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Published:
, doi: 10.1088/1674-1137/ae66d0
Abstract:
In this paper, we analyze the dynamics of test particles in a Kalb-Ramond black hole (BH) spacetime coupled to nonlinear electrodynamics. After explicitly constructing the corresponding BH metric, including the nonlinear electromagnetic contributions to the geometry, we study the geodesic equations, focusing on the effective potential, the innermost stable circular orbits (ISCOs), and test-particle trajectories. This provides a quantitative description of orbital motion under the combined gravitational, Kalb-Ramond, and nonlinear electromagnetic effects. We then examine small perturbations of circular geodesics and derive the associated epicyclic frequencies for local and distant observers. These results show how the Kalb-Ramond field and nonlinear electrodynamics influence orbital stability, quasi-periodic oscillations (QPOs), and possible high-energy astrophysical signatures. Next, we numerically model Bondi-Hoyle-Lyttleton (BHL) accretion onto Kalb-Ramond BHs to assess how spacetime parameters affect flow morphology and dynamics. As the deformation parameters increase, the shock cone becomes more collimated, the stagnation point moves closer to the event horizon, and the matter density inside the cone decreases. For small deformations, QPO frequencies exhibit systematic shifts with enhanced oscillation amplitudes, whereas strong deformations damp the oscillations and produce a smooth, quasi-steady accretion rate. In this way, we illustrate a direct connection between spacetime geometry, shock-cone structure, and accretion variability, demonstrating that accretion dynamics serve as a sensitive probe of Kalb-Ramond BH spacetimes.
In this paper, we analyze the dynamics of test particles in a Kalb-Ramond black hole (BH) spacetime coupled to nonlinear electrodynamics. After explicitly constructing the corresponding BH metric, including the nonlinear electromagnetic contributions to the geometry, we study the geodesic equations, focusing on the effective potential, the innermost stable circular orbits (ISCOs), and test-particle trajectories. This provides a quantitative description of orbital motion under the combined gravitational, Kalb-Ramond, and nonlinear electromagnetic effects. We then examine small perturbations of circular geodesics and derive the associated epicyclic frequencies for local and distant observers. These results show how the Kalb-Ramond field and nonlinear electrodynamics influence orbital stability, quasi-periodic oscillations (QPOs), and possible high-energy astrophysical signatures. Next, we numerically model Bondi-Hoyle-Lyttleton (BHL) accretion onto Kalb-Ramond BHs to assess how spacetime parameters affect flow morphology and dynamics. As the deformation parameters increase, the shock cone becomes more collimated, the stagnation point moves closer to the event horizon, and the matter density inside the cone decreases. For small deformations, QPO frequencies exhibit systematic shifts with enhanced oscillation amplitudes, whereas strong deformations damp the oscillations and produce a smooth, quasi-steady accretion rate. In this way, we illustrate a direct connection between spacetime geometry, shock-cone structure, and accretion variability, demonstrating that accretion dynamics serve as a sensitive probe of Kalb-Ramond BH spacetimes.
Published:
, doi: 10.1088/1674-1137/ae662e
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This paper primarily investigates the optical properties of two minimal deformations of the Schwarzschild black hole—the Kazakov-Solodukhin and Ghosh-Kumar black holes—under different accretion models. The event horizon, photon sphere, and critical impact parameter of the former increase relative to the Schwarzschild case, whereas those of the latter decrease. Data from the Event Horizon Telescope Collaboration are used to constrain the parameter ranges of the two black holes. Under spherical accretion, the quantum correction of the Kazakov-Solodukhin black hole enlarges the black hole shadow and reduces the integrated intensity, while the shadow of the magnetically charged Ghosh-Kumar black hole shrinks and the integrated intensity increases. The black hole’s shadow radius is independent of the choice of spherical accretion model. For an optically and geometrically thin accretion disk, the integrated intensity is dominated by direct emission, with photon-ring and lensed-ring contributions being negligible. In addition, the photon and lensed rings of the Kazakov-Solodukhin black hole are narrower, whereas those of the Ghosh-Kumar black hole are broader. Whereas the Kazakov-Solodukhin black hole is brighter, the Ghosh-Kumar black hole is dimmer. Additionally, bringing the disk closer to the black hole yields a smaller shadow radius. This paper proposes a method to distinguish different black holes within a specific thin-disk model.
