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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  • Resonance of hypernuclei with complex momentum representation
    Hantao Zhang, Chao-Feng Chen, Xian-Rong Zhou, Zhongzhou Ren
    2025, 49(4): 044101. doi: 10.1088/1674-1137/ad9a8c
    By combining the Skyrme-Hartree-Fock method with complex momentum representation (CMR), the resonant states of $ {}^{17}_\Lambda $O, $ {}^{41}_{\Lambda} $Ca, $ {}^{49}_{\Lambda} $Ca, and $ {}^{57}_\Lambda $Ni were investigated. The phase shifts for hyperon-nucleus elastic scattering were determined with continuum level density (CLD), and the scattering length as well as the resonance energy were obtained by utilizing the effective range expansion. Our method, abbreviated as CMR-CLD, exhibits good consistency with traditional approaches and provides ground work for investigating scattering and resonance problems in deformed and multi-hyperon hypernuclei.
  • Inferring a spinning black hole in an expanding universe via the S2 star around the galactic center
    Jin-Tao Yao, Xin Li
    2025, 49(4): 045106. doi: 10.1088/1674-1137/ad9304
    The nearest black hole to Earth, Sagittarius A$ ^\star $ (Sgr A$ ^\star $), with its intense gravitational field, provides a unique opportunity to explore black hole mysteries. Over the past few decades, monitoring of the S2 star has provided extensive valuable data that can be utilized to examine various gravity theories and black hole paradigms. This paper focuses on the most intriguing objects in astronomy, spinning black holes, and investigates the effects of spin on orbital motion. By applying the Markov Chain Monte Carlo algorithm to publicly available observational data of the S2 star, our findings indicate that current data fail to constrain the spin of Sgr A$ ^\star $. Simulated stars with smaller semi-major axes reveal that the direction of Lense-Thirring precession aligns with the spin direction of Sgr A$ ^\star $. Additionally, by incorporating the cosmological constant, which accounts for the expansion of the universe, into our analysis, we establish an upper limit of $ \Lambda \lesssim 7.3 \times 10^{-34} \text{ km}^{-2} $ on the cosmological constant at the $ 1\sigma $ confidence level. Future long-term monitoring of S-cluster stars, combined with enhanced observational precision, may enable the determination of the spin of Sgr A$ ^\star $ and further tighten the bound on the cosmological constant.
  • An empirical formula of nuclear β-decay half-lives with the transition-strength contribution
    Lei Tian, Wei-Feng Li, Ji-Yu Fang, Zhong-Ming Niu
    2025, 49(4): 044110. doi: 10.1088/1674-1137/ad9303
    An empirical formula of nuclear β-decay half-lives is proposed by including the transition-strength contribution. The inclusion of the transition-strength contribution can reduce nuclear β-decay half-lives by about an order of magnitude, and its effect gradually increases toward the neutron-rich or heavy nuclear regions. For nuclear β-decay half-lives less than 1 s, the empirical formula can describe the experimental data within approximately2 times, which is more accurate than the sophisticated microscopic models. The transition-strength contribution can also be effectively considered by refitting the parameters of other empirical formulas without the transition-strength term although they will still significantly deviate from the new empirical formula in light or heavy neutron-rich nuclear regions. This indicates that the inclusion of the transition-strength contribution in the empirical formula is crucial for the global description of nuclear β-decay half-lives. The extrapolation ability of the new empirical formula was verified by the newly measured β-decay half-lives.
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  • Model-independent constraints on the Hubble constant using lensed quasars and the latest supernova
    Liang Liu, Ai-Yang Bi, Li Tang, Ying Wu
    2025, 49(5): 055107-055107-9. doi: 10.1088/1674-1137/adbc87
    Show Abstract
    The Hubble constant $H_0$, a key parameter quantifying the present expansion rate of the universe, remains a subject of significant debate due to the persistent tension between early- and late-universe measurements. Strong gravitational lensing (SGL) time delays provide an independent avenue to constrain $H_0$. In this paper, we utilize seven SGL systems from the TDCOSMO sample to constrain $H_0$, employing the model-independent approaches: deep neural networks (DNN), Gaussian process (GP), polynomial fitting (polyfit) and Padé approximant (PA). Using these methods, we reconstruct unanchored luminosity distances from the Pantheon+ SNe Ia dataset and obtain $H_0=72.3^{+3.8}_{-3.6}$ km s−1 Mpc−1, $H_0=72.4^{+1.6}_{-1.7}$ km s−1 Mpc−1, $H_0=70.7^{+3.0}_{-3.1}$ km s−1 Mpc−1 and $H_0=74.0^{+2.7}_{-2.7}$ km s−1 Mpc−1, respectively. These estimates are consistent within 1σ level and align with local distance ladder results. Notably, the GP method achieves uncertainties that are half those of the DNN approach, whereas the DNN method offers more reliable confidence intervals in reconstruction at high redshifts. Our findings underscore the potential of these methodologies to refine constraints on $H_0$ and contribute to resolving the Hubble tension with future advancements.
