictions from GENIE, NuWro, GiBUU, and NEUT. In addition, comparisons against models with different treatments of multinucleon correlations, nuclear effects, resonant pion production, and deep inelastic scattering are presented. The data recorded corresponds to $10.61\times {10}^{20}$ protons on target with a peak neutrino energy of approximately 6 GeV. The higher energy and larger statistics of these data extend the kinematic range for model testing beyond previous MINERvA inclusive charged-current measurements. The results are not well modeled by several generator predictions using a variety of input models.

This paper aims at investigating the nonperturbative functional renormalization group for tensorial group field theories with nontrivial kinetic action and closure constraint. We consider the quartic melonic just-renormalizable $[U(1){]}^6$ model and show that due to this closure constraint the first order Ward-Takahashi identity takes the trivial form as for the models with propagators proportional to identity. We then construct the new version of the effective vertex expansion applicable to this class of models, which in particular allows us to close the hierarchical structure of the flow equations in the melonic sector. As a consequence, there are no additional constraints on the flow equations, and then we can focus on the existence of the physical Wilson-Fisher fixed-points in the symmetric phase.

We look for UV fixed points of non-Abelian $SU(n_c)$ gauge theories in $4+2\epsilon$ dimensions with $n_f$ Dirac fermions in the fundamental representation, using the available five-loop $\overline{\mathrm{MS}}$ $\beta$-function and employing Padé-Borel resummation techniques and Padé approximants to the series expansion in $\epsilon$. We find evidence for a five-dimensional UV fixed point for $SU(2)$ theories with $n_f\le 4$ and pure $SU(n_c)$ theories for $n_c\le 4$. We also compute the anomalous dimensions $\gamma$ and ${\gamma }_g$ of respectively the fermion mass bilinear and the gauge kinetic term operator at the UV fixed point.

We demonstrate that the positive frequency modes for a complex scalar field in constant electric field (Schwinger modes), in three different gauges, can be represented as exact Lorentzian worldline path integral amplitudes. Although the mathematical forms of the mode functions differ in each gauge, we show that a simple prescription for Lorentzian worldlines’ boundary conditions dispenses the Schwinger modes in all three gauges (that we considered) in a unified manner. Following that, using our formalism, we derive the exact Bogoliubov coefficients and, hence, the particle number, without appealing to the well-known connection formulas for parabolic cylinder functions. This result is especially relevant in view of the fact that in a general electromagnetic field configuration, one does not have the luxury of closed-form solutions. We argue that the real-time worldline path integral approach may be a promising alternative in such nontrivial cases. We also demonstrate, using Picard-Lefschetz theory, how the so-called worldline instantons emerge naturally from relevant saddle points that are complex.

In this study we present evolving wormhole configurations in third-order Lovelock gravity and investigate the possibility that these solutions satisfy the energy conditions. Using a generalized Friedmann-Robertson-Walker spacetime, we derive evolving wormhole geometries by considering a constraint on the Ricci scalar. In standard cosmological models, the Ricci scalar is independent of the radial coordinate $r$ and is only a function of time. We use this property to introduce dynamic wormhole solutions expanding in an inflationary cosmological background and explore the effects of higher-order Lovelock terms on the dynamics of such wormholes. Our analysis shows that for suitable third-order Lovelock coefficients, there are wormhole solutions that respect the weak energy condition (WEC). In addition to this, we also present other wormhole solutions that satisfy the WEC throughout their respective evolution.

Motivated by electromagnetic-field confinement due to plasma near accreting black holes, we continue our exploration of the linear dynamics of an electromagnetic field propagating in curved spacetime in the presence of plasma by including three effects that were neglected in our previous analysis: collisions in the plasma, thermal corrections, and the angular momentum of the background black hole spacetime. We show that: (i) the plasma-driven long-lived modes survive in a collisional plasma except when the collision timescale is unrealistically small; (ii) thermal effects, which might be relevant for accretion disks around black holes, do not affect the axial long-lived modes; (iii) in the case of a spinning black hole the plasma-driven modes become superradiantly unstable at the linear level; (iv) the polar sector in the small-frequency regime admits a reflection point due to the resonant properties of the plasma. Dissipative effects such as absorption, formation of plasma waves, and nonlinear dynamics play a crucial role in the vicinity of this resonant point.

We show that kinematics of charged particles allows us to model the growth of particles’ energy by consecutive particle splits, once a spherical mirror as a perfectly reflective boundary is placed outside a charged black hole. We consider a charged version of the Penrose process, in which a charged particle decays into two fragments, one of them has negative energy and the other has positive energy that is larger than that of the parent particle. The confinement system with the mirror makes the particles’ energy amplified each time a split of the parent particle occurs. Thus, the energy is a monotonically increasing function of time. However, the energy does not increase unboundedly, but rather asymptotes to a certain finite value, implying no instability of the system in this respect.

The Minkowski functionals are useful statistics to quantify the morphology of various random fields. They have been applied to numerous analyses of geometrical patterns, including various types of cosmic fields, morphological image processing, etc. In some cases, including cosmological applications, small deviations from the Gaussianity of the distribution are of fundamental importance. Analytic formulas for the expectation values of Minkowski functionals with small non-Gaussianity have been derived in limited cases to date. We generalize these previous works to derive an analytic expression for expectation values of Minkowski functionals up to second-order corrections of non-Gaussianity in a space of general dimensions. The derived formula has sufficient generality to be applied to any random fields with weak non-Gaussianity in a statistically homogeneous and isotropic space of any dimensions.

We present new observational constraints on the elastic scattering of dark matter with electrons for dark matter masses between 10 keV and 1 TeV. We consider scenarios in which the momentum-transfer cross section has a power-law dependence on the relative particle velocity, with a power-law index $n\in \{-4,-2,0,2,4,6\}$. We search for evidence of dark matter scattering through its suppression of structure formation. Measurements of the cosmic microwave background temperature, polarization, and lensing anisotropy from Planck 2018 data and of the Milky Way satellite abundance measurements from the Dark Energy Survey and Pan-STARRS1 show no evidence of interactions. We use these datasets to obtain upper limits on the scattering cross section, comparing them with exclusion bounds from electronic recoil data in direct detection experiments. Our results provide the strongest bounds available for dark matter–electron scattering derived from the distribution of matter in the Universe, extending down to sub-MeV dark matter masses, where current direct detection experiments lose sensitivity.

Scalar fields with an energy density dominated by its kinetic part may have played a relevant role in the very early stages of the Universe. Compared to the standard inflationary paradigm, they may lead to modifications in observable quantities, e.g., the anisotropies found in the cosmic microwave background. Kinetically dominated regimes arise in classical fast-roll scenarios as well as in quantum bouncing cosmologies. For instance, kinetic dominance is typical in interesting preinflationary phases of loop quantum cosmology. In this work, we analyze the leading-order effects that the presence of a scalar field potential causes on the primordial cosmological perturbations in these kinetically dominated epochs. These effects can be grouped in two sets, namely, those that affect the effective mass of the perturbations and those that affect the choice of their vacuum state. The effective mass is modified directly by terms that include the potential, but also indirectly by the change in the background dynamics and the relation between the parameterization of these dynamics and the conformal time, usually employed to describe the evolution of the perturbations. On the other hand, away from de Sitter inflation, the Bunch-Davies state is no longer the most natural vacuum at all scales. Recent proposals suggest to modify it by carrying out certain Hamiltonian diagonalization with a suitable asymptotic behavior at large wave number scales. Both this diagonalization condition and the imposed asymptotic behavior depend on the effective mass of the perturbations, and therefore the selected vacuum state varies in the presence of the scalar field potential.