Impact factor of Chinese Physics C is 3.6 in 2023 Impact factor of Chinese Physics C is 3.6 in 2022 2021 Impact Factor 2.944
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  • Study of the $ {{\boldsymbol J}/\boldsymbol\psi\bf\to \boldsymbol\Lambda\bar{\boldsymbol\Sigma}^{\bf 0}\boldsymbol\eta}$ reaction
    Lian-Rong Dai, Wen-Tao Lyu, E. Oset
    2026, 50(11): 113106. doi: 10.1088/1674-1137/ae8cee
    We study the isospin-violating $J/\psi \to \Lambda\bar \Sigma^0 \eta $ reaction, recently measured by the BESIII collaboration, by considering the dominant terms involving $\bar \Sigma^0$ and pairs of pseudoscalar-baryon particles that together form an SU(3) singlet and can therefore couple to the $J/\psi$. We then allow these pairs to undergo final-state interaction to produce the final $\eta \Lambda$. We find that the relevant original channels are $\bar K N$ and $K \Xi$, and that the incomplete cancellation of terms involving charged and neutral particles, owing to their different masses, is responsible for the reaction. With this mechanism, we find good agreement with the three experimental mass distributions.
  • Extending the sensitivity of heavy sterile neutrino searches with solar neutrino experiments
    Yutao Zhu, Haoyang Fu, Wentai Luo, Shaomin Chen, Litao Yang, Zhicai Zhang
    2026, 50(11): 113003. doi: 10.1088/1674-1137/ae9929
    A sensitivity study of the search for heavy sterile neutrinos ($ \nu_H $) in the MeV mass range using solar neutrino experiments is presented. $ \nu_H $, with masses ranging from a few MeV up to approximately 15 MeV, can be produced in the Sun through 8B decay and subsequently decays into $ \nu_e e^+ e^- $. Its flux and lifetime strongly depend on the mixing parameter $ |U_{eH}|^2 $ and mass $ m_{\nu_H} $. The $ \nu_H $ signal can be detected via its decay products, either the $ e^+e^- $ pair or $ \nu_e $, depending on whether $ \nu_H $ decays inside or outside the detector. Expected signal yields for both detection methods (detecting $ e^+e^- $ or $ \nu_e $ signal) are presented across the full $ |U_{eH}|^2 $ and $ m_{\nu_H} $ parameter spaces. These two methods are found to be complementary in different regions of the $ |U_{eH}|^2 $ and $ m_{\nu_H} $ phase spaces. By combining both approaches, we anticipate observing at least a handful of signal events across most of the parameter space of $ 10^{-6} \lt |U_{eH}|^2 \lt 1 $ and 2 MeV $ \lt m_{\nu_H} \lt $ 15 MeV, assuming a 500-ton solar neutrino experiment operating for one year. Key variables, such as the energy spectra of $ \nu_e $ or $ e^+e^- $ and $ \nu_e $ solar angle, are also discussed to help distinguish the signal from major backgrounds, such as solar neutrino events.
  • Isospin diffusion coefficient for nuclear matter
    Han-Wen Cui, Ji-You Fu, Xin-Le Shang, Jian-Min Dong, Wei Zuo
    2026, 50(11): 114104. doi: 10.1088/1674-1137/ae927a
    A systematic evaluation of the isospin diffusion coefficients of symmetric and β-stable nuclear matter in the low-temperature limit is presented within the Abrikosov–Khalatnikov framework. Key microscopic inputs, including the susceptibility, effective mass, and in-medium differential cross sections, are obtained self-consistently within the Brueckner–Hartree–Fock approach using the realistic Av18 potential, with and without a microscopic three-body force. The inclusion of three-body forces suppresses the effective in-medium cross sections and consequently enhances the diffusion coefficient. Compared with the exact Abrikosov–Khalatnikov results, the neutron–proton total cross-section approximation, which retains only the neutron–proton contribution, provides a comparatively robust description, highlighting the dominant role of the neutron–proton channel. Furthermore, the dependence of the diffusion coefficient on the isospin asymmetry β deviates significantly from the quadratic form $ (1-\beta^2) $ and exhibits a symmetric double-peaked structure. This behavior arises primarily from the β dependence of mixing effects associated with the effective mass, in-medium scattering, and Fermi-momentum splitting, in addition to the contribution from the susceptibility. These results provide useful microscopic input for transport simulations and constraints on the nuclear symmetry energy.
