Just Accepted
Display Method:
Published:
, doi: 10.1088/1674-1137/ae6311
Abstract:
The exploration of symmetry laws stands as a cutting-edge direction in modern physics research. This work delves into the examination of P and\begin{document}$ CP $\end{document} \begin{document}$ \Omega_c $\end{document} \begin{document}$ \Omega_c $\end{document} \begin{document}$ \Omega_c\rightarrow \Omega^-\pi^+ $\end{document}
The exploration of symmetry laws stands as a cutting-edge direction in modern physics research. This work delves into the examination of P and
Published:
, doi: 10.1088/1674-1137/ae6630
Abstract:
Gravitational-wave astronomy offers a promising opportunity to directly observe scalar-induced gravitational waves originating from the early universe. Experiments—including ground-based interferometers such as LIGO and Virgo, and pulsar timing arrays (PTAs) based on facilities such as FAST and SKA—are poised to significantly enhance sensitivity to these signals. In this paper, we combine Cosmic Microwave Background (CMB) and Baryon Acoustic Oscillation (BAO) datasets with upper or lower limits on the stochastic gravitational-wave background provided by FAST or SKA to constrain scalar-induced gravitational waves. To provide a comprehensive forecast, we consider two scenarios at a given frequency: one in which FAST or SKA does not detect scalar-induced gravitational waves, thereby setting an upper limit on the fractional energy density; and another in which these waves are detected, thus establishing a lower limit. In the ΛCDM+r model, the scalar spectral index of the power-law power spectrum is constrained to\begin{document}$ n_s=0.9598^{+0.0013}_{-0.0009} $\end{document} \begin{document}$ n_s = 0.9697\pm{0.0033} $\end{document} \begin{document}$ n_s $\end{document} \begin{document}$ \alpha_s $\end{document} \begin{document}$ \alpha_s $\end{document} \begin{document}$ \beta_s $\end{document} \begin{document}$ \alpha_s $\end{document} \begin{document}$ \beta_s $\end{document}
Gravitational-wave astronomy offers a promising opportunity to directly observe scalar-induced gravitational waves originating from the early universe. Experiments—including ground-based interferometers such as LIGO and Virgo, and pulsar timing arrays (PTAs) based on facilities such as FAST and SKA—are poised to significantly enhance sensitivity to these signals. In this paper, we combine Cosmic Microwave Background (CMB) and Baryon Acoustic Oscillation (BAO) datasets with upper or lower limits on the stochastic gravitational-wave background provided by FAST or SKA to constrain scalar-induced gravitational waves. To provide a comprehensive forecast, we consider two scenarios at a given frequency: one in which FAST or SKA does not detect scalar-induced gravitational waves, thereby setting an upper limit on the fractional energy density; and another in which these waves are detected, thus establishing a lower limit. In the ΛCDM+r model, the scalar spectral index of the power-law power spectrum is constrained to
Published:
, doi: 10.1088/1674-1137/ae5ef8
Abstract:
We present a systematic analysis of the Higgs signal strengths at 125 GeV and 95 GeV in a non-supersymmetric\begin{document}$ U(1)_X $\end{document} \begin{document}$ U(1)_X $\end{document} \begin{document}$ U(1)_X $\end{document} \begin{document}$ \chi^2 $\end{document} \begin{document}$ \gamma\gamma $\end{document} \begin{document}$ WW^* $\end{document} \begin{document}$ ZZ^* $\end{document} \begin{document}$ b\bar{b} $\end{document} \begin{document}$ \tau\bar{\tau} $\end{document} \begin{document}$ b\bar{b} $\end{document} \begin{document}$ U(1)_X $\end{document} \begin{document}$ g_X $\end{document} \begin{document}$ g_{YX} $\end{document} \begin{document}$ v_S $\end{document} \begin{document}$ v_P $\end{document}
We present a systematic analysis of the Higgs signal strengths at 125 GeV and 95 GeV in a non-supersymmetric
Published:
, doi: 10.1088/1674-1137/ae5c85
Abstract:
Neutrino Earth tomography provides an observational approach to studying the Earth's deep three-dimensional structure that is distinct from seismology. However, most existing studies still rely on one-dimensional density models and therefore cannot adequately represent lateral heterogeneity within the Earth. To address this issue, this study integrates PREM, CRUST1.0, and HMSL-S06 on a tesseroid grid to construct a non-spherically symmetric three-dimensional Earth density model that includes large low-velocity provinces (LLVPs) in the deep mantle. We also develop a corresponding procedure for extracting neutrino propagation trajectories and derive closed-form expressions for the total mass and axial moment of inertia of the discrete model, which are used as global consistency checks. Within an exact three-flavor oscillation framework, we use public Super-Kamiokande data products to compare the event counts predicted by the three-dimensional model with those from a conventional one-dimensional spherically symmetric model. The results show that, under the present calculation scheme, the differences in the overall event count distributions between the three-dimensional model and the one-dimensional reference model remain limited. This study establishes a three-dimensional calculation framework that can provide a methodological basis for future investigations of how lateral density heterogeneity may affect atmospheric neutrino propagation.
Neutrino Earth tomography provides an observational approach to studying the Earth's deep three-dimensional structure that is distinct from seismology. However, most existing studies still rely on one-dimensional density models and therefore cannot adequately represent lateral heterogeneity within the Earth. To address this issue, this study integrates PREM, CRUST1.0, and HMSL-S06 on a tesseroid grid to construct a non-spherically symmetric three-dimensional Earth density model that includes large low-velocity provinces (LLVPs) in the deep mantle. We also develop a corresponding procedure for extracting neutrino propagation trajectories and derive closed-form expressions for the total mass and axial moment of inertia of the discrete model, which are used as global consistency checks. Within an exact three-flavor oscillation framework, we use public Super-Kamiokande data products to compare the event counts predicted by the three-dimensional model with those from a conventional one-dimensional spherically symmetric model. The results show that, under the present calculation scheme, the differences in the overall event count distributions between the three-dimensional model and the one-dimensional reference model remain limited. This study establishes a three-dimensional calculation framework that can provide a methodological basis for future investigations of how lateral density heterogeneity may affect atmospheric neutrino propagation.
