We discuss the interaction of an open heavy meson ($\overline{D}$ and ${\overline{D}}^{*}$ for charm or $B$ and $B^{*}$ for bottom) and a nucleon ($N$) by considering the $\pi$, $\sigma$, $\rho$, and $\omega$ exchange potentials. We construct a potential model by respecting chiral symmetry for light quarks and spin symmetry for heavy quarks. Model parameters are adjusted by referring the phenomenological nuclear (CD-Bonn) potentials reproducing the low-energy $NN$ scatterings. We show that the resulting interaction may accommodate $\overline{D}N$ and $BN$ bound states with quantum numbers $I(J^P)=0(1/2^{-})$, and $1(1/2^{-})$. We find that, in the present potential model, the $\pi$ exchange potential plays an important role for the isosinglet channel, while the $\sigma$ exchange potential does for the isotriplet one.

The analysis of gravitational-wave (GW) datasets is based on the comparison of measured time series with theoretical templates of the detector’s response to a variety of source parameters. For the Laser Interferometer Space Antenna (LISA), the main scientific observables will be the so-called time-delay interferometry (TDI) combinations, which suppress the otherwise overwhelming laser noise. Computing the TDI response to GWs involves projecting the GW polarizations onto the LISA constellation arms, and then combining projections delayed by a multiple of the light propagation time along the arms. Both computations are difficult to perform efficiently for generic LISA orbits and GW signals. Various approximations are currently used in practice, e.g., assuming constant and equal arm lengths, which yields analytical TDI expressions that are essential to the desirable speed of current analysis codes. In this article, we present fastlisaresponse, a new efficient graphics-processing-unit-accelerated code designed to perform systematics studies on the LISA response in a fully Bayesian context. We examine loud Galactic binary signals first with the typical equal-arm-length approximation and then with a hybrid template that uses accurate orbits for the projections and equal-arm-length orbits for the TDI combinations. The hybrid template is an attempt to preserve the efficient analytical TDI expressions. We conclude that all equal-arm-length parameter-estimation codes, including when only used for TDI, need to be upgraded to the generic response if they are to achieve optimal accuracy for high (but reasonable) SNR sources within the actual LISA data.

Recently, Evslin has constructed the kink form factor relevant to the scattering of an ultrarelativistic meson with an arbitrary nonrelativistic scalar kink. However the formula was only applied to the sine-Gordon model, where the form factor was long ago determined by Weisz using integrability. In this paper, using various known analytic results for the ($1+1$)-dimensional real scalar ${\mathrm{\Phi }}^4$ model and a kink wave packet construction, we analytically calculate the leading quantum correction to the form factor of the ${\mathrm{\Phi }}^4$ kink. We discuss its properties in general and also in the ultrarelativistic meson case and provide a numerical check of our results.

We update and improve past efforts to predict the leptonic Dirac $CP$-violating phase with models that predict perturbatively modified tribimaximal or bimaximal mixing. Simple perturbations are applied to both mixing patterns in the form of rotations between two sectors. By translating these perturbed mixing matrices to the standard parametrization for the neutrino mixing matrix we derive relations between the Dirac $CP$ phase and the oscillation angles. We use these relations together with current experimental results to constrain the allowed range for the $CP$ phase and determine its probability density. Furthermore, we elaborate on the prospects for future experiments probing on the perturbations considered in this work. We present a model with $A_4$ modular symmetry that is consistent with one of the described perturbed scenarios and successfully predicts current oscillation parameter data.

Supersymmetric extensions of the Standard Model with scalar superpartners above 10 TeV are well motivated since the Higgs boson mass can be explained by quantum corrections while maintaining gauge coupling unification. If supersymmetry breaking is transmitted to gauginos via anomaly mediation, the gaugino masses are loop suppressed compared to scalar masses, and the lightest supersymmetric particle is the Higgsino or wino, which can be the dark matter. In this setup, we identify the regions of parameter space that reproduce the observed Higgs boson mass and the thermal abundance of dark matter. We analyze the effects of complex phases in the gaugino mass parameters on the electron electric dipole moment (EDM) and the dark matter scattering cross section. We find that, for scalar masses up to 10 PeV and any size of the complex phases, the model with Higgsino dark matter is within reach of planned experiments—Advanced ACME via electron EDM and LUX-ZEPLIN via dark matter direct detection—with complementary discovery potentials, and the model with wino dark matter is within reach of future electron EDM experiments.