This paper primarily investigates the optical properties of two minimal deformations of the Schwarzschild black hole—the Kazakov-Solodukhin and Ghosh-Kumar black holes—under different accretion models. The event horizon, photon sphere, and critical impact parameter of the former increase relative to the Schwarzschild case, whereas those of the latter decrease. Data from the Event Horizon Telescope Collaboration are used to constrain the parameter ranges of the two black holes. Under spherical accretion, the quantum correction of the Kazakov-Solodukhin black hole enlarges the black hole shadow and reduces the integrated intensity, while the shadow of the magnetically charged Ghosh-Kumar black hole shrinks and the integrated intensity increases. The black hole’s shadow radius is independent of the choice of spherical accretion model. For an optically and geometrically thin accretion disk, the integrated intensity is dominated by direct emission, with photon-ring and lensed-ring contributions being negligible. In addition, the photon and lensed rings of the Kazakov-Solodukhin black hole are narrower, whereas those of the Ghosh-Kumar black hole are broader. Whereas the Kazakov-Solodukhin black hole is brighter, the Ghosh-Kumar black hole is dimmer. Additionally, bringing the disk closer to the black hole yields a smaller shadow radius. This paper proposes a method to distinguish different black holes within a specific thin-disk model.
Published:
, doi: 10.1088/1674-1137/ae68ed
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We constructed a four-Higgs-doublet model (4HDM) invariant under D5 symmetry and investigated its complete neutral vacuum structure in detail. Assuming explicit CP conservation in the scalar potential, we examined whether CP symmetry can be spontaneously broken. We provided a complete list of all possible real and complex vacua, along with the constraints on the potential parameters required for each vacuum solution to exist. We also discussed the positive-definiteness conditions that the Hessian must satisfy for each vacuum to be a local minimum of the potential. The results show that, after spontaneous symmetry breaking, some complex vacua lead to spontaneous CP violation in the potential, whereas the remaining complex vacua still preserve CP conservation. Among these CP-violating complex vacua, one can be regarded as the most general form. Furthermore, we discussed the relationship between real and complex vacua.
We constructed a four-Higgs-doublet model (4HDM) invariant under D5 symmetry and investigated its complete neutral vacuum structure in detail. Assuming explicit CP conservation in the scalar potential, we examined whether CP symmetry can be spontaneously broken. We provided a complete list of all possible real and complex vacua, along with the constraints on the potential parameters required for each vacuum solution to exist. We also discussed the positive-definiteness conditions that the Hessian must satisfy for each vacuum to be a local minimum of the potential. The results show that, after spontaneous symmetry breaking, some complex vacua lead to spontaneous CP violation in the potential, whereas the remaining complex vacua still preserve CP conservation. Among these CP-violating complex vacua, one can be regarded as the most general form. Furthermore, we discussed the relationship between real and complex vacua.
Published:
, doi: 10.1088/1674-1137/ae662f
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We develop a framework for the formation of exotic muonic kaon atoms (\begin{document}$ K\mu $\end{document} \begin{document}$ D^{0} $\end{document} \begin{document}$ \mathrm{BR}(D^{0} \to(K\mu )\nu_{\mu})=2.29\times10^{-10} $\end{document} \begin{document}$ K\mu $\end{document} \begin{document}$ D^{0} $\end{document} \begin{document}$ p+p $\end{document} \begin{document}$ K\mu $\end{document}
We develop a framework for the formation of exotic muonic kaon atoms (
Published:
, doi: 10.1088/1674-1137/ae662d
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We explore the interplay between the magnetic field and non-extensivity in shaping the complex heavy-quark potential in the quark-gluon plasma via the dielectric permittivity. Within the real-time formalism with hard-thermal-loop resummation, we determine the non-extensive corrections to the gluon self-energy and the resummed gluon propagator in the Keldysh representation, and we apply these results to compute the medium's dielectric permittivity. Our study shows that increases in the magnetic field and in non-extensivity enhance screening and flatten the real part of the potential, whereas they affect the imaginary part in opposite ways. When the gluon-loop contribution to the gluon self-energy is excluded, the imaginary part of the potential exhibits pronounced anisotropy in the presence of a magnetic field, especially at small quark-antiquark separations, while non-extensivity can weaken this anisotropy. When the gluon-loop contribution is included, the degree of anisotropy of the imaginary part of the potential is largely reduced and becomes nearly insensitive to non-extensive effects. These results pave the way for further studies of the properties of heavy quarkonia in a magnetized, non-extensive quark-gluon plasma.