Published:
, doi: 10.1088/1674-1137/ae5ef3
Abstract:
Since the Event Horizon Telescope (EHT) collaboration released horizon-scale images of the supermassive black holes Sgr A* and M87*, a new observational window for probing black hole spacetimes in the strong-gravity regime has opened. As an important class of Kerr black hole mimickers, rotating Simpson-Visser (SV) black holes exhibit a degeneracy with Kerr black holes in terms of shadow size, making them difficult to distinguish using shadow observations alone. Motivated by this issue, we present a systematic investigation of the radiative properties and optical appearance of rotating SV black holes surrounded by a thin accretion disk, focusing on the influence of the regularization parameter g on the relevant observables. The results show that although the kinematic quantities and the location of the innermost stable circular orbit (ISCO) depend on the regularization parameter g, the radiative efficiency of the rotating SV black hole is the same as that of its Kerr counterpart. Within the Novikov-Thorne thin-disk model, we study the radiative flux, effective temperature, and spectral luminosity; adopting observational parameters relevant to Sgr A* and M87*, we compute concrete examples for rotating SV black holes and compare them with those for Kerr black holes. The results show that the parameter g suppresses the maximum values of these quantities. In addition, using a backward ray-tracing technique, we numerically simulate the optical appearance of rotating SV black holes and analyze the corresponding intensity images, redshift, and observed flux distributions. Our results indicate that these quantities are sensitive to g. In particular, as g increases, the observed intensity is significantly suppressed, and the photon ring region exhibits a remarkable increase in width. Our findings suggest that accretion-disk-related observables may provide important avenues to distinguish between rotating SV black holes and Kerr black holes, and offer theoretical guidance for future high-resolution observations.
Since the Event Horizon Telescope (EHT) collaboration released horizon-scale images of the supermassive black holes Sgr A* and M87*, a new observational window for probing black hole spacetimes in the strong-gravity regime has opened. As an important class of Kerr black hole mimickers, rotating Simpson-Visser (SV) black holes exhibit a degeneracy with Kerr black holes in terms of shadow size, making them difficult to distinguish using shadow observations alone. Motivated by this issue, we present a systematic investigation of the radiative properties and optical appearance of rotating SV black holes surrounded by a thin accretion disk, focusing on the influence of the regularization parameter g on the relevant observables. The results show that although the kinematic quantities and the location of the innermost stable circular orbit (ISCO) depend on the regularization parameter g, the radiative efficiency of the rotating SV black hole is the same as that of its Kerr counterpart. Within the Novikov-Thorne thin-disk model, we study the radiative flux, effective temperature, and spectral luminosity; adopting observational parameters relevant to Sgr A* and M87*, we compute concrete examples for rotating SV black holes and compare them with those for Kerr black holes. The results show that the parameter g suppresses the maximum values of these quantities. In addition, using a backward ray-tracing technique, we numerically simulate the optical appearance of rotating SV black holes and analyze the corresponding intensity images, redshift, and observed flux distributions. Our results indicate that these quantities are sensitive to g. In particular, as g increases, the observed intensity is significantly suppressed, and the photon ring region exhibits a remarkable increase in width. Our findings suggest that accretion-disk-related observables may provide important avenues to distinguish between rotating SV black holes and Kerr black holes, and offer theoretical guidance for future high-resolution observations.
Published:
, doi: 10.1088/1674-1137/ae5ef7
Abstract:
The internal structure of the light scalar state\begin{document}$ a_0(1450) $\end{document} \begin{document}$ q\bar{q} $\end{document} \begin{document}$ D \to a_0(1450)\ell \nu_\ell $\end{document} \begin{document}$ \ell=(e, \mu) $\end{document} \begin{document}$ \langle\xi^{n}\rangle |_{\mu} $\end{document} \begin{document}$ a_{n}(\mu) $\end{document} \begin{document}$ \mu_0=1\; {\rm{GeV}} $\end{document} \begin{document}$ \mu_k= 1.4\; {\rm{GeV}} $\end{document} \begin{document}$ n=(1,3,5) $\end{document} \begin{document}$ f_+^{({\rm{S}}1)}(0) = 0.836_{-0.119}^{+0.116} $\end{document} \begin{document}$ f_+^{({\rm{S}}2)}(0)=0.767_{-0.105}^{+0.106} $\end{document} \begin{document}$ f_-(0)=0.630_{-0.077}^{+0.078} $\end{document} \begin{document}$ z(q^2, t) $\end{document} \begin{document}$ q^2 $\end{document} \begin{document}$ q^2=10^{-5} \; {\rm{GeV}}^2 $\end{document} \begin{document}$ {d\Gamma}/{d\cos\theta_\ell } $\end{document} \begin{document}$ \cos\theta_\ell \in [-1,1] $\end{document} \begin{document}$ D^0 \to a_0(1450)^- \ell^+ \nu_\ell $\end{document} \begin{document}$ D^- \to a_0(1450)^0 \ell^- \bar{\nu}_\ell $\end{document} \begin{document}$ 10^{-6} $\end{document} \begin{document}$ D^- \to a_0(1450)^0 \ell^- \bar{\nu}_\ell $\end{document} \begin{document}$ {\cal{A}}_{\rm{FB}} $\end{document} \begin{document}$ {\cal{A}}_{\lambda_\ell} $\end{document} \begin{document}$ q^2 $\end{document} \begin{document}$ {\cal{F}}_{\rm{H}} $\end{document}
The internal structure of the light scalar state
Published:
, doi: 10.1088/1674-1137/ae62fa
Abstract:
In this work, we present the first computation of the full one-loop electroweak radiative corrections to the process\begin{document}$ \mu^- \mu^+ \to W^\pm W^\mp \to hh $\end{document} \begin{document}$ \sqrt{s} = 10\; \text{TeV} $\end{document} \begin{document}$ {\cal{L}} = 10000\; \text{fb}^{-1} $\end{document} \begin{document}$ t\bar{t}b\bar{b} $\end{document} \begin{document}$ 2\sigma $\end{document}
In this work, we present the first computation of the full one-loop electroweak radiative corrections to the process
Published:
, doi: 10.1088/1674-1137/ae62fc
Abstract:
We study the equation of state (EoS) of QCD matter in a bottom-up holographic setup that combines an Einstein-Maxwell-dilaton (EMD) sector with an improved Karch-Katz-Son-Stephanov (KKSS) flavor action. In the probe approximation, we perform an inverse reconstruction of the model functions by parameterizing them with neural networks and solving the EMD equations via a differentiable ODE solver (a neural ODE framework), calibrating the model to a reference thermodynamic table for\begin{document}$(2+1)$\end{document} \begin{document}$\mu_B=0$\end{document} \begin{document}$\mu_B=0$\end{document} \begin{document}$\beta_1$\end{document}
