Strong decays of ${\mathrm{\Xi }}_c$ baryons with radial or orbital $\lambda$- and $\rho$-mode excitations with positive parity have been studied in a ${}^3{P}_0$ model. As candidates of these kinds of excited charmed strange baryons, possible configurations and $J^P$ quantum numbers of ${\mathrm{\Xi }}_c(2930)$, ${\mathrm{\Xi }}_c(2980)$, ${\mathrm{\Xi }}_c(3055)$, ${\mathrm{\Xi }}_c(3080)$, and ${\mathrm{\Xi }}_c(3123)$ have been assigned based on experimental data. There are 40 kinds of configurations to describe the first radial or orbital excited ${\mathrm{\Xi }}_c$ in $\lambda$- and $\rho$-mode excitations with positive parity. In these assignments, ${\mathrm{\Xi }}_c(2930)$ may be a $2S$-wave excited ${\tilde{\mathrm{\Xi }}}_{c1}({\frac{1}{2}}^{+})$ or ${\tilde{\mathrm{\Xi }}}_{c1}({\frac{3}{2}}^{+})$, or a $D$-wave excited ${\widehat{\mathrm{\Xi }}}_{c1}^{\prime }({\frac{1}{2}}^{+})$, ${\check{\mathrm{\Xi }}}_{c1}^0({\frac{1}{2}}^{+})$, ${\check{\mathrm{\Xi }}}_{c1}^2({\frac{1}{2}}^{+})$, ${\widehat{\mathrm{\Xi }}}_{c1}^{\prime }({\frac{3}{2}}^{+})$, ${\check{\mathrm{\Xi }}}_{c1}^0({\frac{3}{2}}^{+})$, or ${\check{\mathrm{\Xi }}}_{c1}^2({\frac{3}{2}}^{+})$. ${\mathrm{\Xi }}_c(2980{)}^{+}$ may be a $2S$-wave excited ${\tilde{\mathrm{\Xi }}}_{c1}({\frac{1}{2}}^{+})$ or ${\tilde{\mathrm{\Xi }}}_{c0}^{\prime }({\frac{1}{2}}^{+})$ with $J^P={\frac{1}{2}}^{+}$, or a $D$-wave excited ${\check{\mathrm{\Xi }}}_{c0}^{\prime 0}({\frac{1}{2}}^{+})$ or ${\check{\mathrm{\Xi }}}_{c1}^0({\frac{1}{2}}^{+})$ with $J^P={\frac{1}{2}}^{+}$. ${\mathrm{\Xi }}_c(3055{)}^{+}$ may be a $2S$-wave excited ${\acute{\mathrm{\Xi }}}_{c1}^{\prime }({\frac{3}{2}}^{+})$ or ${\acute{\mathrm{\Xi }}}_{c0}({\frac{1}{2}}^{+})$. It may be a $D$-wave excited ${\mathrm{\Xi }}_{c1}^{\prime }({\frac{3}{2}}^{+})$, ${\mathrm{\Xi }}_{c2}^{\prime }({\frac{5}{2}}^{+})$, ${\mathrm{\Xi }}_{c2}({\frac{3}{2}}^{+})$, or ${\mathrm{\Xi }}_{c2}({\frac{5}{2}}^{+})$. ${\mathrm{\Xi }}_c(3080{)}^{+}$ is very possibly a $2S$-wave excited ${\acute{\mathrm{\Xi }}}_{c0}({\frac{1}{2}}^{+})$ and seems not to be a $D$-wave excitation of ${\mathrm{\Xi }}_c$. Because of the poor experimental information for ${\mathrm{\Xi }}_c(3123)$, it is impossible to identify this state at present. It is found that the channel $\mathrm{\Lambda }D$ vanishes in the strong decay of $P$-wave, $D$-wave, and $2S$-wave excited ${\mathrm{\Xi }}_c$ without $\rho$-mode excitation between the two light quarks ($n_{\rho }=L_{\rho }=0$). In different configurations, some branching fraction ratios related to the internal structure of the $2S$-wave and $D$-wave of ${\mathrm{\Xi }}_c$ are different. These ratios have been computed and can be employed to distinguish different configurations in forthcoming experiments.

The Bessel-inspired behavior of parton densities at small Bjorken $x$ values, obtained in the case of the flat initial conditions for Dokshitzer-Gribov-Lipatov-Altarelli-Parisi evolution equations, is used along with “frozen” and analytic modifications of the strong coupling constant to study the so-called European Muon Collaboration effect. Among other results, this approach allowed predicting small $x$ behavior of the gluon density in nuclei.