We explore the interplay between the magnetic field and non-extensivity in shaping the complex heavy-quark potential in the quark-gluon plasma via the dielectric permittivity. Within the real-time formalism with hard-thermal-loop resummation, we determine the non-extensive corrections to the gluon self-energy and the resummed gluon propagator in the Keldysh representation, and we apply these results to compute the medium's dielectric permittivity. Our study shows that increases in the magnetic field and in non-extensivity enhance screening and flatten the real part of the potential, whereas they affect the imaginary part in opposite ways. When the gluon-loop contribution to the gluon self-energy is excluded, the imaginary part of the potential exhibits pronounced anisotropy in the presence of a magnetic field, especially at small quark-antiquark separations, while non-extensivity can weaken this anisotropy. When the gluon-loop contribution is included, the degree of anisotropy of the imaginary part of the potential is largely reduced and becomes nearly insensitive to non-extensive effects. These results pave the way for further studies of the properties of heavy quarkonia in a magnetized, non-extensive quark-gluon plasma.
Published:
, doi: 10.1088/1674-1137/ae6633
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The proton drip-line marks the limiting location where the proton binding energy vanishes. Ground-state proton emission is a signature of having crossed this drip line. We determine the locations of the proton drip-line for odd-Z nuclei along isotopic chains toward the neutron-deficient side, based on experimentally measured nuclear masses and proton emission half-lives. The odd-odd characteristics and a plateau at\begin{document}$N = Z$\end{document} \begin{document}$33 \leq Z \leq 47$\end{document}
The proton drip-line marks the limiting location where the proton binding energy vanishes. Ground-state proton emission is a signature of having crossed this drip line. We determine the locations of the proton drip-line for odd-Z nuclei along isotopic chains toward the neutron-deficient side, based on experimentally measured nuclear masses and proton emission half-lives. The odd-odd characteristics and a plateau at
Published:
, doi: 10.1088/1674-1137/ae68ee
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The Belle Collaboration has recently reported a measurement of the branching fraction for the semileptonic decay\begin{document}$ B^{-}\to\pi^{+}\pi^{-}\ell^{-}\bar\nu_\ell $\end{document} \begin{document}$ \ell=e $\end{document} \begin{document}$ \pi\pi $\end{document} \begin{document}$ B\to\pi\pi $\end{document} \begin{document}$ {\cal B}_N(B^{-}\to\pi^{+}\pi^{-}\ell^{-}\bar\nu_\ell)=(3.5\pm 1.4^{+4.3}_{-2.4})\times 10^{-5} $\end{document}
The Belle Collaboration has recently reported a measurement of the branching fraction for the semileptonic decay
Published:
, doi: 10.1088/1674-1137/ae66d3
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In this study, by utilizing the constructed generalized free energy alongside the Mean First-Passage Time and the Kramers escape rate from stochastic dynamics, we have obtained a comprehensive landscape of the phase transitions for the Bardeen-AdS-class black hole. This black hole model admits two distinct categories of solutions. Type I black holes feature a regular black hole solution, while Type II black holes possess a vacuum state solution. In the phase transition between the small black hole and the large black hole for Type I, the process may pass through a stable, metastable, or unstable regular black hole as an intermediate state. In contrast, for Type II black holes, the phase transition occurs exclusively between the vacuum state and the small black hole, and the transition process does not involve any regular black hole intermediate states.
In this study, by utilizing the constructed generalized free energy alongside the Mean First-Passage Time and the Kramers escape rate from stochastic dynamics, we have obtained a comprehensive landscape of the phase transitions for the Bardeen-AdS-class black hole. This black hole model admits two distinct categories of solutions. Type I black holes feature a regular black hole solution, while Type II black holes possess a vacuum state solution. In the phase transition between the small black hole and the large black hole for Type I, the process may pass through a stable, metastable, or unstable regular black hole as an intermediate state. In contrast, for Type II black holes, the phase transition occurs exclusively between the vacuum state and the small black hole, and the transition process does not involve any regular black hole intermediate states.
Published:
, doi: 10.1088/1674-1137/ae6631
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We develop a framework for calculating nucleon-deuteron scattering using the Faddeev equations, employing strict perturbation theory to treat subleading interactions in chiral effective field theory (ChEFT). Rather than evaluating the distorted-wave expansion directly, our approach solves a hierarchy of integral equations to obtain subleading scattering amplitudes. We benchmark the method against the wave-packet continuum discretization. This framework benefits from the fact that renormalization-group-invariant chiral forces involve only a limited number of two-body partial waves at leading order. We use it to calculate differential cross sections and analyzing powers for nucleon-deuteron elastic scattering up to next-to-leading order.