We study the equation of state (EoS) of QCD matter in a bottom-up holographic setup that combines an Einstein-Maxwell-dilaton (EMD) sector with an improved Karch-Katz-Son-Stephanov (KKSS) flavor action. In the probe approximation, we perform an inverse reconstruction of the model functions by parameterizing them with neural networks and solving the EMD equations via a differentiable ODE solver (a neural ODE framework), calibrating the model to a reference thermodynamic table for
Published:
, doi: 10.1088/1674-1137/ae5ef6
Abstract:
The atomic nucleus, viewed as a system of bound quarks, should, in principle, be described within an effective theory of low-energy quantum chromodynamics. This paper provides an overview of recently developed models that embody essential features of the desired effective theory. The Fermi gas model helps explain why the number of d quarks is approximately equal to that of u quarks in stable light nuclei up to\begin{document}$ {}^{40}_{20}{\rm Ca} $\end{document} \begin{document}$ {{\rm{AdS}}}_5 $\end{document} \begin{document}$ {\mathbb R}_{1,3} $\end{document} \begin{document}$ Z_{{\rm{max}}} $\end{document} \begin{document}$ Z_{{\rm{max}}}\approx 82 $\end{document} \begin{document}$ {}^{208}_{82}{\rm Pb} $\end{document}
The atomic nucleus, viewed as a system of bound quarks, should, in principle, be described within an effective theory of low-energy quantum chromodynamics. This paper provides an overview of recently developed models that embody essential features of the desired effective theory. The Fermi gas model helps explain why the number of d quarks is approximately equal to that of u quarks in stable light nuclei up to
Published:
, doi: 10.1088/1674-1137/ae5f08
Abstract:
In this work, we investigate the production and decay of molecular states with quark content\begin{document}$cc\bar c\bar q$\end{document} \begin{document}$J^P=1^+$\end{document} \begin{document}${\eta_c D^*}$\end{document} \begin{document}${J/\psi D^*}$\end{document} \begin{document}$B_c$\end{document} \begin{document}$10^{-4}$\end{document} \begin{document}${{\eta}_cD^*}$\end{document} \begin{document}$10^{-5}$\end{document} \begin{document}${J/\psi D^*}$\end{document} \begin{document}${{\eta}_cD^*}$\end{document} \begin{document}${J/\psi D^*}$\end{document} \begin{document}${\cal{O}}$\end{document} \begin{document}$\text{MeV}$\end{document}
In this work, we investigate the production and decay of molecular states with quark content
Published:
, doi: 10.1088/1674-1137/ae643e
Abstract:
We report stronger evidence for the\begin{document}$X(7200)$\end{document} \begin{document}$X(6900)$\end{document} \begin{document}$J/\psi$\end{document} \begin{document}$X(6900)$\end{document} \begin{document}$>12\sigma$\end{document} \begin{document}$X(7200)$\end{document} \begin{document}$3.7\sigma$\end{document} \begin{document}$6.6\sigma$\end{document} \begin{document}$6.6\sigma$\end{document}
We report stronger evidence for the
Published:
, doi: 10.1088/1674-1137/ae5ef2
Abstract:
The Kerr/CFT correspondence establishes a correspondence between extremal black holes in higher dimensions and a chiral conformal field theory (CFT) in their near-horizon limit. A generalization of this framework, known as the EVH/CFT correspondence, has been developed for four- and five-dimensional AdS black holes. It was further proposed in [1 ] that, for \begin{document}${\rm{AdS}}_{D=6,7}$\end{document} \begin{document}$(D-2)$\end{document} \begin{document}$(D-3)$\end{document} \begin{document}${\rm{AdS}}_{D=6,7}$\end{document}
The Kerr/CFT correspondence establishes a correspondence between extremal black holes in higher dimensions and a chiral conformal field theory (CFT) in their near-horizon limit. A generalization of this framework, known as the EVH/CFT correspondence, has been developed for four- and five-dimensional AdS black holes. It was further proposed in [
Published:
, doi: 10.1088/1674-1137/ae5ef9
Abstract:
Accurate neutron capture cross section data are essential for validating nuclear models, understanding the origin of heavy elements, and improving reactor safety assessments. Measuring weakly absorbing nuclides at the milli-barn scale is challenging due to low-intensity signals, high-level environmental background, and sensitivity to target impurities. To investigate the capability of milli-barn scale neutron capture cross section measurement using the\begin{document}$\text{C}_6\text{D}_6$\end{document} \begin{document}$^{209}$\end{document} \begin{document}$(n, \gamma)$\end{document} \begin{document}$^{209}$\end{document} \begin{document}$\text{C}_6\text{D}_6$\end{document}
Accurate neutron capture cross section data are essential for validating nuclear models, understanding the origin of heavy elements, and improving reactor safety assessments. Measuring weakly absorbing nuclides at the milli-barn scale is challenging due to low-intensity signals, high-level environmental background, and sensitivity to target impurities. To investigate the capability of milli-barn scale neutron capture cross section measurement using the
Published:
, doi: 10.1088/1674-1137/ae5c84
Abstract:
We study the pre-inflationary evolution of the universe within the framework of loop quantum cosmology for a scalar field with potential\begin{document}$ V(\phi)=M^{4}\frac{\phi^{2}}{M_{Pl}^{2}}\left(1+\alpha\frac{\phi^{2}}{M_{Pl}^{2}}\right) $\end{document} \begin{document}$ n_s $\end{document}
We study the pre-inflationary evolution of the universe within the framework of loop quantum cosmology for a scalar field with potential
Published:
, doi: 10.1088/1674-1137/ae5dae
Abstract:
In the present work, new measurements of differential and angle-integrated cross sections for the 10B(n, α1)7Li*, 10B(n, α0)7Li and 10B(n, α)7Li reactions were performed at CSNS Back-n white neutron source. The Light-charged Particle Detector Array (LPDA) system was used to detect the charged particles. The 6Li-Si monitor was employed to measure the neutron flux. The differential cross sections for the 10B(n, α)7Li reaction were obtained from 20.2o to 158.7o (13 angles) in the neutron energy region from 0.3 eV to 3.0 MeV (70 energy points). The differential cross sections for the 10B(n, α0)7Li and 10B(n, α1)7Li* reactions were also obtained at the same angular positions in the neutron energy region from 0.3 eV to 1.0 MeV (65 energy points). Fitting with the Legendre polynomial series, the angle-integrated cross sections of these three reactions were obtained through integration. The experimental data for these three reactions across such a wide neutron energy range are valuable references for future nuclear data evaluations.