We study rare three-body decays of the $\mathrm{\Omega }$ baryon using SU(3) chiral perturbation theory, the successful effective field theory of quantum chromodynamics at low energies. At leading order, we calculate the branching fractions of the decay ${\mathrm{\Omega }}^{-}\to \mathrm{\Xi }\pi \pi$ for all possible combinations of pions. For one channel, we find an order-of-magnitude discrepancy between theory and experiment. This tension is known to exist in the nonrelativistic limit, and we confirm that it remains in the relativistic calculation. Fairly independent of the values of the low-energy constants, we establish lower limits for the branching fractions of these three-body $\mathrm{\Omega }$ decays, which reaffirm the gap between theory and experiment. We point out that this discrepancy is closely tied to the $\mathrm{\Delta }I=1/2$ selection rule. In turn, this means that the three-body decays constitute an interesting tool to scrutinize the selection rule. Using next-to-leading-order calculations, we also provide predictions for the decay ${\mathrm{\Omega }}^{-}\to {\mathrm{\Xi }}^0{\mu }^{-}{\overline{\nu }}_{\mu }$. We show that fully differential distributions will provide access to low-energy constants needed in the axial-vector transitions from a decuplet to octet baryon. Since data for all of these rare three-body $\mathrm{\Omega }$ decays are scarce (fully differential data are nonexistent), we recommend that they be remeasured at running and upcoming experiments, such as BESIII, LHCb, Belle-II, and PANDA.

We construct a type-II holographic superconductor from an anisotropic rotating background metric. We study the effects of the magnetic field on the vortex structure, including continuous deformations from triangular to square lattices or vice versa. Our holographic model reproduces known experimental vortex lattice deformations and the increment of the vortex population by increasing the external magnetic field.

Composed of ultralight bosons, fuzzy dark matter provides an intriguing solution to challenges that the standard cold dark matter model encounters on subgalactic scales. The ultralight dark matter with mass $m\sim {10}^{-23}\mathrm{eV}$ will induce a periodic oscillation in gravitational potentials with a frequency in the nanohertz band, leading to observable effects in the arrival times of radio pulses from pulsars. Unlike scalar dark matter, pulsar timing signals induced by the vector dark matter are dependent on the oscillation direction of the vector fields. In this work, we search for ultralight vector dark matter in the mass range of $[2\times {10}^{-24},2\times {10}^{-22}]\mathrm{eV}$ through its gravitational effect in the Parkes Pulsar Timing Array (PPTA) second data release. Since no statistically significant detection is made, we place 95% upper limits on the local dark matter density as ${\rho }_{\mathrm{VF}}\lesssim 5{\mathrm{GeV}/\mathrm{cm}}^3$ for $m\lesssim {10}^{-23}\mathrm{eV}$. As no preferred direction is found for the vector dark matter, these constraints are comparable to those given by the scalar dark matter search with an earlier 12-year dataset of PPTA.

We consider the O(6) nonlinear sigma model, with the level-1 Wess-Zumino-Witten term in $3+1$ space-time dimensions. If we divide the O(6) order parameter into two sets of three components, the solitons (hedgehogs) in the first and second set play the role of charge and monopole in the electromagnetic duality. The condensation of these solitons can trigger a direct transition between orders characterized by the two sets of order parameters. We conjecture that the critical point occurs when the theory is self-dual. Moreover, the theory possesses two deconfined phases, where finite-energy hedgehogs coexist with gapless U(1) gauge bosons.

The global polarization of $\mathrm{\Lambda }/\overline{\mathrm{\Lambda }}$ and the splitting between them induced by rotation and magnetic field has been investigated in a dynamical quark model by taking into account the axial-vector interaction and the anomalous magnetic moment of quarks. It is found that the rotation leads to the spin polarization of quarks and antiquarks with the same sign, while the magnetic field leads to the opposite sign, which corresponds to the $\overline{\mathrm{\Lambda }}-\mathrm{\Lambda }$ polarization splitting. The combination of the two effects leads to perfect agreement with experimental data. Quantitatively, the axial-vector interaction contributes 30% of the global polarization and the anomalous magnetic moment of quarks contributes 40% to the splitting of $\overline{\mathrm{\Lambda }}-\mathrm{\Lambda }$ polarization. However, at $\sqrt{s_{NN}}\le 7.7\mathrm{GeV}$, it still remains a challenge to reach enough magnitude of the magnetic field at freeze-out.

