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Published:
, doi: 10.1088/1674-1137/aeb489
Abstract:
The persistent discrepancy between early-time and late-Universe measurements of the Hubble constant, commonly known as the\begin{document}$ H_0 $\end{document} \begin{document}$ f(Q) $\end{document} \begin{document}$ + $\end{document} \begin{document}$ H_0 $\end{document} \begin{document}$ H_0 $\end{document} \begin{document}$ H_0 $\end{document}
The persistent discrepancy between early-time and late-Universe measurements of the Hubble constant, commonly known as the
Published:
, doi: 10.1088/1674-1137/aeb48c
Abstract:
We investigate the dynamics of charged test particles around a static black hole surrounded by anisotropic matter and immersed in an external, asymptotically uniform magnetic field. Using the Hamilton–Jacobi formalism, we analyze circular orbits, the structure of the effective potential, innermost stable circular orbits (ISCOs), and radiative efficiency, explicitly accounting for the effects of the anisotropy parameter K, the equation-of-state parameter ω, and the magnetic coupling parameter\begin{document}$ \Omega_B $\end{document} \begin{document}$ \omega = 1/3 $\end{document} \begin{document}$ \Omega_B $\end{document}
We investigate the dynamics of charged test particles around a static black hole surrounded by anisotropic matter and immersed in an external, asymptotically uniform magnetic field. Using the Hamilton–Jacobi formalism, we analyze circular orbits, the structure of the effective potential, innermost stable circular orbits (ISCOs), and radiative efficiency, explicitly accounting for the effects of the anisotropy parameter K, the equation-of-state parameter ω, and the magnetic coupling parameter
Published:
, doi: 10.1088/1674-1137/aeb3f0
Abstract:
We investigate a coupled ϕCDM cosmological model in which energy exchange between dark energy and dark matter is governed by the derivative interaction term\begin{document}$ Q = 3\alpha \dot{\rho}_m $\end{document} \begin{document}$ {\cal{O}}(10^{-4}) $\end{document} \begin{document}$ 1\sigma $\end{document} \begin{document}$ w_{\phi}=-1 $\end{document} \begin{document}$ H_0 $\end{document}
We investigate a coupled ϕCDM cosmological model in which energy exchange between dark energy and dark matter is governed by the derivative interaction term
Published:
Abstract:
State-resolved cross sections for the 20Ne(n, αi)17O (i=0,1,2,3) reactions were measured in the 8.9 – 11.5 MeV neutron energy region (11 energy points) at the HI-13 tandem accelerator of the China Institute of Atomic Energy (CIAE). The present measurements extend the data of the α0, α1, α2, and α3 channels from 9.6 MeV to 11.5 MeV, where previous measurements reported only the summed (α0+ α1) cross sections. A twin gridded ionization chamber (GIC) filled with a neon-based gas mixture was used as the charged-particle detection, with the neon gas serving as an active sample. Corrections for detector efficiency, background interference, and neutron-field non-uniformity were performed by combining experimental measurements and detailed Monte Carlo simulations. From 9.6 to 11.5 MeV, the measured 20Ne(n, α0)17O and 20Ne(n, α1)17O cross sections decrease as neutron energy increases, and are generally consistent with those in JENDL-5. The 20Ne(n, α2)17O cross sections are generally above those in JENDL-5, whereas the 20Ne(n, α3)17O cross sections are below those in JENDL-5. In detail, the measured excitation functions exhibit noticeable fluctuations that are not included in JENDL-5. The TALYS-2.2 calculations can describe the measured α0, α1 and α2 cross sections reasonably, whereas the calculated α3 cross sections are generally higher than the measured α3 cross sections. The present data provide new state-resolved constraints for modeling the 20Ne(n, α)17O reaction and improving nuclear data evaluation.