In the present work, new measurements of differential and angle-integrated cross sections for the 10B(n, α1)7Li*, 10B(n, α0)7Li and 10B(n, α)7Li reactions were performed at CSNS Back-n white neutron source. The Light-charged Particle Detector Array (LPDA) system was used to detect the charged particles. The 6Li-Si monitor was employed to measure the neutron flux. The differential cross sections for the 10B(n, α)7Li reaction were obtained from 20.2o to 158.7o (13 angles) in the neutron energy region from 0.3 eV to 3.0 MeV (70 energy points). The differential cross sections for the 10B(n, α0)7Li and 10B(n, α1)7Li* reactions were also obtained at the same angular positions in the neutron energy region from 0.3 eV to 1.0 MeV (65 energy points). Fitting with the Legendre polynomial series, the angle-integrated cross sections of these three reactions were obtained through integration. The experimental data for these three reactions across such a wide neutron energy range are valuable references for future nuclear data evaluations.
Published:
, doi: 10.1088/1674-1137/ae5a87
Abstract:
We investigate the discovery potential of the\begin{document}$T_{bc}$\end{document} \begin{document}$J^P = 0^+$\end{document} \begin{document}$pp$\end{document} \begin{document}$\sqrt{s} = 13~{\rm{TeV}}$\end{document} \begin{document}$T_{bc} \to B^- D^+$\end{document} \begin{document}${\mathtt{MadGraph5\_aMC@NLO}}$\end{document} \begin{document}${\mathtt{Pythia8.3}}$\end{document} \begin{document}$T_{bc}$\end{document} \begin{document}$\sigma_{{\rm{eff}}}$\end{document} \begin{document}$B D$\end{document} \begin{document}$5\sigma$\end{document} \begin{document}$T_{bc}$\end{document} \begin{document}$103~{\rm{nb}}$\end{document} \begin{document}$18~{\rm{nb}}$\end{document} \begin{document}$T_{cc}^+$\end{document} \begin{document}$0.3~{\rm{nb}}$\end{document} \begin{document}$5\sigma$\end{document} \begin{document}$103~{\rm{nb}}$\end{document} \begin{document}$18~{\rm{nb}}$\end{document} \begin{document}$300~{\rm{fb}}^{-1}$\end{document} \begin{document}$300~{\rm{fb}}^{-1}$\end{document} \begin{document}$\sigma(T_{bc}) \times {\cal{B}}(T_{bc} \to B^- D^+)$\end{document} \begin{document}$5\sigma$\end{document}
We investigate the discovery potential of the
Published:
, doi: 10.1088/1674-1137/ae5d27
Abstract:
Elemental fragmentation cross sections (EFCSs) of the\begin{document}$N=Z$\end{document} \begin{document}$^{36}$\end{document} \begin{document}$^{34}$\end{document} \begin{document}$^{32}$\end{document} \begin{document}$^{30}$\end{document} \begin{document}$^{28}$\end{document} \begin{document}$^{34}$\end{document} \begin{document}$^{30}$\end{document} \begin{document}$N=Z$\end{document} \begin{document}$\Delta Z$\end{document} \begin{document}$N=Z$\end{document}
Elemental fragmentation cross sections (EFCSs) of the
Published:
, doi: 10.1088/1674-1137/ae5c70
Abstract:
A sensitivity study of\begin{document}$ \bar{K}_1(1270) $\end{document} \begin{document}$ \bar{K}_1(1270) $\end{document} \begin{document}$ K^-\pi^+\pi^- $\end{document} \begin{document}$ K^-\pi^+\pi^0 $\end{document} \begin{document}$ K_S^0\pi^+\pi^- $\end{document} \begin{document}$ K_S^0\pi^-\pi^0 $\end{document} \begin{document}$ {\cal{B}}(\bar{K}_1(1270)\to \bar K\pi\pi) $\end{document}
A sensitivity study of
Published:
, doi: 10.1088/1674-1137/ae5d29
Abstract:
This paper systematically revisits the critical orbits of test particles in various black hole backgrounds, including Schwarzschild, Reissner–Nordströom, Kerr, and Kerr–Newman spacetimes. We identify the critical orbits directly from the root structure of the radial equation, and we provide explicit expressions that relate the relevant parameters—energy, angular momentum, and charge-to-mass ratio—to the critical radius, as well as explicit formulas for the critical orbits in each case. Special attention is given to the relationships among the photon spheres, black hole shadows, and critical null geodesics. We also present extensive numerical results.
This paper systematically revisits the critical orbits of test particles in various black hole backgrounds, including Schwarzschild, Reissner–Nordströom, Kerr, and Kerr–Newman spacetimes. We identify the critical orbits directly from the root structure of the radial equation, and we provide explicit expressions that relate the relevant parameters—energy, angular momentum, and charge-to-mass ratio—to the critical radius, as well as explicit formulas for the critical orbits in each case. Special attention is given to the relationships among the photon spheres, black hole shadows, and critical null geodesics. We also present extensive numerical results.