To find out the possible scenarios for quantum gravity consistent with the observed Universe, we numerically investigate the nonperturbative renormalization group equations of a general quadratic gravity theory recently derived by Sen et al. [J. High Energy Phys. 03 (2022) 130]. As boundary conditions, we impose consistency with the Hubble and laboratory scale experiments, as well as the Starobinsky model of inflation. We find two kinds of trajectories that go to different regimes at the trans-Planckian scales: (i) a trajectory that flows to the asymptotically free regime and (ii) a trajectory that flows to the asymptotically safe regime. To determine the early-time cosmological scenario, additional observational data from beyond the homogeneous and isotropic space-time are necessary.

We consider the volume of the gauge orbit space for gauge fields on four-dimensional complex projective space. The analysis uses a parametrization of gauge fields where gauge transformations act homogeneously on the fields, facilitating a manifestly gauge-invariant analysis. The volume element contains a four-dimensional Wess-Zumino-Witten (WZW) action for a Hermitian matrix-valued field. There is also a masslike term for certain components of the gauge field. We discuss how the mass term could be related to results from lattice simulations as well as Schwinger-Dyson equations. We argue for a kinematic regime where the Yang-Mills theory can be approximated by the 4d-WZW theory. The result is suggestive of the instanton liquid picture of QCD. Further it is also indicative of the mechanism for confinement being similar to what happens in two dimensions.

A parametrization of gauge fields on complex projective spaces of arbitrary dimension is given as a generalization of the real two-dimensional case. Gauge transformations act homogeneously on the fields, facilitating a manifestly gauge-invariant analysis. Specializing to four dimensions, we consider the nature of the effective action due to chiral scalars interacting with the gauge fields. The key qualitatively significant terms include a possible gauge-invariant mass term and a finite four-dimensional Wess-Zumino-Witten (WZW) action. We comment on relating the mass term to lattice simulations as well as Schwinger-Dyson analyses and also on relating the WZW action to the instanton liquid picture of QCD.

Thomas-Whitehead (TW) gravity was recently introduced as a projective gauge theory of gravity over a d-dimensional manifold that embeds reparametrization invariance into the action functional for gravitation through the use of the Thomas-Whitehead connection. The projective invariance in this d-dimensional theory enjoys an intimate relationship with the Virasoro coadjoint elements found in string theory as one of the components of the connection, ${\mathcal{D}}_{ab}$, is directly related to the coadjoint elements of the Virasoro algebra. TW gravity exploits projective Gauss-Bonnet terms in the action functional which allows the theory to collapse to Einstein’s theory of general relativity in the limit that ${\mathcal{D}}_{ab}$ vanishes. In this paper we develop the graded extension of TW gravity, super-TW gravity, in the framework of a DeWitt supermanifold. We construct the Lagrangian for super-TW gravity, give a detailed derivation of the classical field equations, and discuss the graded extension of the projective connection as a prelude to a future understanding of TW-supergravity (which has manifest supersymmetry) and its relationship to the super-Virasoro algebra.

We study the chaotic signatures of the geodesic dynamics of a nonspinning test particle in the effective-one-body (EOB) formalism for the inspiral process of spinning binary black holes. We first show that the second-order post-Newtonian (2PN) EOB dynamics is nonintegrable by demonstrating that the EOB metric does not satisfy the criterion for the existence of the Carter constant. We then employ the numerical study to find the plateaus of the rotation curve, which are associated with the existence of Birkhoff islands in the Poincaré surface of section, signifying the chaotic dynamics in the system. Our results show the signatures of chaos for the EOB dynamics, especially in the regime of interest for which the Kerr bounds of the component black holes hold. We also find that chaotic behavior is more obvious as the spin parameter $a$ of the deformed EOB background metric increases. Our results can help to uncover the implications of dynamical chaos in gravitational wave astronomy. Finally, we also present some preliminary results due to corrections at 3PN order.

Expanding upon our previous study of competing critical phenomena in black hole formation, we numerically investigate the behavior of dominant exponents across the boundary separating asymptotically dispersing and collapsing regions in a two-dimensional configuration space of initial data. We find that across the type II boundary section the dominant exponent remains constant, equal to the reciprocal of Choptuik’s well-known quasiuniversal value, whereas across the type I section the exponent noticeably varies. We postulate that this change reflects the existence of a third critical solution in addition to the two primary competing solutions, possibly another member of the family of metastable soliton stars constituting the type I attractor.