State-resolved cross sections for the 20Ne(n, αi)17O (i=0,1,2,3) reactions were measured in the 8.9 – 11.5 MeV neutron energy region (11 energy points) at the HI-13 tandem accelerator of the China Institute of Atomic Energy (CIAE). The present measurements extend the data of the α0, α1, α2, and α3 channels from 9.6 MeV to 11.5 MeV, where previous measurements reported only the summed (α0+ α1) cross sections. A twin gridded ionization chamber (GIC) filled with a neon-based gas mixture was used as the charged-particle detection, with the neon gas serving as an active sample. Corrections for detector efficiency, background interference, and neutron-field non-uniformity were performed by combining experimental measurements and detailed Monte Carlo simulations. From 9.6 to 11.5 MeV, the measured 20Ne(n, α0)17O and 20Ne(n, α1)17O cross sections decrease as neutron energy increases, and are generally consistent with those in JENDL-5. The 20Ne(n, α2)17O cross sections are generally above those in JENDL-5, whereas the 20Ne(n, α3)17O cross sections are below those in JENDL-5. In detail, the measured excitation functions exhibit noticeable fluctuations that are not included in JENDL-5. The TALYS-2.2 calculations can describe the measured α0, α1 and α2 cross sections reasonably, whereas the calculated α3 cross sections are generally higher than the measured α3 cross sections. The present data provide new state-resolved constraints for modeling the 20Ne(n, α)17O reaction and improving nuclear data evaluation.
Published:
, doi: 10.1088/1674-1137/aeb2cd
Abstract:
Since the first direct detection of gravitational waves (GWs) from a binary black hole merger by the LIGO–Virgo Collaboration, GWs have emerged as a powerful probe of astrophysics and cosmology. If extragalactic compact dark matter (DM) candidates, such as primordial black holes, constitute a non-negligible fraction of the DM component over a broad mass range, they can imprint distinctive microlensing signatures in GW signals. In this work, we develop a framework to infer the population properties of extragalactic compact DM by simulating microlensed GWs in the frequency band of the third-generation ground-based GW detector Einstein Telescope and analyzing the resulting signals using hierarchical Bayesian inference. For a population described by a power-law mass function, we show that detecting as few as several microlensed GW events among 104 binary black hole coalescences can constrain the compact-DM abundance to the level of ~10-3. This forecast demonstrates that searching for and identifying microlensing signatures in future GW observations can provide a complementary approach to constraining compact DM scenarios.
Since the first direct detection of gravitational waves (GWs) from a binary black hole merger by the LIGO–Virgo Collaboration, GWs have emerged as a powerful probe of astrophysics and cosmology. If extragalactic compact dark matter (DM) candidates, such as primordial black holes, constitute a non-negligible fraction of the DM component over a broad mass range, they can imprint distinctive microlensing signatures in GW signals. In this work, we develop a framework to infer the population properties of extragalactic compact DM by simulating microlensed GWs in the frequency band of the third-generation ground-based GW detector Einstein Telescope and analyzing the resulting signals using hierarchical Bayesian inference. For a population described by a power-law mass function, we show that detecting as few as several microlensed GW events among 104 binary black hole coalescences can constrain the compact-DM abundance to the level of ~10-3. This forecast demonstrates that searching for and identifying microlensing signatures in future GW observations can provide a complementary approach to constraining compact DM scenarios.
Published:
, doi: 10.1088/1674-1137/aeb2b5
Abstract:
We investigate the quasinormal modes of massless scalar and electromagnetic perturbations in charged Euler--Heisenberg black holes surrounded by perfect fluid dark matter. The quasinormal frequencies are calculated using the asymptotic iteration method and the sixth-order WKB approximation, and the relative deviations between the two methods are quantitatively analyzed to verify the reliability of the results. The greybody factors for both perturbations are also evaluated within the sixth-order WKB framework. We systematically examine the effects of the black hole charge Q, the nonlinear electrodynamic parameter a, the dark matter parameter λ, and the angular quantum number l on the quasinormal frequencies and greybody factors. We find that these parameters significantly modify the structure of the effective potential barriers and consequently affect the oscillation frequencies, damping rates, and wave transmission and reflection properties of the perturbed fields.
We investigate the quasinormal modes of massless scalar and electromagnetic perturbations in charged Euler--Heisenberg black holes surrounded by perfect fluid dark matter. The quasinormal frequencies are calculated using the asymptotic iteration method and the sixth-order WKB approximation, and the relative deviations between the two methods are quantitatively analyzed to verify the reliability of the results. The greybody factors for both perturbations are also evaluated within the sixth-order WKB framework. We systematically examine the effects of the black hole charge Q, the nonlinear electrodynamic parameter a, the dark matter parameter λ, and the angular quantum number l on the quasinormal frequencies and greybody factors. We find that these parameters significantly modify the structure of the effective potential barriers and consequently affect the oscillation frequencies, damping rates, and wave transmission and reflection properties of the perturbed fields.