Published:
, doi: 10.1088/1674-1137/ae5884
Abstract:
Femtoscopy offers a sensitive probe of hadron emission sources and hadronic interactions. In this study, we examine relativistic corrections to scattering phase shifts and correlation functions using the two-body Dirac equation framework. We analyze the impact of the Darwin term and spin-dependent potentials, showing that these relativistic effects, especially spin-related interactions, significantly enhance the proton-proton correlation function. Our findings emphasize the necessity of including relativistic corrections for precise femtoscopic analyses.
Femtoscopy offers a sensitive probe of hadron emission sources and hadronic interactions. In this study, we examine relativistic corrections to scattering phase shifts and correlation functions using the two-body Dirac equation framework. We analyze the impact of the Darwin term and spin-dependent potentials, showing that these relativistic effects, especially spin-related interactions, significantly enhance the proton-proton correlation function. Our findings emphasize the necessity of including relativistic corrections for precise femtoscopic analyses.
Published:
, doi: 10.1088/1674-1137/ae5c7d
Abstract:
We develop a self-consistent nonlinear extension of diffusive shock acceleration that incorporates cosmic-ray (CR) backreaction on the shock precursor together with a physically motivated upstream escape mechanism that yields an exponential high-energy cutoff. The CR pressure gradient decelerates the upstream flow ahead of the shock, generating an extended precursor in which higher-rigidity particles sample a larger cumulative velocity gradient and thereby acquire a progressively harder spectrum. Finite-size and escape effects are modeled by a momentum-dependent loss term, which naturally terminates acceleration and steepens the spectrum near the cutoff. The precursor compression ratio is not imposed as a closure condition; instead, it is determined dynamically by enforcing consistency between the injection rate inferred from thermal leakage at the subshock and the injection strength required by the nonlinear shock modification, with CR-driven wave heating providing stabilizing negative feedback. Applying the model to young supernova-remnant–like parameters and standard one-zone Galactic diffusion, we reproduce the main features of the latest DAMPE proton spectrum: gradual hardening from hundreds of GeV to multi-TeV energies, followed by an exponential cutoff at tens of TeV. The resulting spectral evolution follows directly from the competition between precursor-mediated nonlinear feedback and upstream escape.
We develop a self-consistent nonlinear extension of diffusive shock acceleration that incorporates cosmic-ray (CR) backreaction on the shock precursor together with a physically motivated upstream escape mechanism that yields an exponential high-energy cutoff. The CR pressure gradient decelerates the upstream flow ahead of the shock, generating an extended precursor in which higher-rigidity particles sample a larger cumulative velocity gradient and thereby acquire a progressively harder spectrum. Finite-size and escape effects are modeled by a momentum-dependent loss term, which naturally terminates acceleration and steepens the spectrum near the cutoff. The precursor compression ratio is not imposed as a closure condition; instead, it is determined dynamically by enforcing consistency between the injection rate inferred from thermal leakage at the subshock and the injection strength required by the nonlinear shock modification, with CR-driven wave heating providing stabilizing negative feedback. Applying the model to young supernova-remnant–like parameters and standard one-zone Galactic diffusion, we reproduce the main features of the latest DAMPE proton spectrum: gradual hardening from hundreds of GeV to multi-TeV energies, followed by an exponential cutoff at tens of TeV. The resulting spectral evolution follows directly from the competition between precursor-mediated nonlinear feedback and upstream escape.
Published:
Abstract:
An analysis of experimental data on measurements of the resonant and fine structure of the β-decay strength function\begin{document}$S_{\beta}(E)$\end{document} \begin{document}$S_{\beta}(E)$\end{document} \begin{document}$S_{\beta}(E)$\end{document} \begin{document}$E_{\text {GTR}}{-}E_{\text {IAR}})$\end{document} \begin{document}$SU(4)$\end{document}
An analysis of experimental data on measurements of the resonant and fine structure of the β-decay strength function
Published:
, doi: 10.1088/1674-1137/ae4dd8
Abstract:
We investigate the propagating modes of New General Relativity (NGR) in second-order linear perturbations in the Lagrangian density (first-order in field equations). The Dirac-Bergmann analysis has revealed a violation of local Lorentz invariance in NGR. We review the recent status of NGR, considering the results of its Dirac-Bergmann analysis. We then reconsider the vierbein perturbation framework and identify the origin of each perturbation field in the vierbein field components. This identification is mandatory for adequately fixing gauges while guaranteeing consistency with the invariance ensured by the Dirac-Bergmann analysis. We find that the spatially flat gauge is adequate for analyzing a theory with the violation of local Lorentz invariance. Based on the established vierbein perturbative framework, introducing a real scalar field as matter, we perform a second-order perturbative analysis of NGR with respect to tensor, scalar, pseudo-scalar, and vector and pseudo-vector modes. We reveal the possible propagating modes of each type of NGR. In particular, we find that Type 3 has stable five propagating modes, i.e., tensor, scalar, and vector modes, compared to five non-linear degrees of freedom, which results in its Dirac-Bergmann analysis; The linear perturbation theory of Type 3 is preferable for applications to cosmology. Finally, we discuss our results in comparison to previous related work and conclude this study.
We investigate the propagating modes of New General Relativity (NGR) in second-order linear perturbations in the Lagrangian density (first-order in field equations). The Dirac-Bergmann analysis has revealed a violation of local Lorentz invariance in NGR. We review the recent status of NGR, considering the results of its Dirac-Bergmann analysis. We then reconsider the vierbein perturbation framework and identify the origin of each perturbation field in the vierbein field components. This identification is mandatory for adequately fixing gauges while guaranteeing consistency with the invariance ensured by the Dirac-Bergmann analysis. We find that the spatially flat gauge is adequate for analyzing a theory with the violation of local Lorentz invariance. Based on the established vierbein perturbative framework, introducing a real scalar field as matter, we perform a second-order perturbative analysis of NGR with respect to tensor, scalar, pseudo-scalar, and vector and pseudo-vector modes. We reveal the possible propagating modes of each type of NGR. In particular, we find that Type 3 has stable five propagating modes, i.e., tensor, scalar, and vector modes, compared to five non-linear degrees of freedom, which results in its Dirac-Bergmann analysis; The linear perturbation theory of Type 3 is preferable for applications to cosmology. Finally, we discuss our results in comparison to previous related work and conclude this study.