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  • Branch-dependent chaos bound behavior of spinning particles in a spherically symmetric black hole spacetime
    Xiaowei Li, Chuang Yang, Deyou Chen
    2027, 51(1): 015107-015107-14. doi: 10.1088/1674-1137/aeaa13
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    We investigate the instability of spinning test particles and the associated classical chaos bound in a spherically symmetric black hole spacetime with two photon spheres. The radial effective potential admits two branches of unstable circular orbits in the near-horizon and far-horizon regions. Although both branches are locally unstable, their Lyapunov exponents have different relationships with the black hole surface gravity. The near-horizon branch satisfies the bound, whereas the far-horizon branch can violate it. We further examine the effects of particle spin, total angular momentum, and black hole parameters. Spin-curvature coupling shifts the unstable orbits and modifies their instability, whereas the total angular momentum and background parameters generally have larger effects. Our results show that the validity of the classical orbital chaos bound is branch dependent.
  • Constraining Lorentz symmetry breaking in bumblebee gravity with extreme mass-ratio inspirals
    Sheng Long, Zhong-wu Xia, Huajie Gong, Zhoujian Cao, Qiyuan Pan, Jiliang Jing
    2027, 51(1): 015105-015105-10. doi: 10.1088/1674-1137/aea1f0
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    Extreme mass-ratio inspirals (EMRIs), with their long-lived and highly relativistic orbital evolution, can probe strong-field spacetime geometry and provide an important means of testing general relativity. In this work, we investigate EMRI waveforms in a Schwarzschild-like black hole spacetime arising in bumblebee gravity, where Lorentz symmetry breaking (LSB) is characterized by the dimensionless parameter ℓ. We construct EMRI waveforms within the Augmented Analytic Kludge (AAK) framework using the modified orbital frequencies and fluxes. We find that ℓ significantly affects orbital evolution and thereby modifies the waveform. These modifications grow with increasing ℓ and are further enhanced for more eccentric orbits. Furthermore, using Bayesian analysis, we obtain the posterior distributions of the EMRI parameters with ℓ included. Our results show that all injected source parameters are recovered within their $ 1\,\sigma $ credible intervals. We find that the bumblebee parameter ℓ can be constrained with an uncertainty of order $ {\cal{O}}(10^{-4}) $ by LISA.
  • Analytic solution for the motion of spinning particles in plane gravitational wave spacetime
    Ke Wang
    2027, 51(1): 015104-015104-10. doi: 10.1088/1674-1137/ae9c1c
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    The interaction between spin and gravitational waves causes spinning bodies to deviate from geodesic motion. In this work, we obtain an analytic solution to the Mathisson–Papapetrou–Dixon equations at linear order in spin for plane gravitational-wave spacetimes. Our approach combines a parallel-transported tetrad with the translational Killing symmetries of plane-wave spacetimes, yielding six conserved quantities that fully determine the momentum, spin evolution, and worldline. The resulting transverse and longitudinal motions are expressed in closed form as single integrals over the retarded time, providing a unified, model-independent framework for computing spin–curvature-induced deviations. This analytic solution provides a versatile tool for studying spin-dependent effects in gravitational memory, Penrose-limit geometries, and high-energy scattering regimes.
Current Issued
Chinese Physics C
2026 Vol. 50, No. 11
Published: 01 November 2026
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Chinese Physics C
IF: 3.0

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ISSN 1674-1137 CN 11-5641/O4

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