We develop a framework for calculating nucleon-deuteron scattering using the Faddeev equations, employing strict perturbation theory to treat subleading interactions in chiral effective field theory (ChEFT). Rather than evaluating the distorted-wave expansion directly, our approach solves a hierarchy of integral equations to obtain subleading scattering amplitudes. We benchmark the method against the wave-packet continuum discretization. This framework benefits from the fact that renormalization-group-invariant chiral forces involve only a limited number of two-body partial waves at leading order. We use it to calculate differential cross sections and analyzing powers for nucleon-deuteron elastic scattering up to next-to-leading order.
Published:
, doi: 10.1088/1674-1137/ae66d1
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In the present work, the strong decays of the discovered\begin{document}$ P_c(4380) $\end{document} \begin{document}$ P_c(4440) $\end{document} \begin{document}$ P_c(4457) $\end{document} \begin{document}$ P_c(4380) $\end{document} \begin{document}$ P_c(4440) $\end{document} \begin{document}$ P_c(4457) $\end{document} \begin{document}$ P_c $\end{document}
In the present work, the strong decays of the discovered
Published:
, doi: 10.1088/1674-1137/ae6310
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Hadron-hadron interactions, being nonperturbative in nature, play a significant role in addressing phenomenological questions in particle physics. Femtoscopy is a powerful tool in heavy-ion collision experiments, enabling the extraction of hadron-hadron interactions via momentum-correlation functions (CFs). These CFs are typically expressed as a convolution of source functions and hadron-hadron wave functions, with the latter encoding information about the interactions. However, source functions remain poorly constrained and are commonly approximated by a Gaussian form. Reconstructing source functions from experimental correlation data constitutes an "inverse problem." To address this, we propose a toy model based on Tikhonov regularization. Using a square-well potential with four distinct strengths, we calculate the CFs for inputs of a Gaussian source function and its mixed form. The resulting CFs are then used to reconstruct the source functions via Tikhonov regularization. Our results show that the Gaussian source function can be successfully reconstructed, highlighting the potential of this approach for extracting realistic source functions from hadron pairs of interest.
Hadron-hadron interactions, being nonperturbative in nature, play a significant role in addressing phenomenological questions in particle physics. Femtoscopy is a powerful tool in heavy-ion collision experiments, enabling the extraction of hadron-hadron interactions via momentum-correlation functions (CFs). These CFs are typically expressed as a convolution of source functions and hadron-hadron wave functions, with the latter encoding information about the interactions. However, source functions remain poorly constrained and are commonly approximated by a Gaussian form. Reconstructing source functions from experimental correlation data constitutes an "inverse problem." To address this, we propose a toy model based on Tikhonov regularization. Using a square-well potential with four distinct strengths, we calculate the CFs for inputs of a Gaussian source function and its mixed form. The resulting CFs are then used to reconstruct the source functions via Tikhonov regularization. Our results show that the Gaussian source function can be successfully reconstructed, highlighting the potential of this approach for extracting realistic source functions from hadron pairs of interest.
Published:
, doi: 10.1088/1674-1137/ae6632
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In this study, we investigate the accretion dynamics and test particle motion around a non-rotating, spherically symmetric Lee-Wick black hole (BH) to reveal how the model parameters affect orbital stability and the quasi-periodic oscillations (QPOs) observed in X-ray binary systems. In this work, we deliberately explore parameter values both within the admissible region defined by\begin{document}$ S_2 \gt 0 $\end{document} \begin{document}$ -2\sqrt{S_2} \lt S_1 \lt 2\sqrt{S_2} $\end{document} \begin{document}$ S_1 $\end{document} \begin{document}$ S_2 $\end{document} \begin{document}$ S_1 $\end{document} \begin{document}$ S_2 $\end{document}
In this study, we investigate the accretion dynamics and test particle motion around a non-rotating, spherically symmetric Lee-Wick black hole (BH) to reveal how the model parameters affect orbital stability and the quasi-periodic oscillations (QPOs) observed in X-ray binary systems. In this work, we deliberately explore parameter values both within the admissible region defined by
Published:
, doi: 10.1088/1674-1137/ae66d2
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This article delves into the observational properties of a Schwarzschild-like black hole (BH). Initially, the research provides a succinct examination of the spacetime geometry and the configuration of its horizon. Furthermore, we study the photon dynamics around the Schwarzschild-like BH in the presence of plasma using the Hamiltonian formalism. We found that the photon sphere radii increase under the influence of plasma frequency and vice versa for the spacetime parameters. Further exploration is dedicated to understanding how plasma affects the shadow of the BH, and we find that the radius of the BH shadow shrinks with the rise of the ξ parameter and plasma frequency. We then turn to constraining the spacetime parameters and the plasma frequency by using the observational data released by the Event Horizon Telescope (EHT) collaboration for M87* and Sgr A*. Additionally, the research scrutinizes the phenomenon of gravitational weak lensing in the vicinity of a Schwarzschild-like BH, considering both uniform and non-uniform plasma scenarios. The outcomes demonstrate that the angle of deflection increases under the influence of a uniform plasma frequency, whereas the opposite is true for non-uniform plasma. In both scenarios, a rise in the spacetime parameters results in a decrease in the deflection angle. Finally, we investigate the magnification of the gravitationally lensed image. The effect of the spacetime parameters and plasma frequencies on the total magnification is the same as in the deflection angles.
