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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  • A three-body form factor at sub-leading power in the high-energy limit: planar contributions
    Yishuai Guo, Zhi-Feng Liu, Mingming Lu, Tianya Xia, Li-Lin Yang
    2025, 49(9): 093102-093102-14. doi: 10.1088/1674-1137/addcc7
    Show Abstract
    We analyzed two-loop planar contributions to a three-body form factor at next-to-leading power in the high-energy limit, where the masses of the external particles are much smaller than their energies. Calculations were performed by exploiting differential equations for the expansion coefficients, both to facilitate linear relations among them and to derive their analytic expressions. The results are expressed in terms of generalized polylogarithms involving a few simple symbol letters. Our method can readily be applied to calculations of non-planar contributions as well. Our results provide crucial information for establishing sub-leading factorization theorems for massive scattering amplitudes in the high-energy limit.
  • α-decay half-lives of superheavy nuclei within a one-parameter model
    Li-Qian Qi, Hong-Min Wang, Jian-Po Cui, Yan-Zhao Wang, Jian-Zhong Gu
    2025, 49(9): 094102-094102-11. doi: 10.1088/1674-1137/addcc8
    Show Abstract
    The α-decay half-lives of superheavy nuclei (SHN) with charge numbers $ Z \geq 104 $ are investigated by employing a phenomenological one-parameter model based on quantum-mechanical tunneling through a potential barrier, where both the centrifugal and overlapping effects have been considered. It is shown that the experimental α-decay half-lives of the 81 SHN are reproduced well. Moreover, the order of magnitude for the α-particle preformation probability inside a parent nucleus ($S_{ {\alpha }} $) is found to be $ 10^{-2} $. Then, within this model, the $S_{ {\alpha }} $ values and α-decay half-lives of Z = 118−120 isotopes are predicted by inputting the α-decay energies ($ Q_{\alpha } $) extracted from the relativistic continuum Hartree-Bogoliubov (RCHB) theory, Duflo-Zuker 19 (DZ19, where 19 denotes the number of fitting parameters) model, improved Weizsacker-Skyrme (lMWS) model, and machine learning (ML) approach. By analyzing the evolutions of $ Q_{\alpha } $, $S_{ {\alpha} }$ and α-decay half-lives of Z = 118−120 isotopes with the neutron number N of the parent nucleus, it is found that the shell effect at N = 184 is evident for all nuclear mass models. Meanwhile, for the case of the RCHB, N = 172 is determined as a submagic number. However, the submagic number at N = 172 is replaced by N = 178 for the ML approach.
  • Investigating the shadows of new regular black holes with a Minkowski core: effects of spherical accretion and core type differences
    Yi Xiong, Jin Pu, Yi Ling, Guo-Ping Li, Gao-Ming Deng
    2025, 49(9): 095101-095101-13. doi: 10.1088/1674-1137/addfce
    Show Abstract
    We investigated the shadows and optical appearances of a new type of regular black holes (BHs) with a Minkowski core under various spherical accretion scenarios. These BHs are constructed by modifying the Newtonian potential based on the minimum observable length in the Generalized Uncertainty Principle (GUP). They correspond one-to-one with traditional regular BHs featuring a de-Sitter (dS) core (such as Bardeen/Hayward BHs), characterized by a quantum gravity effect parameter ($ \alpha_0 $) and spacetime deformation factor (n). We found that the characteristic parameters give rise to some novel observable features. For these new BHs, both the shadow and photon sphere radii decrease with the increase in $ \alpha_0 $, while the observed specific intensity increases. Conversely, as n increases, the shadow and photon sphere radii increase, while the observed specific intensity decreases. Under different spherical accretion scenarios, the shadows and photon sphere radii remain identical; however, the observed specific intensity is greater under static spherical accretion than under infalling spherical accretion. Additionally, we found that these regular BHs with different cores exhibit variations in shadows and optical appearances, particularly under static spherical accretion. Compared with Bardeen BH, the new BHs exhibit a lower observed specific intensity, a dimmer photon ring, and smaller shadow and photon sphere radii. Larger values of $ \alpha_0 $ lead to more significant differences, and a similar trend was also observed when comparing with Hayward BH. Under infalling spherical accretion, the regular BHs with different cores exhibit only slight differences in observed specific intensity, which become more evident when $ \alpha_0 $ is relatively large. This suggests that the unique spacetime features of these regular BHs with different cores can be distinguished through astronomical observation.
Current Issued
Chinese Physics C
2025 Vol. 49, No. 8
Published: 01 August 2025
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Chinese Physics C
IF: 3.6

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ISSN 1674-1137 CN 11-5641/O4

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