Published:
, doi: 10.1088/1674-1137/aeb253
Abstract:
We develop a relativistic proton-neutron quasiparticle random-phase approximation (pnQRPA) plus proton-neutron quasiparticle-vibration coupling (pnQPVC) model, based on localized relativistic Hartree-Fock-Bogoliubov theory with the PCF-PK1 density functional. This model incorporates localized exchange terms and tensor couplings. The localized exchange terms enable the residual interaction, particularly the isovector-pseudovector (tPV) channel, to be determined fully self-consistently without any phenomenological adjustment of the tPV coupling strength. We apply the newly developed relativistic pnQPVC model to the Gamow-Teller (GT) strength distributions in\begin{document}$^{116-134}$\end{document} \begin{document}$\beta^-$\end{document} \begin{document}$N=50$\end{document} \begin{document}$N=82$\end{document}
We develop a relativistic proton-neutron quasiparticle random-phase approximation (pnQRPA) plus proton-neutron quasiparticle-vibration coupling (pnQPVC) model, based on localized relativistic Hartree-Fock-Bogoliubov theory with the PCF-PK1 density functional. This model incorporates localized exchange terms and tensor couplings. The localized exchange terms enable the residual interaction, particularly the isovector-pseudovector (tPV) channel, to be determined fully self-consistently without any phenomenological adjustment of the tPV coupling strength. We apply the newly developed relativistic pnQPVC model to the Gamow-Teller (GT) strength distributions in
Published:
, doi: 10.1088/1674-1137/aead6f
Abstract:
We investigate the dependence of corrections from initial-state radiation in\begin{document}$ e^+ e^- $\end{document}
We investigate the dependence of corrections from initial-state radiation in
Published:
, doi: 10.1088/1674-1137/aeac00
Abstract:
Within the framework of the dinuclear system (DNS) model, the synthesis of superheavy nuclei in 48Ca-, 50Ti-, 51V-, and 54Cr-induced fusion reactions on actinide nuclei has been systematically investigated. The nucleus–nucleus potential and the potential energy surface in the DNS model are calculated using the well-established Skyrme energy-density functional with the parameter sets SKM, SKM*, Ska, Z, and SLy4, respectively. The available experimental data from Dubna, GSI, RIKEN, and Berkeley are well reproduced by the model. It is found that the fusion-evaporation residue excitation functions and production cross sections of superheavy nuclei are correlated with nuclear matter properties. The 48Ca-induced reaction, i.e., 48Ca + 248Cm, has a larger production cross section for synthesizing the superheavy nucleus livermorium than the non-magic systems 50Ti + 244Pu and 54Cr + 238U. The production cross sections of new superheavy elements with atomic numbers\begin{document}$ Z=119 $\end{document}
Within the framework of the dinuclear system (DNS) model, the synthesis of superheavy nuclei in 48Ca-, 50Ti-, 51V-, and 54Cr-induced fusion reactions on actinide nuclei has been systematically investigated. The nucleus–nucleus potential and the potential energy surface in the DNS model are calculated using the well-established Skyrme energy-density functional with the parameter sets SKM, SKM*, Ska, Z, and SLy4, respectively. The available experimental data from Dubna, GSI, RIKEN, and Berkeley are well reproduced by the model. It is found that the fusion-evaporation residue excitation functions and production cross sections of superheavy nuclei are correlated with nuclear matter properties. The 48Ca-induced reaction, i.e., 48Ca + 248Cm, has a larger production cross section for synthesizing the superheavy nucleus livermorium than the non-magic systems 50Ti + 244Pu and 54Cr + 238U. The production cross sections of new superheavy elements with atomic numbers
Published:
Abstract:
We present a comprehensive analysis of the recently discovered TeV gamma-ray source LHAASO J2238+5900. Based on data collected by LHAASO, our fitting results indicate that the source is significantly extended, with an angular extension of\begin{document}$0.54^{\circ}\pm0.01^{\circ}$\end{document} \begin{document}$\Gamma=1.97\pm0.06$\end{document} \begin{document}$41.0\pm3.5$\end{document}
