We perform extensive nonlinear numerical simulations of the spherical collapse of (charged) wave packets onto a charged black hole within Einstein-Maxwell theory and in Einstein-Maxwell-scalar theory featuring nonminimal couplings and a spontaneous scalarization mechanism. We confirm that black holes in full-fledged Einstein-Maxwell theory cannot be overcharged past extremality and no naked singularities form, in agreement with the cosmic censorship conjecture. We show that naked singularities do not form even in Einstein-Maxwell-scalar theory, although it is possible to form scalarized black holes with charge above the Reissner-Nordström bound. We argue that charge and mass extraction due to superradiance at the fully nonlinear level is crucial to bound the charge-to-mass ratio of the final black hole below extremality. We also discuss some “descalarization” mechanisms for scalarized black holes induced either by superradiance or by absorption of an opposite-charged wave packet; in all cases the final state after descalarization is a subextremal Reissner-Nordström black hole.

Intermediate mass-ratio inspiral (IMRI) binaries—containing stellar-mass black holes coalescing into intermediate-mass black holes $(M>100M_{\odot })$—are a highly anticipated source of gravitational waves (GWs) for Advanced LIGO/Virgo. Their detection and source characterization would provide a unique probe of strong-field gravity and stellar evolution. Because of the asymmetric component masses and the large primary, these systems generically excite subdominant modes while reducing the importance of the dominant quadrupole mode. Including higher order harmonics can also result in a $10\%–25\%$ increase in signal-to-noise ratio for IMRIs, which may help to detect these systems. We show that by including subdominant gravitational-wave modes into the analysis we can achieve a precise characterization of IMRI source properties. For example, we find that the source properties for IMRIs can be measured to within 2%–15% accuracy at a fiducial signal-to-noise ratio of 25 if subdominant modes are included. When subdominant modes are neglected, the accuracy degrades to 9%–44% and significant biases are seen in chirp mass, mass ratio, primary spin, and luminosity distances. We further demonstrate that including subdominant modes in the waveform model can enable an informative measurement of both individual spin components and improve the source localization by a factor of $\sim 10$. We discuss some important astrophysical implications of high precision source characterization enabled by subdominant modes such as constraining the mass gap and probing formation channels.

In this paper, we investigate the gravitational-wave generation problem at the first post-Newtonian order in the context of Einstein-Cartan theory by exploiting the Blanchet-Damour formalism. The quantum intrinsic spin carried by slowly moving, weakly stressed, weakly self-gravitating sources is described geometrically by means of the torsion tensor. We obtain the expression of the source multipole moments with the required accuracy. The analysis of the physical meaning of the lowest-order nonradiative moments and of the asymptotic gravitational waveform is also performed. Eventually, we draw our conclusions and estimate the order of magnitude of the spin contributions in the gravitational-wave signal.

The axion quark nuggets introduced in the literature are a candidate for cold dark matter which, in addition, may be relevant in baryogenesis scenarios. The present work studies the evolution of these objects till they enter in the color superconducting phase. This evolution was already considered in [S. Ge, X. Liang, and A. Zhitnitsky, Phys. Rev. D 97, 043008 (2018).], where it is concluded that a large chemical potential $\mu$ is induced on the bulk of the object. That work takes the baryon number accumulated at the domain wall surrounding the object as predominant, and suggests that internal and external fluxes are compensated in such a way that they not modify considerably the dynamics of the object if they are neglected. In the present work the possibility that the bulk contribution to the baryon number may be relevant at initial stages, and that the object may emit a large amount of neutrinos due to quark-antiquark annihilations is taken into account. This results into a more violent contraction of the object and perhaps a more effective cooling. The outcome is that the formed objects may have an smaller size. Even taking into account these corrections, it is concluded that the cosmological applications of these objects are not spoiled. These applications are discussed along the text.