Published:
, doi: 10.1088/1674-1137/ae4a0c
Abstract:
We present an updated analysis of the angular distribution for\begin{document}$ \psi(3686) \to p\bar{p} $\end{document} \begin{document}$ 1+\alpha\cos^2\theta $\end{document} \begin{document}$ \psi(3686) $\end{document} \begin{document}$ \cos\theta $\end{document} \begin{document}$ \psi(3686)\to p\bar{p} $\end{document} \begin{document}$ \alpha = 1.00 \pm 0.03 $\end{document} \begin{document}$ \sin(2\phi) $\end{document}
We present an updated analysis of the angular distribution for
Published:
Abstract:
We performed a next-to-leading-order (NLO) QCD sum rules analysis of the\begin{document}$1^{-+}$\end{document} \begin{document}$1.7\,\text{GeV}$\end{document} \begin{document}$1^{-+}$\end{document} \begin{document}$2.0\,\text{GeV}$\end{document} \begin{document}$\pi_{1}(2015)$\end{document} \begin{document}$\pi_{1}(2015)$\end{document} \begin{document}$\pi_{1}(1400)$\end{document}
We performed a next-to-leading-order (NLO) QCD sum rules analysis of the
Published:
, doi: 10.1088/1674-1137/ae457a
Abstract:
In this paper, we investigate the quantum gravitational corrections to the thermodynamical quantities of Reissner-Nordstr?m black holes within the framework of effective field theory. The effective action originates from integrating out massless particles, including gravitons, at the one-loop level. We perform a complete thermodynamic analysis for both non-extremal and extremal black holes and are mainly concerned with the shift in the charge-to-mass ratio\begin{document}$ q/M$\end{document} \begin{document}$ q/M>1$\end{document}
In this paper, we investigate the quantum gravitational corrections to the thermodynamical quantities of Reissner-Nordstr?m black holes within the framework of effective field theory. The effective action originates from integrating out massless particles, including gravitons, at the one-loop level. We perform a complete thermodynamic analysis for both non-extremal and extremal black holes and are mainly concerned with the shift in the charge-to-mass ratio
Published:
Abstract:
This work examines the\begin{document}$ h\to Z\gamma $\end{document} \begin{document}$ h\to\gamma\gamma $\end{document} \begin{document}$ U(1)' $\end{document} \begin{document}$ Z' $\end{document} \begin{document}$ h \to Z\gamma $\end{document} \begin{document}$ f\bar{f}Z $\end{document} \begin{document}$ b\to s\ell^+\ell^- $\end{document} \begin{document}$ m_{H^\pm}>200 $\end{document} \begin{document}$ \lambda_{hH^+H^-}<0 $\end{document} \begin{document}$ 1\sigma $\end{document} \begin{document}$ \mu_{\gamma\gamma} $\end{document} \begin{document}$ f\bar{f}Z $\end{document} \begin{document}$ \mathcal{Q}_{tL} $\end{document} \begin{document}$ \mathcal{Q}_{tR} $\end{document} \begin{document}$ b\to s\ell^+\ell^- $\end{document} \begin{document}$ 14\% $\end{document} \begin{document}$ \mu_{Z\gamma} $\end{document}
This work examines the
Published:
Abstract:
We investigate a negative potential-induced scalarization of the Einstein-Euler-Heisenberg (EEH) black hole in the EEH-scalar theory, characterized by mass M, Euler-Heisenberg parameter μ and magnetic charge q. In the regime\begin{document}$ \mu>\mu_{{\rm{max}}} = 0.019 $\end{document} \begin{document}$ M=1/2 $\end{document} \begin{document}$ q/M \gt 1 $\end{document} \begin{document}$ q>0 $\end{document} \begin{document}$ q<1/2 $\end{document} \begin{document}$ q>1/2 $\end{document}
We investigate a negative potential-induced scalarization of the Einstein-Euler-Heisenberg (EEH) black hole in the EEH-scalar theory, characterized by mass M, Euler-Heisenberg parameter μ and magnetic charge q. In the regime
Published:
Abstract:
In this study, we investigate the dynamics of test particles in the spacetime of a static, spherically symmetric black hole (BH), illustrated within the non-local gravity models. In this case, after presenting the BH geometries and horizon structures, we examine the motion of particles by analyzing the effective potential, the innermost stable circular orbits (ISCOs), and the corresponding effective force. Also, we then extend the study to small perturbations of circular orbits, exploring harmonic oscillations characterized by the frequencies measured both by local observers and by distant ones, as well as the periastron precession effects. Particular attention is devoted to the interplay between the non-local gravity corrections and the stability properties of geodesics. In this case, we analyze the center-of-mass energy (CME) of colliding particles near the event horizon and show the influence of BH parameters on energy extraction processes. In this context, the results show how non-local modifications of gravity affect the standard predictions of BH structure, orbital stability, and high-energy particle dynamics, with possible implications for astrophysical observations and theoretical models of strong gravity. This study examines the differences between the inverse electrodynamics BH and the Schwarzschild BH configuration, showing how additional parameters influence the dynamics and stability of the test particles.