  • Configuration-interaction relativistic Hartree-Fock model
    Jia Liu, Yi-Fei Niu, Wen-Hui Long
    2025, 49(6): 064104-064104-13. doi: 10.1088/1674-1137/adbdba
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    The configuration interaction relativistic Hartree-Fock (CI-RHF) model is developed in this work. Compared to the conventional configuration interaction shell model (CISM), the CI-RHF model can be applied to study the structural properties of a wide range of nuclei without readjusting any parameters, as the effective Hamiltonian for different model spaces can be deduced consistently from a universal density-dependent Lagrangian based on the Hartree-Fock single-particle basis. The convergence of intermediate-state excitations has been examined in evaluating the effective interactions, and the core-polarization effects are illustrated, taking $ ^{18} {\rm{O}}$ as an example. Employing the CI-RHF model, both the bulk properties and low-lying spectra of even-even nuclei $^{18-28} {\rm{Ne}}$ have been well-reproduced with the model space restricted to the $ sd $ shell. Studies of the isotopic evolution concerning charge radii and low-lying spectra highlight the shell closure at $ N=14 $ for neon isotopes. Furthermore, the cross-shell calculations extending from the $ sd $ to $ pf $ shell successfully reproduced the low-lying spectra of $ ^{30} {\rm{Ne}}$ and $ ^{32} {\rm{Ne}}$. Notably, remarkably low excitation energies $ E(2^{+}_{1}) $ of $ ^{30} {\rm{Ne}}$ suggest the disappearance of the conventional magicity $ N=20 $.
  • Collective impact of higher-order deformations of target nuclei on the fusion dynamics of heavy-ion induced reactions
    Harshit Sharma, Raj Kumar, Manoj K. Sharma
    2025, 49(6): 064110-064110-12. doi: 10.1088/1674-1137/adbace
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    Several studies on fusion reaction dynamics focused on the impact of quadrupole $\beta_2^{\pm}$ deformation. However, existing literature highlights the importance of the octupole $\beta_3^{\pm}$ and hexadecapole $\beta_4^{\pm}$ deformations associated with both the projectile and target nuclei. However, the collective influence of these deformations ($\beta_2$, $\beta_3$, and $\beta_4$) on the fusion reaction dynamics has not been examined explicitly. In this study, we investigated the collective influence of higher-order deformations up to $\beta_4$ on the barrier characteristics, in particular $V_B$, $R_B$, and $\hbar\omega$, and their impact on the fusion cross-sections of heavy-ion induced reactions in the mass range $163\leq{ {A}}\leq182$. The reactions were examined at both compact and elongated configurations of the deformed nuclei. Heavy ion-induced reactions, which consist of target nuclei with higher-order deformations up to $\beta_4$, reveal a notable alteration in the barrier characteristics $V_B$ and $R_B$, along with a significant change in orientation $\theta_i$ for both compact and elongated configurations. In addition, the incorporation of deformations up to $\beta_4$ and their corresponding orientations $\theta_i$ contributes to enhanced capture cross-sections $\sigma_{cap}$ as well as integrated cross-sections $\sigma_{int.}$, resulting in better agreement with experimental data for $^{16}{\rm{O}}$-induced reactions with $^{148}{\rm{Nd}}$, $^{149-150}{\rm{Sm}}$, and $^{32}{\rm{S}}$-induced reactions with $^{150}{\rm{Sm}}$. We conclude that the incorporation of deformations of all orders up to $\beta_4$ at their optimized compact and elongated configurations is essential because it provides better outcomes compared to the optimized configurations of $\beta_2$ and $\beta_3$ deformed nuclei.
Current Issued
Chinese Physics C
2025 Vol. 49, No. 4
Published: 28 March 2025
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Chinese Physics C
IF: 3.6

Monthly issued, founded in 1977

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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
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