Transverse momentum spectra of charged pions, kaons, and protons are measured in proton-proton collisions at $\sqrt{s}=13\mathrm{TeV}$ with the CMS detector at the LHC. The particles, identified via their energy loss in the silicon tracker, are measured in the transverse momentum range of $p_{\mathrm{T}}\approx 0.1–1.7\mathrm{GeV}/c$ and rapidities $|y|<1$. The $p_{\mathrm{T}}$ spectra and integrated yields are compared to previous results at smaller $\sqrt{s}$ and to predictions of Monte Carlo event generators. The average $p_{\mathrm{T}}$ increases with particle mass and charged particle multiplicity of the event. Comparisons with previous CMS results at $\sqrt{s}=0.9$, 2.76, and 7 TeV show that the average $p_{\mathrm{T}}$ and the ratios of hadron yields feature very similar dependences on the particle multiplicity in the event, independently of the center-of-mass energy of the pp collision.

We search for the $J^{PC}=0^{--}$ and $1^{+-}$ light tetraquark states with masses up to $2.46\mathrm{GeV}/c^2$ in $\mathrm{\Upsilon }(1S)$ and $\mathrm{\Upsilon }(2S)$ decays with data samples of $(102\pm 2)$ million and $(158\pm 4)$ million events, respectively, collected with the Belle detector. No significant signals are observed in any of the studied production modes, and 90% credibility level (C.L.) upper limits on their branching fractions in $\mathrm{\Upsilon }(1S)$ and $\mathrm{\Upsilon }(2S)$ decays are obtained. The inclusive branching fractions of the $\mathrm{\Upsilon }(1S)$ and $\mathrm{\Upsilon }(2S)$ decays into final states with $f_1(1285)$ are measured to be $\mathcal{B}(\mathrm{\Upsilon }(1S)\to f_1(1285)+\text{anything})=(46\pm 28(\mathrm{stat})\pm 13(\mathrm{syst}))\times {10}^{-4}$ and $\mathcal{B}(\mathrm{\Upsilon }(2S)\to f_1(1285)+\text{anything})=(22\pm 15(\mathrm{stat})\pm 6.3(\mathrm{syst}))\times {10}^{-4}$. The measured ${\chi }_{b2}\to J/\psi +\text{anything}$ branching fraction is measured to be $(1.50\pm 0.34(\mathrm{stat})\pm 0.22(\mathrm{syst}))\times {10}^{-3}$, and 90% C.L. upper limits for the ${\chi }_{b0,b1}\to J/\psi +\text{anything}$ branching fractions are found to be $2.3\times {10}^{-3}$ and $1.1\times {10}^{-3}$, respectively. For $\mathcal{B}({\chi }_{b1}\to \omega +\text{anything})$, the branching fraction is measured to be $(4.9\pm 1.3(\mathrm{stat})\pm 0.6(\mathrm{syst}))\times {10}^{-2}$. All results reported here are the first measurements for these modes.

We propose a method inspired by discrete light cone quantization to determine the heat kernel for a Schrödinger field theory (Galilean boost invariant with $z=2$ anisotropic scaling symmetry) living in $d+1$ dimensions, coupled to a curved Newton-Cartan background, starting from a heat kernel of a relativistic conformal field theory ($z=1$) living in $d+2$ dimensions. We use this method to show that the Schrödinger field theory of a complex scalar field cannot have any Weyl anomalies. To be precise, we show that the Weyl anomaly ${\mathcal{A}}_{d+1}^G$ for Schrödinger theory is related to the Weyl anomaly of a free relativistic scalar CFT ${\mathcal{A}}_{d+2}^R$ via ${\mathcal{A}}_{d+1}^G=2\pi \delta (m){\mathcal{A}}_{d+2}^R$, where $m$ is the charge of the scalar field under particle number symmetry. We provide further evidence of the vanishing anomaly by evaluating Feynman diagrams in all orders of perturbation theory. We present an explicit calculation of the anomaly using a regulated Schrödinger operator, without using the null cone reduction technique. We generalize our method to show that a similar result holds for theories with a single time-derivative and with even $z>2$.

The cosmological coincidences between the matter and radiation energy densities at recombination as well as between the densities of matter and the cosmological constant at the present time are well known. We point out that, moreover, the third intersection between the energy densities of radiation and the cosmological constant coincides with the reionization epoch. To quantify the statistical relevance of this concurrence, we compute the Bayes factor between the concordance cosmology with free Thomson scattering optical depth and a model for which this parameter is inferred from imposing a match between the time of density equality and the epoch of reionization. This is to characterize the potential explanatory gain if one were to find a parameter-free physical connection. We find a very strong preference for such a concurrence on the Jeffreys scale from current cosmological observations. We furthermore discuss the effect of the choice of priors, changes in reionization history, and free sum of neutrino masses. We also estimate the impact of adding intermediate polarization data from the Planck High Frequency Instrument and prospects for future 21 cm surveys. In the first case, the preference for the correlation remains substantial, whereas future data may give results more decisive in pro or substantial in contra of it. Finally, we provide a discussion on different interpretations of these findings. In particular, we show how a connection between the star-formation history and the cosmological background dynamics can give rise to this concurrence.