We compare recently computed waveforms from second-order gravitational self-force (GSF) theory to those generated by a new, GSF-informed, effective one body (EOB) waveform model for (spin-aligned, eccentric) inspiralling black hole binaries with large mass ratios. We focus on quasicircular, nonspinning, configurations and perform detailed GSF/EOB waveform phasing comparisons, either in the time domain or via the gauge-invariant dimensionless function $Q_{\omega }\equiv {\omega }^2/\dot{\omega }$, where $\omega$ is the gravitational wave frequency. The inclusion of high-PN test-mass terms within the EOB radiation reaction (notably, up to 22PN) is crucial to achieve an EOB/GSF phasing agreement below 1 rad up to the end of the inspiral for mass ratios up to 500. For larger mass ratios, up to $5\times {10}^4$, the contribution of horizon absorption becomes more and more important and needs to be accurately modeled. Our results indicate that our GSF-informed EOB waveform model is a promising tool to describe waveforms generated by either intermediate or extreme mass ratio inspirals for future gravitational wave detectors.

We present the first systematic comparison between gravitational waveforms emitted by inspiralling, quasicircular and nonspinning black hole binaries computed with three different approaches: second-order gravitational self-force (2GSF) theory, as implemented in the 1PAT1 model; numerical relativity (NR), as implemented by the SXS collaboration; and the effective one body (EOB) formalism, as implemented in the teobresums waveform model. To compare the models we use both a standard, time-domain waveform alignment and a gauge-invariant analysis based on the dimensionless function $Q_{\omega }(\omega )\equiv {\omega }^2/\dot{\omega }$, where $\omega$ is the gravitational wave frequency. We analyze the domain of validity of the 1PAT1 model, deriving error estimates and showing that the effects of the final transition to plunge, which the model neglects, extend over a significantly larger frequency interval than one might expect. Restricting to the inspiral regime, we find that, while for mass ratios $q=m_1/m_2\le 10$ teobresums is largely indistinguishable from NR, 1PAT1 has a significant dephasing $\gtrsim 1\mathrm{rad}$; conversely, for $q\gtrsim 100$, 1PAT1 is estimated to have phase errors $<0.1\mathrm{rad}$ on a large frequency interval, while teobresums develops phase differences $\gtrsim 1\mathrm{rad}$ with it. Most crucially, on that same large frequency interval we find good agreement between teobresums and 1PAT1 in the intermediate regime $15\lesssim q\lesssim 64$, with $<0.5\mathrm{rad}$ dephasing between them. A simple modification to the teobresums flux further improves this agreement for $q\gtrsim 30$, reducing the dephasing to $\approx 0.27\mathrm{rad}$ even at $q=128$. While our analysis points to the need for more highly accurate, long-inspiral, NR simulations for $q\gtrsim 15$ to precisely quantify the accuracy of EOB/2GSF waveforms, we can clearly identify the primary sources of error and routes to improvement of each model. In particular, our results pave the way for the construction of GSF-informed EOB models for both intermediate and extreme mass ratio inspirals for the next generation of gravitational wave detectors.

We study the cosmological evolution of a nonflat Friedmann-Robertson-Walker Universe filled by pressureless dark matter and Barrow holographic dark energy (BHDE). The latter is a dark energy model based on the holographic principle with Barrow entropy instead of the standard Bekenstein-Hawking one. By assuming the apparent horizon of the Universe as IR cutoff, we explore both the cases where a mutual interaction between the dark components of the cosmos is absent/present. We analyze the behavior of various model parameters, such as the BHDE density parameter, the equation of state parameter, the deceleration parameter, the jerk parameter, and the square of sound speed. We also comment on the observational consistency of our predictions, showing that the interacting model turns out to be favored by recent experimental constraints from $\mathrm{Planck}+\mathrm{WP}+\mathrm{BAO}$, $\mathrm{SNIa}+\mathrm{CMB}+\mathrm{LSS}$ and Union2 SNIa joint analysis over the noninteracting one. The thermal stability of our framework is finally discussed by demanding the positivity of the heat capacities and compressibilities of the cosmic fluid.