We present a comprehensive analysis of the recently discovered TeV gamma-ray source LHAASO J2238+5900. Based on data collected by LHAASO, our fitting results indicate that the source is significantly extended, with an angular extension of
Published:
, doi: 10.1088/1674-1137/aeabfb
Abstract:
Primordial black holes (PBHs) form when large primordial curvature perturbations re-enter the Hubble radius and exceed the classical collapse threshold. These perturbations originate as quantum fluctuations of the inflationary vacuum, which motivates a quantum-information description of the scalar sector responsible for PBH production. We develop a conservative extension of the standard PBH and scalar-induced gravitational-wave (SIGW) framework, in which Gaussian quantum discord is used as a diagnostic of residual quantum correlations rather than as a new PBH formation criterion. We describe each\begin{document}$ ({\boldsymbol{k}}, -{\boldsymbol{k}}) $\end{document} \begin{document}$ Q_{{\rm{dec}}}(k) $\end{document} \begin{document}$ Q_{{\rm{dec}}}(ku)Q_{{\rm{dec}}}(kv) $\end{document} \begin{document}$ Q_{{\rm{dec}}} $\end{document} \begin{document}$ \Omega_{{\rm{GW}}}^{{\rm{eff}}}\simeq Q_{{\rm{dec}}}^2\Omega_{{\rm{GW}}}^{{\rm{class}}} $\end{document}
Primordial black holes (PBHs) form when large primordial curvature perturbations re-enter the Hubble radius and exceed the classical collapse threshold. These perturbations originate as quantum fluctuations of the inflationary vacuum, which motivates a quantum-information description of the scalar sector responsible for PBH production. We develop a conservative extension of the standard PBH and scalar-induced gravitational-wave (SIGW) framework, in which Gaussian quantum discord is used as a diagnostic of residual quantum correlations rather than as a new PBH formation criterion. We describe each
Published:
, doi: 10.1088/1674-1137/aeb2b3
Abstract:
We study the doubly heavy open-flavor tetraquarks\begin{document}$ T_{bc}^{(0)} $\end{document} \begin{document}$ J^{P}=0^{+} $\end{document} \begin{document}$ T_{bc}^{(1)} $\end{document} \begin{document}$ J^{P}=1^{+} $\end{document} \begin{document}$ \Sigma_g^+(1S) $\end{document} \begin{document}$ M(T_{bc}^{(0)}) = 7.143 $\end{document} \begin{document}$ M(T_{bc}^{(1)}) = 7.217 $\end{document} \begin{document}$ \Delta_{HF}\simeq 59 $\end{document} \begin{document}$ \partial\Delta_{HF}/\partial\kappa_{\bar b\bar c}=2 $\end{document} \begin{document}$ \langle r\rangle\simeq 0.45 $\end{document} \begin{document}$ \langle 1/r\rangle^{-1}\simeq 0.33 $\end{document} \begin{document}$ B\bar D $\end{document} \begin{document}$ B^{*}\bar D $\end{document} \begin{document}$ B\bar D^{*} $\end{document} \begin{document}$ B^{*}\bar D $\end{document} \begin{document}$ \Sigma_g^+(1S) $\end{document} \begin{document}$ 2\kappa_{ud}\approx 206 $\end{document} \begin{document}$ B^{(*)}\bar D^{(*)} $\end{document} \begin{document}$ \bar{{\bf{6}}}\otimes{\bf{6}} $\end{document} \begin{document}$ \bar{{\bf{6}}} $\end{document}
We study the doubly heavy open-flavor tetraquarks
Published:
, doi: 10.1088/1674-1137/aea547
Abstract:
We prove a new spin–statistics theorem for a class of quantum field theories with pseudo-Hermitian Hamiltonians. Quantum fields with integer spin exhibit fermionic statistics, whereas those with half-integer spin exhibit bosonic statistics, in contrast to the conventional case. This reversal arises from defining canonical field operators using pseudo-Hermitian conjugation rather than Hermitian conjugation, thereby circumventing the conventional spin–statistics theorem. The free fields retain locality, Lorentz covariance, and unitary evolution. However, interactions can violate unitarity because of the intrinsically non-Hermitian nature of pseudo-Hermitian Hamiltonians. We discuss unitarity issues in this quantum field theory and its potential applications to the dS4/CFT3 correspondence.