Here we consider a flat FRW universe whose horizon entropy meets the Rényi entropy of nonextensive systems. In our model, the ordinary energy-momentum conservation law is not always valid. By applying the Clausius relation as well as the Cai-Kim temperature to the apparent horizon of a flat FRW universe, we obtain modified Friedmann equations. Fitting the model to the observational data on the current accelerated universe, some values for the model parameters are also addressed. Our study shows that the current accelerating phase of universe expansion may be described by a geometrical fluid, originated from the nonextensive aspects of geometry, which models a varying dark energy source interacting with the matter field in the Rastall way. Moreover, our results indicate that the probable nonextensive features of spacetime may also be used to model a varying dark energy source which does not interact with the matter field and is compatible with the current accelerated phase of the Universe.

We perform the all-loop renormalization of the $\mathrm{O}(N)$ $\lambda {\varphi }^4$ scalar field theory with Lorentz violation which is exact in the Lorentz-violating $K_{\mu \nu }$ coefficients. This task is fulfilled analytically first explicitly at next-to-leading order and later at all loop levels through an induction process based on a general theorem emerging from the exact approach. We show that the exact results reduce to the approximated ones, previously obtained, in the appropriated limit and comment on their implications. The current exact calculation involving such a symmetry breaking mechanism in the referred theory is the first one in the literature to our knowledge. At the end, we analyze the effect of Lorentz violation on the asymptotic single-particle states.

We present results for the form factors of the isovector axial vector current in the nucleon state using large scale simulations of lattice QCD. The calculations were done using eight ensembles of gauge configurations generated by the MILC collaboration using the HISQ action with $2+1+1$ dynamical flavors. These ensembles span three lattice spacings $a\approx 0.06$, 0.09, and 0.12 fm and light-quark masses corresponding to the pion masses $M_{\pi }\approx 135$, 225, and 310 MeV. High-statistics estimates allow us to quantify systematic uncertainties in the extraction of $G_A(Q^2)$ and the induced pseudoscalar form factor ${\tilde{G}}_P(Q^2)$. We perform a simultaneous extrapolation in the lattice spacing, lattice volume and light-quark masses of the axial charge radius $r_A$ data to obtain physical estimates. Using the dipole ansatz to fit the $Q^2$ behavior we obtain $r_A{|}_{\text{dipole}}=0.49(3)\mathrm{fm}$, which corresponds to ${\mathcal{M}}_A=1.39(9)\mathrm{GeV}$, and is consistent with ${\mathcal{M}}_A=1.35(17)\mathrm{GeV}$ obtained by the miniBooNE collaboration. The estimate obtained using the $z$-expansion is $r_A{|}_{z-\text{expansion}}=0.46(6)\mathrm{fm}$, and the combined result is $r_A{|}_{\text{combined}}=0.48(4)\mathrm{fm}$. Analysis of the induced pseudoscalar form factor ${\tilde{G}}_P(Q^2)$ yields low estimates for $g_P^{*}$ and $g_{\pi \mathrm{NN}}$ compared to their phenomenological values. To understand these, we analyze the partially conserved axial current (PCAC) relation by also calculating the pseudoscalar form factor. We find that these low values are due to large deviations in the PCAC relation between the three form factors, and in the pion-pole dominance hypothesis.

We extend the idea of fermion bags to Hamiltonian lattice field theories in the continuous time formulation. Using a class of models we argue that the temperature is a parameter that splits the fermion dynamics into small spatial regions that can be used to identify fermion bags. Using this idea we construct a continuous time quantum Monte Carlo algorithm and compute critical exponents in the $3d$ Ising Gross-Neveu universality class using a single flavor of massless Hamiltonian staggered fermions. We find $\eta =0.54(6)$ and $\nu =0.88(2)$ using lattices up to $N=2304$ sites. We argue that even sizes up to $N=10,000$ sites should be accessible with supercomputers available today.