This article delves into the observational properties of a Schwarzschild-like black hole (BH). Initially, the research provides a succinct examination of the spacetime geometry and the configuration of its horizon. Furthermore, we study the photon dynamics around the Schwarzschild-like BH in the presence of plasma using the Hamiltonian formalism. We found that the photon sphere radii increase under the influence of plasma frequency and vice versa for the spacetime parameters. Further exploration is dedicated to understanding how plasma affects the shadow of the BH, and we find that the radius of the BH shadow shrinks with the rise of the ξ parameter and plasma frequency. We then turn to constraining the spacetime parameters and the plasma frequency by using the observational data released by the Event Horizon Telescope (EHT) collaboration for M87* and Sgr A*. Additionally, the research scrutinizes the phenomenon of gravitational weak lensing in the vicinity of a Schwarzschild-like BH, considering both uniform and non-uniform plasma scenarios. The outcomes demonstrate that the angle of deflection increases under the influence of a uniform plasma frequency, whereas the opposite is true for non-uniform plasma. In both scenarios, a rise in the spacetime parameters results in a decrease in the deflection angle. Finally, we investigate the magnification of the gravitationally lensed image. The effect of the spacetime parameters and plasma frequencies on the total magnification is the same as in the deflection angles.
Published:
, doi: 10.1088/1674-1137/ae643d
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We investigate the intrinsic distributions of key Gamma-Ray Burst (GRB) parameters that are essential to understanding the physics of their central engines, radiation mechanisms, and cosmological evolution. Using our independently developed GodEyes Monte Carlo framework, we generate synthetic long-GRB samples tailored to the Swift/BAT detector and explicitly incorporate instrumental selection effects. In particular, we account for the loss of low-peak-flux events due to the detector's sensitivity threshold, thereby enabling consistent comparisons between theoretical models and observations. Our results constrain the intrinsic distributions of several fundamental properties, including redshift, peak luminosity, isotropic energy, and related quantities. We find that the inferred intrinsic distribution of the spectral index\begin{document}$ \alpha^{\rm{PL}}$\end{document}
We investigate the intrinsic distributions of key Gamma-Ray Burst (GRB) parameters that are essential to understanding the physics of their central engines, radiation mechanisms, and cosmological evolution. Using our independently developed GodEyes Monte Carlo framework, we generate synthetic long-GRB samples tailored to the Swift/BAT detector and explicitly incorporate instrumental selection effects. In particular, we account for the loss of low-peak-flux events due to the detector's sensitivity threshold, thereby enabling consistent comparisons between theoretical models and observations. Our results constrain the intrinsic distributions of several fundamental properties, including redshift, peak luminosity, isotropic energy, and related quantities. We find that the inferred intrinsic distribution of the spectral index
Published:
, doi: 10.1088/1674-1137/ae6311
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The exploration of symmetry laws stands as a cutting-edge direction in modern physics research. This work delves into the examination of P and\begin{document}$ CP $\end{document} \begin{document}$ \Omega_c $\end{document} \begin{document}$ \Omega_c $\end{document} \begin{document}$ \Omega_c\rightarrow \Omega^-\pi^+ $\end{document}
The exploration of symmetry laws stands as a cutting-edge direction in modern physics research. This work delves into the examination of P and
Published:
, doi: 10.1088/1674-1137/ae6630
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Gravitational-wave astronomy offers a promising opportunity to directly observe scalar-induced gravitational waves originating from the early universe. Experiments—including ground-based interferometers such as LIGO and Virgo, and pulsar timing arrays (PTAs) based on facilities such as FAST and SKA—are poised to significantly enhance sensitivity to these signals. In this paper, we combine Cosmic Microwave Background (CMB) and Baryon Acoustic Oscillation (BAO) datasets with upper or lower limits on the stochastic gravitational-wave background provided by FAST or SKA to constrain scalar-induced gravitational waves. To provide a comprehensive forecast, we consider two scenarios at a given frequency: one in which FAST or SKA does not detect scalar-induced gravitational waves, thereby setting an upper limit on the fractional energy density; and another in which these waves are detected, thus establishing a lower limit. In the ΛCDM+r model, the scalar spectral index of the power-law power spectrum is constrained to\begin{document}$ 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 $\end{document}