We prove a new spin–statistics theorem for a class of quantum field theories with pseudo-Hermitian Hamiltonians. Quantum fields with integer spin exhibit fermionic statistics, whereas those with half-integer spin exhibit bosonic statistics, in contrast to the conventional case. This reversal arises from defining canonical field operators using pseudo-Hermitian conjugation rather than Hermitian conjugation, thereby circumventing the conventional spin–statistics theorem. The free fields retain locality, Lorentz covariance, and unitary evolution. However, interactions can violate unitarity because of the intrinsically non-Hermitian nature of pseudo-Hermitian Hamiltonians. We discuss unitarity issues in this quantum field theory and its potential applications to the dS4/CFT3 correspondence.
Published:
, doi: 10.1088/1674-1137/aeb254
Abstract:
Partial wave analysis (PWA) is a key method in hadron physics for extracting the properties of hadronic resonances. As experimental statistics increase, conventional implementations face substantial challenges in memory usage and computational speed. We present\begin{document}$\mathrm{CTPWA} $\end{document}
Partial wave analysis (PWA) is a key method in hadron physics for extracting the properties of hadronic resonances. As experimental statistics increase, conventional implementations face substantial challenges in memory usage and computational speed. We present
Published:
, doi: 10.1088/1674-1137/ad8ec2
Abstract:
The direct CP asymmetry in the weak decay process of hadrons is commonly attributed to the weak phase of the CKM matrix and the indeterminate strong phase. We propose a method to generate a significant phase difference through the interference between ρ and ω mesons, taking into account the G-parity allowed decay process of\begin{document}$\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
Published:
, doi: 10.1088/1674-1137/aeb3f1
Abstract:
In this paper, we study the optical appearance of a 4D Einstein-Gauss-Bonnet asymmetric thin-shell wormhole. Using Visser's cut-and-paste construction, we determine the photon sphere radius and critical impact parameter for different values of the Gauss-Bonnet coupling α. We then investigate the effective potential and photon motion in the wormhole spacetime. We find that the effective potential, light-ray trajectories, and azimuthal angle are closely related to the mass ratio of the two spacetimes. Considering an optically thin accretion disk as the only light source, we find that the images of the asymmetric thin-shell wormhole exhibit additional photon rings and lensing bands that are absent for a 4D Einstein-Gauss-Bonnet black hole. Furthermore, the sizes of these extra rings increase with α, whereas the photon ring of a 4D EGB black hole shrinks as α increases. This opposite α dependence is the main distinguishing signature of the wormhole geometry, and the resulting exceptionally bright rings may provide a useful observational criterion for distinguishing and characterizing a thin-shell wormhole spacetime. We also verify that the mass ratio and throat radius significantly affect the morphology of these extra photon rings.
In this paper, we study the optical appearance of a 4D Einstein-Gauss-Bonnet asymmetric thin-shell wormhole. Using Visser's cut-and-paste construction, we determine the photon sphere radius and critical impact parameter for different values of the Gauss-Bonnet coupling α. We then investigate the effective potential and photon motion in the wormhole spacetime. We find that the effective potential, light-ray trajectories, and azimuthal angle are closely related to the mass ratio of the two spacetimes. Considering an optically thin accretion disk as the only light source, we find that the images of the asymmetric thin-shell wormhole exhibit additional photon rings and lensing bands that are absent for a 4D Einstein-Gauss-Bonnet black hole. Furthermore, the sizes of these extra rings increase with α, whereas the photon ring of a 4D EGB black hole shrinks as α increases. This opposite α dependence is the main distinguishing signature of the wormhole geometry, and the resulting exceptionally bright rings may provide a useful observational criterion for distinguishing and characterizing a thin-shell wormhole spacetime. We also verify that the mass ratio and throat radius significantly affect the morphology of these extra photon rings.
Published:
, doi: 10.1088/1674-1137/aea8f4
Abstract:
The innermost stable circular orbit (ISCO) provides a fundamental test of spacetime structure. However, the influence of anisotropic energy–momentum tensors on its properties in higher-dimensional black hole spacetimes remains incompletely understood. In this work, we investigate the upper bound on the ISCO radius in higher-dimensional, static, spherically symmetric, and asymptotically flat black hole spacetimes in the presence of an anisotropic energy–momentum tensor. We assume that the energy–momentum tensor satisfies the weak energy condition, has a nonpositive trace, and obeys constraints on the radial and tangential pressures, which are collectively equivalent to the dominant energy condition with additional restrictions. By analyzing the effective potential for timelike geodesics and imposing the ISCO conditions, we demonstrate that, in general, no upper bound exists on the ISCO radius in higher-dimensional spacetimes. The results show that the allowed equations of state of matter at the ISCO depend explicitly on the spacetime dimension. In the large-D limit, both the radial and tangential equations of state vanish, corresponding to pressureless dust behavior. These findings advance our understanding of orbital stability in higher-dimensional gravitational systems and highlight fundamental differences from four-dimensional black hole dynamics.