Using a sample of $1.31\times {10}^{9}J/\psi$ events collected with the BESIII detector at the BEPCII collider, we study the decays of $J/\psi \to K_S{K}_L$ and $K_S{K}_S$. The branching fraction of $J/\psi \to K_S{K}_L$ is determined to be $\mathcal{B}(J/\psi \to K_S{K}_L)=(1.93\pm 0.01(\mathrm{stat})\pm 0.05(\mathrm{syst}))\times {10}^{-4}$, which significantly improves on previous measurements. No clear signal is observed for the $J/\psi \to K_S{K}_S$ process, and the upper limit at the 95% confidence level for its branching fraction is determined to be $\mathcal{B}(J/\psi \to K_S{K}_S)<1.4\times {10}^{-8}$, which improves on the previous searches by 2 orders in magnitude and reaches the order of the Einstein-Podolsky-Rosen expectation.

We claim that the paper by Zhong-Ying Fan and Xiaobao Wang on nonlinear electrodynamics coupled to general relativity [Phys. Rev. D 94,124027 (2016)], although correct in general, in some respects repeats previously obtained results without giving proper references. There is also an important point missing in this paper, which is necessary for understanding the physics of the system: in solutions with an electric charge, a regular center requires a non-Maxwell behavior of Lagrangian function $L(f)$, $(f=F_{\mu \nu }{F}^{\mu \nu })$ at small $f$. Therefore, in all electric regular black hole solutions with a Reissner-Nordström asymptotic, the Lagrangian $L(f)$ is different in different parts of space, and the electromagnetic field behaves in a singular way at surfaces where $L(f)$ suffers branching.

We make a theoretical prediction for the ratio of the dark energy to other components in the Universe based on the scenario of the sequestering mechanism [1–3] which was recently proposed as one possible way to solve the cosmological constant problem. In order to evaluate the value of dark energy and the others, we assume a specific scale factor which describes the big-crunch scenario in the scalar-tensor theory. We specify the parameter region where the one can explain the observed dark energy-matter ratio.

We derive expressions for the total Hamiltonian energy of gravitating systems in higher-dimensional theories in terms of the Riemann tensor, allowing a cosmological constant $\mathrm{\Lambda }\in \mathbb{R}$. Our analysis covers asymptotically anti–de Sitter spacetimes, asymptotically flat spacetimes, as well as Kaluza-Klein asymptotically flat spacetimes. We show that the Komar mass equals the Arnowitt-Deser-Misner (ADM) mass in stationary asymptotically flat spacetimes in all dimensions, generalizing the four-dimensional result of Beig, and that this is no longer true with Kaluza-Klein asymptotics. We show that the Hamiltonian mass does not necessarily coincide with the ADM mass in Kaluza-Klein asymptotically flat spacetimes, and that the Witten positivity argument provides a lower bound for the Hamiltonian mass—and not for the ADM mass—in terms of the electric charge. We illustrate our results on the five-dimensional Rasheed metrics, which we study in some detail, pointing out restrictions that arise from the requirement of regularity, which have gone seemingly unnoticed so far in the literature.

We explore the quasistationary profile of a massive charged scalar field in a class of charged black holes in de Rham-Gabadadze-Tolley (dRGT) massive gravity. We discuss how the linear term in the metric, which is a unique character of the dRGT massive gravity, affects the structure of the spacetime. Numerical calculations of the quasinormal modes are performed for a charged scalar field in the dRGT black hole background. For an asymptotically de Sitter (dS) black hole, an improved asymptotic iteration method is used to obtain the associated quasinormal frequencies. The unstable modes are found for the $\ell =0$ case, and their corresponding real parts satisfy the superradiant condition. For $\ell =2$, the results show that all the de Sitter black holes considered here are stable against a small perturbation. For an asymptotically dRGT anti-de Sitter (AdS) black hole, unstable modes are found with the frequency satisfying the superradiant condition. Effects of massive-gravity parameters are discussed. Analytic calculation reveals the unique diffusive nature of quasinormal modes in the massive-gravity model with the linear term. Numerical results confirm the existence of the characteristic diffusive modes in both the dS and AdS cases.

Using some of the latest cosmological data sets publicly available, we derive the strongest bounds in the literature on the sum of the three active neutrino masses, $M_{\nu }$, within the assumption of a background flat $\mathrm{\Lambda }\mathrm{CDM}$ cosmology. In the most conservative scheme, combining Planck cosmic microwave background temperature anisotropies and baryon acoustic oscillations (BAO) data, as well as the up-to-date constraint on the optical depth to reionization ($\tau$), the tightest 95% confidence level upper bound we find is $M_{\nu }<0.151\mathrm{eV}$. The addition of Planck high-$\ell$ polarization data, which, however, might still be contaminated by systematics, further tightens the bound to $M_{\nu }<0.118\mathrm{eV}$. A proper model comparison treatment shows that the two aforementioned combinations disfavor the inverted hierarchy at $\sim 64\%\mathrm{C}.\mathrm{L}.$ and $\sim 71\%\mathrm{C}.\mathrm{L}.$, respectively. In addition, we compare the constraining power of measurements of the full-shape galaxy power spectrum versus the BAO signature, from the BOSS survey. Even though the latest BOSS full-shape measurements cover a larger volume and benefit from smaller error bars compared to previous similar measurements, the analysis method commonly adopted results in their constraining power still being less powerful than that of the extracted BAO signal. Our work uses only cosmological data; imposing the constraint $M_{\nu }>0.06\mathrm{eV}$ from oscillations data would raise the quoted upper bounds by $\mathcal{O}(0.1\sigma )$ and would not affect our conclusions.