Velocity fields can be reconstructed at cosmological scales from their influence on the correlation between the cosmic microwave background and large-scale structure. Effects that induce such correlations include the kinetic Sunyaev Zel’dovich (kSZ) effect and the moving-lens effect, both of which will be measured to high precision with upcoming cosmology experiments. Galaxy measurements also provide a window into measuring velocities from the effect of redshift-space distortions (RSDs). The information that can be accessed from the kSZ or RSDs, however, is limited by astrophysical uncertainties and systematic effects, which may significantly reduce our ability to constrain cosmological parameters such as $f{\sigma }_8$. In this paper, we show how the large-scale transverse-velocity field, which can be reconstructed from measurements of the moving-lens effect, can be used to measure $f{\sigma }_8$ to high precision.

Despite strong evidence for the existence of large amounts of dark matter (DM) in our Universe, there is no direct indication of its presence in our own solar system. All estimates of the local DM density rely on extrapolating results on much larger scales. We demonstrate for the first time the possibility of simultaneously measuring the local DM density and interaction cross section with a direct detection experiment. It relies on the assumption that incoming DM particles frequently scatter on terrestrial nuclei prior to detection, inducing an additional time-dependence of the signal. We show that for sub-GeV DM, with a large spin-independent DM-proton cross section, future direct detection experiments should be able to reconstruct the local DM density with smaller than 50% uncertainty.

We discuss helicity polarization, which can be locally induced from both vorticity and helicity charge in noncentral heavy ion collisions. Helicity charge redistribution can be generated in viscous fluid, and contributes to azimuthal asymmetry of the polarization along global angular momentum or beam momentum. We also discuss detecting the initial net helicity charge from topological charge fluctuation or initial color longitudinal field by the helicity correlation of two hyperons and the helicity alignment of vector mesons in central heavy ion collisions.

We study the sensitivity of the Fermilab Short-Baseline Neutrino (SBN) experiments, MicroBooNE, ICARUS, and SBND, to MeV- to GeV-scale inelastic dark matter interacting through a dark photon mediator. These models provide interesting scenarios of light thermal dark matter, which, while challenging to probe with direct and indirect detection experiments, are amenable to accelerator-based searches. We consider production of the dark sector states with both the Fermilab Booster 8 GeV and NuMI 120 GeV proton beams and study the signatures of scattering and decay of the heavy excited dark state in the SBN detectors. These distinct signatures probe complementary regions of parameter space. All three experiments will be able to cover new ground, with an excellent near-term opportunity to search for cosmologically motivated targets explaining the observed dark matter abundance.

We study supersymmetric (SUSY) effects on $C_7({\mu }_b)$ and $C_7^{\prime }({\mu }_b)$ which are the Wilson coefficients (WCs) for $b\to s\gamma$ at b-quark mass scale ${\mu }_b$ and are closely related to radiative $B$-meson decays. The SUSY-loop contributions to $C_7({\mu }_b)$ and $C_7^{\prime }({\mu }_b)$ are calculated at leading order (LO) in the Minimal Supersymmetric Standard Model (MSSM) with general quark-flavor violation (QFV). For the first time we perform a systematic MSSM parameter scan for the WCs $C_7({\mu }_b)$ and $C_7^{\prime }({\mu }_b)$ respecting all the relevant constraints, i.e., the theoretical constraints from vacuum stability conditions and the experimental constraints, such as those from $K$- and $B$-meson data and electroweak precision data, as well as recent limits on SUSY particle masses and the 125 GeV Higgs boson data from LHC experiments. From the parameter scan we find the following: (1) The MSSM contribution to $\mathrm{Re}(C_7({\mu }_b))$ can be as large as $\sim \pm 0.05$, which could correspond to about $3\sigma$ significance of New Physics (NP) signal in the future LHCb and Belle II experiments. (2) The MSSM contribution to $\mathrm{Re}(C_7^{\prime }({\mu }_b))$ can be as large as $\sim -0.08$, which could correspond to about $4\sigma$ significance of NP signal in the future LHCb and Belle II experiments. (3) These large MSSM contributions to the WCs are mainly due to (i) large scharm-stop mixing and large scharm/stop involved trilinear couplings $T_{U23}$, $T_{U32}$ and $T_{U33}$, (ii) large sstrange-sbottom mixing and large sstrange-sbottom involved trilinear couplings $T_{D23}$, $T_{D32}$ and $T_{D33}$ and (iii) large bottom Yukawa coupling $Y_b$ for large $\tan \beta$ and large top Yukawa coupling $Y_t$. In case such large NP contributions to the WCs are really observed in the future experiments at Belle II and the LHCb Upgrade, this could be the imprint of QFV SUSY (the MSSM with general QFV) and would encourage to perform further studies of the WCs $C_7^{\prime }({\mu }_b)$ and $C_7^{\mathrm{MSSM}}({\mu }_b)$ at higher order (NLO/NNLO) level in this model.