In this study, we investigate the dynamics of test particles in the spacetime of a static, spherically symmetric black hole (BH), illustrated within the non-local gravity models. In this case, after presenting the BH geometries and horizon structures, we examine the motion of particles by analyzing the effective potential, the innermost stable circular orbits (ISCOs), and the corresponding effective force. Also, we then extend the study to small perturbations of circular orbits, exploring harmonic oscillations characterized by the frequencies measured both by local observers and by distant ones, as well as the periastron precession effects. Particular attention is devoted to the interplay between the non-local gravity corrections and the stability properties of geodesics. In this case, we analyze the center-of-mass energy (CME) of colliding particles near the event horizon and show the influence of BH parameters on energy extraction processes. In this context, the results show how non-local modifications of gravity affect the standard predictions of BH structure, orbital stability, and high-energy particle dynamics, with possible implications for astrophysical observations and theoretical models of strong gravity. This study examines the differences between the inverse electrodynamics BH and the Schwarzschild BH configuration, showing how additional parameters influence the dynamics and stability of the test particles.
Published:
, doi: 10.1088/1674-1137/ae4578
Abstract:
Two\begin{document}$ 7\alpha $\end{document} \begin{document}$ ^{28}\mathrm{Si} $\end{document} \begin{document}$ ^{28}\mathrm{Si} $\end{document}
Two
Published:
, doi: 10.1088/1674-1137/ae5ef5
Abstract:
Identifying the thermodynamic conditions marking the onset of fission cycling is crucial for modeling heavy-element production in the r-process. In this work, we develop a framework to determine this onset over the\begin{document}$ (T_9, n_n) $\end{document} \begin{document}$ N \approx 184 $\end{document} \begin{document}$ S_n^{0}(T_9, n_n) $\end{document} \begin{document}$ 94 \leqslant Z \leqslant 106 $\end{document}
Identifying the thermodynamic conditions marking the onset of fission cycling is crucial for modeling heavy-element production in the r-process. In this work, we develop a framework to determine this onset over the
Published:
, doi: 10.1088/1674-1137/ae62f8
Abstract:
In this work, we focus on the possible linear relationship between short-range correlations (SRCs) and the EMC effect for partons in nuclei. First, we test a linear relationship pertaining to gluons in bound nuclei; it is manifested as a correlation between the slope of the reduced cross-section ratio in deep inelastic scattering (DIS) and the cross-section of sub-threshold\begin{document}$ J/\psi $\end{document}
In this work, we focus on the possible linear relationship between short-range correlations (SRCs) and the EMC effect for partons in nuclei. First, we test a linear relationship pertaining to gluons in bound nuclei; it is manifested as a correlation between the slope of the reduced cross-section ratio in deep inelastic scattering (DIS) and the cross-section of sub-threshold
Published:
, doi: 10.1088/1674-1137/ae5c6f
Abstract:
The Large Array of imaging atmospheric Cherenkov Telescopes (LACT) is a next-generation Cherenkov telescope array designed to study the morphology and energy spectra of ultra-high-energy gamma-ray sources in hybrid operation with the Large High Altitude Air Shower Observatory (LHAASO). With its excellent angular resolution, large effective area, and powerful gamma/hadron discrimination capabilities, LACT achieves outstanding sensitivity for observations of gamma-ray sources In this paper, we present an optimized configuration for the LACT array, developed through comprehensive Monte Carlo simulations. Based on these simulations, we conducted on-site surveys at the LHAASO site and selected the most effective array layout. Detailed performance studies show that this optimized configuration delivers excellent sensitivity across various observational modes. Furthermore, we present a detailed outlook on LACT's potential observations of gamma-ray sources in the LHAASO catalog. By incorporating the measured energy spectra from LHAASO and accounting for LACT's detector response function at different zenith angles, we estimate the number of detectable events over a one-year observation period. This analysis provides a foundation for developing a preliminary observation strategy for LACT in the coming years.
The Large Array of imaging atmospheric Cherenkov Telescopes (LACT) is a next-generation Cherenkov telescope array designed to study the morphology and energy spectra of ultra-high-energy gamma-ray sources in hybrid operation with the Large High Altitude Air Shower Observatory (LHAASO). With its excellent angular resolution, large effective area, and powerful gamma/hadron discrimination capabilities, LACT achieves outstanding sensitivity for observations of gamma-ray sources In this paper, we present an optimized configuration for the LACT array, developed through comprehensive Monte Carlo simulations. Based on these simulations, we conducted on-site surveys at the LHAASO site and selected the most effective array layout. Detailed performance studies show that this optimized configuration delivers excellent sensitivity across various observational modes. Furthermore, we present a detailed outlook on LACT's potential observations of gamma-ray sources in the LHAASO catalog. By incorporating the measured energy spectra from LHAASO and accounting for LACT's detector response function at different zenith angles, we estimate the number of detectable events over a one-year observation period. This analysis provides a foundation for developing a preliminary observation strategy for LACT in the coming years.
Published:
, doi: 10.1088/1674-1137/ae50e5
Abstract:
In this current work, we shed light on the unified approach to both dark energy and dark matter via the generalized Chaplygin gas model in symmetric teleparallel gravity (STGR). We have employed the equation of state provided by the generalized Chaplygin gas, which naturally arises in string theory, tachyonic field theory, and Randall-Sundrum type brane world solutions. We show that such a generalized Chaplygin gas can not only provide a lucrative candidate for dark energy but also a viable candidate for dark matter via Bose-Einstein Condensation (BEC). We have also taken into account the interaction between dark matter and dark energy to provide a more realistic perspective. We performed MCMC analysis with combined Hubble and Pantheon data sets. We have also performed the Om diagnostics and the\begin{document}$ r-s $\end{document}
In this current work, we shed light on the unified approach to both dark energy and dark matter via the generalized Chaplygin gas model in symmetric teleparallel gravity (STGR). We have employed the equation of state provided by the generalized Chaplygin gas, which naturally arises in string theory, tachyonic field theory, and Randall-Sundrum type brane world solutions. We show that such a generalized Chaplygin gas can not only provide a lucrative candidate for dark energy but also a viable candidate for dark matter via Bose-Einstein Condensation (BEC). We have also taken into account the interaction between dark matter and dark energy to provide a more realistic perspective. We performed MCMC analysis with combined Hubble and Pantheon data sets. We have also performed the Om diagnostics and the
Published:
Abstract:
Experiments with the 48Ca and 54Cr induced reactions were performed at the gas-filled recoil separator SHANS2 (Spectrometer for Heavy Atoms and Nuclear Structure-2) of the China Accelerator Facility for superheavy Elements (CAFE2). The isotopic distributions of nuclei produced in the reactions 48Ca +243 Am, 54Cr +243 Am, and 54Cr +238 U were investigated. Bombardments were conducted at the energies near the respective Coulomb barriers, with the SHANS2 magnetic rigidities set to collect fusion-evaporation residues. α-decay spectroscopy was employed to identify products, revealing 58 different isotopes in these experiments. The analysis indicates that the distribution of nuclides produced in different reactions exhibits clear systematic trends. Based on their mass distributions, these nuclei were attributed to the products from the quasi-fission (QF) process. In addition, several short-lived fission events were identified and attributed to the fission isomers near the target.