We present a direct approach to nonparametrically reconstruct the linear density field from an observed nonlinear map. We solve for the unique displacement potential consistent with the nonlinear density and positive definite coordinate transformation using a multigrid algorithm. We show that we recover the linear initial conditions up to the nonlinear scale ($r_{{\delta }_r{\delta }_L}>0.5$ for $k\lesssim 1h/\mathrm{Mpc}$) with minimal computational cost. This reconstruction approach generalizes the linear displacement theory to fully nonlinear fields, potentially substantially expanding the baryon acoustic oscillations and redshift space distortions information content of dense large scale structure surveys, including for example SDSS main sample and 21 cm intensity mapping initiatives.

The analysis of perturbative quantities is a powerful tool to distinguish between different dark energy models and gravity theories degenerated at the background level. In this work, we generalize the integral solution of the matter density contrast for general relativity gravity [V. Sahni and A. Starobinsky, Int. J. Mod. Phys. D 15, 2105 (2006)., U. Alam, V. Sahni, and A. A. Starobinsky, Astrophys. J. 704, 1086 (2009).] to a wide class of modified gravity (MG) theories. To calculate this solution, it is necessary to have prior knowledge of the Hubble rate, the density parameter at the present epoch (${\mathrm{\Omega }}_{m0}$), and the functional form of the effective Newton’s constant that characterizes the gravity theory. We estimate in a model-independent way the Hubble expansion rate by applying a nonparametric reconstruction method to model-independent cosmic chronometer data and high-$z$ quasar data. In order to compare our generalized solution of the matter density contrast, using the nonparametric reconstruction of $H(z)$ from observational data, with a purely theoretical one, we choose a parametrization of the screened modified gravity and the ${\mathrm{\Omega }}_{m0}$ from WMAP-9 Collaborations. Finally, we calculate the growth index for the analyzed cases, finding very good agreement between theoretical values and the obtained ones using the approach presented in this work.

The possibility of a subdominant component of dark matter dissipating energy could lead to dramatic new phenomenology such as the formation of a dark disk. One rigorous way to assess this possibility and settle the debate on its feasibility is to include the dissipative dark component in a numerical hydrodynamical simulation. A necessary input to such a simulation is a prescription including energy dissipation rates of different processes and rates of processes that change the number densities of dark ions and atoms. In this article, we study the simplest dissipative dark sector which consists of a dark electron and proton, both charged under a dark gauged $U(1)$. We present approximate analytic formulas for energy loss rates due to Compton scattering, bremsstrahlung, recombination, collisional ionization, and collisional excitation as well as the rates of number density change. We also include the heating rate due to photoionization. The work serves as the first step to realize a numerical simulation including a dissipative dark sector, which hopefully can shed more light on the formation and properties of a dark disk originating from dark matter self-interactions.

The reaction $e^{+}{e}^{-}\to {\mathrm{\Lambda }}_c^{+}{\overline{\mathrm{\Lambda }}}_c^{-}$ is investigated at energies close to the threshold with emphasis on the role played by the $X(4630)$ resonance. The interaction in the final ${\mathrm{\Lambda }}_c^{+}{\overline{\mathrm{\Lambda }}}_c^{-}$ system, constructed within chiral effective field theory and supplemented by a pole diagram that represents a bare $X(4630)$ resonance, is taken into account rigorously. The pole parameters of the $X(4630)$ are extracted and found to be compatible with the ones of the $X(4660)$ resonance that have been established in the reaction $e^{+}{e}^{-}\to {\pi }^{+}{\pi }^{-}\psi (2S)$. The actual result for the $X(4630)$ is $M=(4652.5\pm 3.4)\mathrm{MeV}$ and $\mathrm{\Gamma }=(62.6\pm 5.6)\mathrm{MeV}$. Predictions for the ${\mathrm{\Lambda }}_c^{+}$ electromagnetic form factors in the timelike region are presented.