We propose the use of the Earth as a transducer for ultralight dark-matter detection. In particular, we point out a novel signal of kinetically mixed dark-photon dark matter: a monochromatic oscillating magnetic field generated at the surface of the Earth. Similar to the signal in a laboratory experiment in a shielded box (or cavity), this signal arises because the lower atmosphere is a low-conductivity air gap sandwiched between the highly conductive interior of the Earth below and ionosphere or interplanetary medium above. At low masses (frequencies) the signal in a laboratory detector is usually suppressed by the size of the detector multiplied by the dark-matter mass. Crucially, in our case the suppression is by the radius of the Earth, and not by the (much smaller) height of the atmosphere. We compute the size and global vectorial pattern of our magnetic field signal, which enables sensitive searches for this signal using unshielded magnetometers dispersed over the surface of the Earth. In principle, the signal we compute exists for any dark photon in the mass range ${10}^{-21}\mathrm{eV}\lesssim m_{A^{\prime }}\lesssim 3\times {10}^{-14}\mathrm{eV}$. We summarize the results of our companion paper [M. A. Fedderke et al., Search for dark-photon dark matter in the SuperMAG geomagnetic field dataset, arXiv:2108.08852], in which we detail such a search using a publicly available dataset from the SuperMAG Collaboration: we report no robust signal candidates and so place constraints in the (more limited) dark-photon dark-matter mass range $2\times {10}^{-18}\mathrm{eV}\lesssim m_{A^{\prime }}\lesssim 7\times {10}^{-17}\mathrm{eV}$ (corresponding to frequencies $6\times {10}^{-4}\mathrm{Hz}\lesssim f\lesssim 2\times {10}^{-2}\mathrm{Hz}$). These constraints are complementary to existing astrophysical bounds. Future searches for this signal may improve the sensitivity over a wide range of ultralight dark-matter candidates and masses.

We present a calculation of the up, down, strange, and charm quark masses performed within the lattice QCD framework. We use the twisted-mass fermion action and carry out simulations that include in the sea two light mass-degenerate quarks, as well as the strange and charm quarks. In the analysis, we use gauge ensembles simulated at three values of the lattice spacing and with light quarks that correspond to pion masses in the range from 350 MeV to the physical value, while the strange and charm quark masses are tuned approximately to their physical values. We use several quantities to set the scale in order to check for finite lattice spacing effects, and in the continuum limit, we get compatible results. The quark mass renormalization is carried out nonperturbatively using the (modified) Regularization Independent Momentum Subtraction (${\mathrm{RI}}^{\prime }\text{−}\mathrm{MOM}$) method converted into the $\overline{\mathrm{MS}}$ scheme. For the determination of the quark masses, we use physical observables from both the meson and the baryon sectors, obtaining $m_{ud}=3.636(66)({}_{-57}^{+60})\mathrm{MeV}$ and $m_s=98.7(2.4)({}_{-3.2}^{+4.0})\mathrm{MeV}$ in the $\overline{\mathrm{MS}}(2\mathrm{GeV})$ scheme and $m_c=1036(17)({}_{-8}^{+15})\mathrm{MeV}$ in the $\overline{\mathrm{MS}}(3\mathrm{GeV})$ scheme, where the first errors are statistical and the second ones are combinations of systematic errors. For the quark mass ratios, we get $m_s/m_{ud}=27.17(32)({}_{-38}^{+56})$ and $m_c/m_s=11.48(12)({}_{-19}^{+25})$.