The innermost stable circular orbit (ISCO) provides a fundamental test of spacetime structure. However, the influence of anisotropic energy–momentum tensors on its properties in higher-dimensional black hole spacetimes remains incompletely understood. In this work, we investigate the upper bound on the ISCO radius in higher-dimensional, static, spherically symmetric, and asymptotically flat black hole spacetimes in the presence of an anisotropic energy–momentum tensor. We assume that the energy–momentum tensor satisfies the weak energy condition, has a nonpositive trace, and obeys constraints on the radial and tangential pressures, which are collectively equivalent to the dominant energy condition with additional restrictions. By analyzing the effective potential for timelike geodesics and imposing the ISCO conditions, we demonstrate that, in general, no upper bound exists on the ISCO radius in higher-dimensional spacetimes. The results show that the allowed equations of state of matter at the ISCO depend explicitly on the spacetime dimension. In the large-D limit, both the radial and tangential equations of state vanish, corresponding to pressureless dust behavior. These findings advance our understanding of orbital stability in higher-dimensional gravitational systems and highlight fundamental differences from four-dimensional black hole dynamics.
Published:
, doi: 10.1088/1674-1137/aeaa12
Abstract:
Quantum phases establish a connection between gravitation and quantum information, offering a novel avenue for exploring the properties of space-time. In this paper, we investigate the quantum correlations (QCs) of neutrinos in the Kerr-Newman space-time for both zero- and nonzero-angular-momentum propagation. The results show that, for zero-angular-momentum propagation, the oscillation periods of the survival probability and QCs progressively decrease with propagation distance in the inward direction. In the outward direction, increasing M lengthens the oscillation periods of\begin{document}$P_{\nu_e\rightarrow\nu_e}$\end{document}
Quantum phases establish a connection between gravitation and quantum information, offering a novel avenue for exploring the properties of space-time. In this paper, we investigate the quantum correlations (QCs) of neutrinos in the Kerr-Newman space-time for both zero- and nonzero-angular-momentum propagation. The results show that, for zero-angular-momentum propagation, the oscillation periods of the survival probability and QCs progressively decrease with propagation distance in the inward direction. In the outward direction, increasing M lengthens the oscillation periods of
Published:
, doi: 10.1088/1674-1137/aeb3f5
Abstract:
The exploration of exotic nuclear phenomena is a central theme in nuclear physics. In this work, the exotic structures of neutron-rich phosphorus, sulfur, chlorine, and argon isotopic chains are systematically investigated using the relativistic mean field combined with the complex momentum representation (RMF+CMR) approach. Based on the calculated two-neutron separation energies, the neutron drip-line positions of the four isotopic chains are predicted. In addition, the single-particle levels of these four isotopic chains are examined. The increasing difference between the neutron and proton rms radii indicates enhanced neutron-skin character in the neutron-rich region. Finally, diffuse density distributions are observed across the P, S, Cl, and Ar isotopic chains.
The exploration of exotic nuclear phenomena is a central theme in nuclear physics. In this work, the exotic structures of neutron-rich phosphorus, sulfur, chlorine, and argon isotopic chains are systematically investigated using the relativistic mean field combined with the complex momentum representation (RMF+CMR) approach. Based on the calculated two-neutron separation energies, the neutron drip-line positions of the four isotopic chains are predicted. In addition, the single-particle levels of these four isotopic chains are examined. The increasing difference between the neutron and proton rms radii indicates enhanced neutron-skin character in the neutron-rich region. Finally, diffuse density distributions are observed across the P, S, Cl, and Ar isotopic chains.
Published:
, doi: 10.1088/1674-1137/aeb2b2
Abstract:
We revisit the X(2356) enhancement observed by BESIII in\begin{document}$ e^+e^-\to\Lambda\bar\Lambda\eta $\end{document} \begin{document}$ \Lambda\bar\Lambda $\end{document}
We revisit the X(2356) enhancement observed by BESIII in
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