Experiments with the 48Ca and 54Cr induced reactions were performed at the gas-filled recoil separator SHANS2 (Spectrometer for Heavy Atoms and Nuclear Structure-2) of the China Accelerator Facility for superheavy Elements (CAFE2). The isotopic distributions of nuclei produced in the reactions 48Ca +243 Am, 54Cr +243 Am, and 54Cr +238 U were investigated. Bombardments were conducted at the energies near the respective Coulomb barriers, with the SHANS2 magnetic rigidities set to collect fusion-evaporation residues. α-decay spectroscopy was employed to identify products, revealing 58 different isotopes in these experiments. The analysis indicates that the distribution of nuclides produced in different reactions exhibits clear systematic trends. Based on their mass distributions, these nuclei were attributed to the products from the quasi-fission (QF) process. In addition, several short-lived fission events were identified and attributed to the fission isomers near the target.
Published:
Abstract:
We extract the non-perturbative Heavy Quark Effective Theory (HQET) parameters from the inclusive semi-leptonic decay\begin{document}$ \Lambda_c^+ \to X e^+ \nu_e $\end{document} \begin{document}$ \Lambda_c^+ $\end{document} \begin{document}$ e^+e^- $\end{document} \begin{document}$ \Lambda_c^+ $\end{document} \begin{document}$ \Lambda_c^+ $\end{document} \begin{document}$ \mu_\pi^2(\Lambda_c^+) $\end{document} \begin{document}$ \rho_D^3(\Lambda_c^+) $\end{document}
We extract the non-perturbative Heavy Quark Effective Theory (HQET) parameters from the inclusive semi-leptonic decay
Published:
Abstract:
We investigate the steady, axisymmetric, force-free magnetosphere of Kerr–Sen black hole (BH) within the framework of the Einstein–Maxwell–dilaton–axion (EMDA) theory. By perturbatively solving the nonlinear Grad–Shafranov (GS) equation, we determine the magnetic field configuration and quantify the influence of the dilaton parameter r2 on the energy extraction rate and radiative efficiency. Our results show that both the energy extraction power and the radiative efficiency increase with r2, exceeding those of the standard Kerr BH, whereas the extraction efficiency remain consistent with the Kerr case. In addition, we perform χ2 statistical analysis using observational data from six binary BH systems, which indicates that the Kerr BH currently provides a better fit for bulk Lorentz factors Γ = 2 and 5.
We investigate the steady, axisymmetric, force-free magnetosphere of Kerr–Sen black hole (BH) within the framework of the Einstein–Maxwell–dilaton–axion (EMDA) theory. By perturbatively solving the nonlinear Grad–Shafranov (GS) equation, we determine the magnetic field configuration and quantify the influence of the dilaton parameter r2 on the energy extraction rate and radiative efficiency. Our results show that both the energy extraction power and the radiative efficiency increase with r2, exceeding those of the standard Kerr BH, whereas the extraction efficiency remain consistent with the Kerr case. In addition, we perform χ2 statistical analysis using observational data from six binary BH systems, which indicates that the Kerr BH currently provides a better fit for bulk Lorentz factors Γ = 2 and 5.
Published:
, doi: 10.1088/1674-1137/ad8ec2
Abstract:
The direct CP asymmetry in the weak decay process of hadrons is commonly attributed to the weak phase of the CKM matrix and the indeterminate strong phase. We propose a method to generate a significant phase difference through the interference between ρ and ω mesons, taking into account the G-parity allowed decay process of\begin{document}$\omega \rightarrow \pi^{+}\pi^{-}\pi^{0}$\end{document} ![]()
![]()
\begin{document}$\rho^{0} \rightarrow \pi^{+}\pi^{-}\pi^{0}$\end{document} ![]()
![]()
The direct CP asymmetry in the weak decay process of hadrons is commonly attributed to the weak phase of the CKM matrix and the indeterminate strong phase. We propose a method to generate a significant phase difference through the interference between ρ and ω mesons, taking into account the G-parity allowed decay process of
IF: 3.1
Monthly issued, founded in 1977
Sponsored by:
ISSN 1674-1137 CN 11-5641/O4
Original research articles, Ietters and reviews Covering theory and experiments in the fieids of
- Particle physics
- Nuclear physics
- Particle and nuclear astrophysics
- Cosmology
Author benefits
- A SCOAP3 participating journal - free Open Access publication for qualifying articles
- Average 24 days to first decision
- Fast-track publication for selected articles
- Subscriptions at over 3000 institutions worldwide
- Free English editing on all accepted articles
News
- CPC Announces 2025 Outstanding Reviewers
- Chinese Physics C Outstanding Reviewer Award 2023
- Impact factor of Chinese Physics C is 3.6 in 2022
- 2022 CPC Outstanding Reviewer Awards
- The 2023 Chinese New Year-Office closure
Cover Story
- Cover Story (Issue 4, 2026): Initial performance results of the JUNO detector
- Cover Story (Issue 3, 2026): Comprehensive investigation on baryon number violating nucleon decays involving an axion-like particle
- Cover Story (Issue 2, 2026) |The images of Brans-Dicke-Kerr type naked singularities
- Cover Story (Issue 1, 2026) A focused review of quintom cosmology: from quintom dark energy to quintom bounce
- Cover Story (Issue 11, 2025) The Earth-Magnet Assists DAMPE in Studying Cosmic Anti-Electrons
Advertising