The infrared behavior of the quark propagator is studied at one loop and in the Landau gauge ($\xi =0$) using the screened massive expansion of full QCD and three different resummation schemes for the quark self-energy. The shift of the expansion point of perturbation theory, which defines the screened expansion, together with a nonstandard renormalization of the bare parameters, proves sufficient to describe the dynamical generation of an infrared quark mass also in the chiral limit. Analytically, the scale for such a mass is set by a mass parameter $M$, whose value is fixed by a fit to the lattice data for quenched QCD. The quark mass function $\mathcal{M}(p^2)$ is shown to be in very good agreement with the lattice results. The quark $Z$ function, on the other hand, shows the wrong qualitative behavior in all but one of the studied resummation schemes, where its behavior is qualitatively correct, but only at sufficiently high energies.

The role of the triangle mechanism in the decay process $J/\psi \to K^{-}{K}^{+}{a}_1(1260)$ is probed. In this mechanism, a close-up resonance with mass 1823 MeV and width 122 MeV decays into $K^{*}\varphi ,K^{*}\to K\pi$ and then $K^{*}\overline{K}$ fuses into the $a_1(1260)$ resonance. We find that this mechanism leads to a triangle singularity around $M_{\mathrm{inv}}(K^{-}{a}_1(1260))\approx 1920\mathrm{MeV}$, where the axial-vector meson $a_1(1260)$ is considered as a dynamically generated resonance. With the help of the triangle mechanism we find sizable branching ratios $\mathrm{Br}(J/\psi \to K^{-}{K}^{+}{a}_1(1260),a_1\to \pi \rho )=1.210\times {10}^{-5}$ and $\mathrm{Br}(J/\psi \to K^{-}{K}^{+}{a}_1(1260))=3.501\times {10}^{-5}$. Such an effect from the triangle mechanism of the decay process could be investigated by such as BESIII, LHCb and Belle-II experiments. This potential investigation can help us obtain the information of the axial-vector meson $a_1(1260)$.

In this work we study the $\mathrm{\Sigma }\pi$ and $\mathrm{\Lambda }\pi$ production off free nucleons driven by the strangeness-changing weak charged current. We calculate the total cross sections for all possible channels and estimate the flux-averaged total cross sections for experiments like MiniBooNE, SciBooNE, T2K, and Minerva. The model is based on the lowest order effective SU(3) chiral Lagrangians in the presence of an external weak charged current and contains Born and the lowest-lying decuplet resonant mechanisms that can contribute to these reaction channels. We also compare and discuss our results with others following similar and very different approaches.

Using $980.6{\mathrm{fb}}^{-1}$ of data collected with the Belle detector operating at the KEKB asymmetric-energy $e^{+}{e}^{-}$ collider, we present a measurement of the branching fraction of the singly Cabibbo-suppressed decay ${\mathrm{\Lambda }}_c^{+}\to p\omega$. A clear ${\mathrm{\Lambda }}_c^{+}$ signal is observed for ${\mathrm{\Lambda }}_c^{+}\to p\omega$ with a statistical significance of 9.1 standard deviations, and we measure the ratio of branching fractions $\mathcal{B}({\mathrm{\Lambda }}_c^{+}\to p\omega )/\mathcal{B}({\mathrm{\Lambda }}_c^{+}\to p{K}^{-}{\pi }^{+})=(1.32\pm 0.12(\mathrm{stat})\pm 0.10(\mathrm{syst}))\times {10}^{-2}$, from which we infer the branching fraction $\mathcal{B}({\mathrm{\Lambda }}_c^{+}\to p\omega )=(8.27\pm 0.75(\mathrm{stat})\pm 0.62(\mathrm{syst})\pm 0.42(\mathrm{ref}))\times {10}^{-4}$. The first quoted uncertainty is statistical, the second systematic, and the third from the reference mode ${\mathrm{\Lambda }}_c^{+}\to p{K}^{-}{\pi }^{+}$.