Gravitational-wave astronomy offers a promising opportunity to directly observe scalar-induced gravitational waves originating from the early universe. Experiments—including ground-based interferometers such as LIGO and Virgo, and pulsar timing arrays (PTAs) based on facilities such as FAST and SKA—are poised to significantly enhance sensitivity to these signals. In this paper, we combine Cosmic Microwave Background (CMB) and Baryon Acoustic Oscillation (BAO) datasets with upper or lower limits on the stochastic gravitational-wave background provided by FAST or SKA to constrain scalar-induced gravitational waves. To provide a comprehensive forecast, we consider two scenarios at a given frequency: one in which FAST or SKA does not detect scalar-induced gravitational waves, thereby setting an upper limit on the fractional energy density; and another in which these waves are detected, thus establishing a lower limit. In the ΛCDM+r model, the scalar spectral index of the power-law power spectrum is constrained to
Published:
, doi: 10.1088/1674-1137/ae5ef8
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We present a systematic analysis of the Higgs signal strengths at 125 GeV and 95 GeV in a non-supersymmetric\begin{document}$ 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/ae5ef3
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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/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 $\end{document}
In this work, we present the first computation of the full one-loop electroweak radiative corrections to the process
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, doi: 10.1088/1674-1137/ae62fc
Abstract:
We study the equation of state (EoS) of QCD matter in a bottom-up holographic setup that combines an Einstein-Maxwell-dilaton (EMD) sector with an improved Karch-Katz-Son-Stephanov (KKSS) flavor action. In the probe approximation, we perform an inverse reconstruction of the model functions by parameterizing them with neural networks and solving the EMD equations via a differentiable ODE solver (a neural ODE framework), calibrating the model to a reference thermodynamic table for\begin{document}$(2+1)$\end{document} \begin{document}$\mu_B=0$\end{document} \begin{document}$\mu_B=0$\end{document} \begin{document}$\beta_1$\end{document}
We study the equation of state (EoS) of QCD matter in a bottom-up holographic setup that combines an Einstein-Maxwell-dilaton (EMD) sector with an improved Karch-Katz-Son-Stephanov (KKSS) flavor action. In the probe approximation, we perform an inverse reconstruction of the model functions by parameterizing them with neural networks and solving the EMD equations via a differentiable ODE solver (a neural ODE framework), calibrating the model to a reference thermodynamic table for
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, doi: 10.1088/1674-1137/ae643e
Abstract:
We report stronger evidence for the\begin{document}$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/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/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/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/ae6b21
Abstract:
We investigate the impacts of strong magnetic fields on neutrino transport in core-collapse supernovae (CCSNe) using the leakage scheme. The magnetic field quantizes the momentum of electrons and positrons, resulting in the modification of weak-interaction cross sections and the chemical potentials of electrons and positrons. We derive a formula for the neutrino leakage scheme, including these two impacts, and perform 1D CCSN simulations with\begin{document}$ {\tt{GR1D}}$\end{document} \begin{document}$ 10^{16} $\end{document} \begin{document}$ 10^{17} $\end{document}
We investigate the impacts of strong magnetic fields on neutrino transport in core-collapse supernovae (CCSNe) using the leakage scheme. The magnetic field quantizes the momentum of electrons and positrons, resulting in the modification of weak-interaction cross sections and the chemical potentials of electrons and positrons. We derive a formula for the neutrino leakage scheme, including these two impacts, and perform 1D CCSN simulations with
Published:
, doi: 10.1088/1674-1137/ae5ef5
Abstract:
Identifying the thermodynamic conditions marking the onset of fission cycling is crucial for modeling heavy-element production in the r-process. In this work, we develop a framework to determine this onset over the\begin{document}$ (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/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}$\end{document} ![]()
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\begin{document}$\rho^{0} \rightarrow \pi^{+}\pi^{-}\pi^{0}$\end{document} ![]()
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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
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