The objective of this paper is to construct the accurate (say, to 11 decimal places) frequencies of the quasinormal modes of the five-dimensional Schwarzschild-Tangherlini black hole using three major techniques: the Hill determinant method, the continued fractions method, and the WKB-Padé method and to discuss the limitations of each. It is shown that for the massless scalar, gravitational tensor, gravitational vector, and electromagnetic vector perturbations considered in this paper, the Hill determinant method and the method of continued fractions (both with the convergence acceleration) always give identical results, whereas the WKB-Padé method gives the results that are amazingly accurate in most cases. Notable exception are the gravitational vector perturbations ($j=2$ and $\ell =2$), for which the WKB-Padé approach apparently does not work. Here we have an interesting situation in which the WKB-based methods (WKB-Padé and WKB–Borel–Le Roy) give the complex frequency that differs from the result obtained within the framework of the continued fraction method and the Hill determinant method. For the fundamental mode, deviation of the real part of frequency from the exact value is 0.5% whereas the deviation of the imaginary part is 2.7%. For $\ell \ge 3$ the accuracy of the WKB results is similar again to the accuracy obtained for other perturbations. The case of the gravitational scalar perturbations is briefly discussed.

Here we report a developed high performance and simplified version of the code denominated rio, which can be easily extended, for the generalized BSSN formulation. We implement a code which is regular at the center of symmetry, without use a special procedure for regularization, as usual. We get exponential convergence for constraints. The numerical algorithm is based on the Galerkin-Collocation method developed successfully for diverse physical scenarios by the Numerical Relativity Group at uerj. For the sake of clarity in presentation, we consider here the most simple case to display the most salient features of the procedure. Thus, we focus on the definite tests of the new numerical framework. The timing and performance of the code show that we can reach a better accuracy close to the machine precision, for the Hamiltonian and momentum constraints. rio will be an open source code; currently it is under continuous development to consider more general and realistic problems.

Using Subaru Hyper Suprime-Cam (HSC) year 1 data, we perform the first $k$-cut cosmic shear analysis constraining both $\mathrm{\Lambda }\mathrm{CDM}$ and $f(R)$ Hu-Sawicki modified gravity. To generate the $f(R)$ cosmic shear theory vector, we use the matter power spectrum emulator trained on COLA (COmoving Lagrangian Acceleration) simulations [Phys. Rev. D 103, 123525 (2021). The $k$-cut method is used to significantly down-weight sensitivity to small scale $(k>1h{\mathrm{Mpc}}^{-1})$ modes in the matter power spectrum where the emulator is less accurate, while simultaneously ensuring our results are robust to baryonic feedback model uncertainty. We have also developed a test to ensure that the effects of poorly modeled small scales are nulled as intended. For $\mathrm{\Lambda }\mathrm{CDM}$ we find $S_8={\sigma }_8({\mathrm{\Omega }}_m/0.3{)}^{0.5}=0.789_{-0.022}^{+0.039}$, while the constraints on the $f(R)$ modified gravity parameters are prior dominated. In the future, the $k$-cut method could be used to constrain a large number of theories of gravity where computational limitations make it infeasible to model the matter power spectrum down to extremely small scales.

We study the nonlinear QED signature of x-ray vacuum diffraction in the head-on collision of optical high-intensity and x-ray free-electron laser pulses at finite spatiotemporal offsets between the laser foci. The high-intensity laser driven scattering of signal photons outside the forward cone of the x-ray probe constitutes a prospective experimental signature of quantum vacuum nonlinearity. Resorting to a simplified phenomenological ad hoc model, it was recently argued that the angular distribution of the signal in the far-field is sensitive to the wavefront curvature of the probe beam in the interaction region with the high-intensity pump. In this work, we model both the pump and probe fields as pulsed paraxial Gaussian beams and reanalyze this effect from first principles. We focus on vacuum diffraction both as an individual signature of quantum vacuum nonlinearity and as a potential means to improve the signal-to-background separation in vacuum birefringence experiments.