\begin{document}$ T/U $\end{document}) for even-even nuclei in their ground states. Notably, the nuclei with maximal value of \begin{document}$ T/U $\end{document} are generally stable for a certain isobaric chain with \begin{document}$ Z\le 82 $\end{document}. However, the known magic numbers can be more clearly observed from the \begin{document}$ T/U $\end{document}ratio than from nuclear binding energy, particularly for the isobaric chains with semi-magic nuclei. Combining the predicted binding energies and the \begin{document}$ T/U $\end{document} ratios from the Skyrme Hartree-Fock-Bogoliubov (HFB) code transformed harmoic oscilattor (HFBTHO) with the parameter set based on the Universal Nuclear Energy Density Funcitonal (UNEDF0), the possible magic numbers in super-heavy mass region were simultaneously studied. The neutron magic number \begin{document}$ N=184 $\end{document} can be clearly observed from the calculated values of \begin{document}$ T/U $\end{document} and the extracted microscopic energies of the nuclei."> Nuclear stability and ratio of kinetic to potential energy -
  • [1]

    W. D. Myers and W. J. Swiatecki, Nucl. Phys. A81(1), 1 (1966)

  • [2]

    S. G. Nilsson, J. R. Nix, A. Sobiczewski,et al., Nucl. Phys. A115(3), 545 (1968)

  • [3]

    S. G. Nilsson, C. F. Tsang, A. Sobiczewski,et al., Nucl. Phys. A131(1), 1 (1969)

  • [4]

    M. Bender, W. Nazarewicz and P. G. Reinhard, Phys. Lett. B515, 42 (2001)

  • [5]

    A. T. Kruppa, M. Bender, W. Nazarewicz,et al., Phys. Rev. C61, 034313 (2000)

  • [6]

    K. Morita, K. Morimoto, D. Kaji,et al., J. Phys. Soc. Jpn.73(10), 2593 (2004)

  • [7]

    K. Morita, K. Morimoto, D. Kaji,et al., J. Phys. Soc. Jpn.76(4), 045001 (2007)

  • [8]

    Y. T. Oganessian, A. V. Yeremin, A. G. Popeko,et al., Nature400, 242 (6741)

  • [9]

    Y. T. Oganessian, F. S. Abdullin, P. D. Bailey,et al., Phys. Rev. C63, 011301 (2000)

  • [10]

    Y. T. Oganessian, V. K. Utyonkov, Yu. V. Lobanov,et al., Phys. Rev. C74, 044602 (2006)

  • [11]

    Y. T. Oganessian, F. S. Abdullin, P. D. Bailey,et al., Phys. Rev. Lett.104, 142502 (2010)

  • [12]

    Y. T. Oganessian, F. S. Abdullin, S. N. Dmitriev,et al., Phys. Rev. C87, 014302 (2013)

  • [13]

    S. Ćwiok, P. H. Heenen and W. Nazarewicz, Nature433, 705 (7027)

  • [14]

    J. M. Lattimer and M. Prakash, Astrophys. J.550, 426 (2001)

  • [15]

    F. Özel, D. Psaltis, T. Güver,et al., Astrophys. J.820, 28 (2016)

  • [16]

    J. Dobaczewski, H. Flocard and J. Treiner, Nucl. Phys. A422, 103 (1984)

  • [17]

    M. V. Stoitsov, J. Dobaczewski, W. Nazarewicz,et al., Comput. Phys. Commun.167, 43 (2005)

  • [18]

    M. V. Stoitsov, N. Schunck, M. Kortelainen,et al., Comput. Phys. Commun.184, 1592 (2013)

  • [19]

    G. Scamps, S. Goriely, E. Olsen,et al., Eur. Phys. J. A57, 333 (2021)

  • [20]

    S. Goriely, N. Chamel, and J.M. Pearson, Phys. Rev. Lett.102, 152503 (2009)

  • [21]

    M. Bender, P. H. Heenen and P. G. Reinhard, Rev. Mod. Phys.75, 121 (2003)

  • [22]

    Y. El Bassem and M. Oulne, Nucl. Phys. A957, 22 (2017)

  • [23]

    Ali H. Taqi, Malik A. Hasan, Arab. J. Sci. Eng.47, 761 (2022)

  • [24]

    M. Kortelainen, T. Lesinski, J. Moré,et al., Phys. Rev. C82, 024313 (2010)

  • [25]

    E. Chabanat, P. Bonche, P. Haensel,et al., Nucl. Phys. A635, 231 (1998)

  • [26]

    J. Bartel, P. Quentin, M. Brack,et al., Nucl. Phys. A386, 79 (1982)

  • [27]

    M. Beiner, H. Flocard, N. Van Giai,et al., Nucl. Phys. A238, 29 (1975)

  • [28]

    M. Wang, W. J. Huang, F. G. Kondev,et al., Chin. Phys. C45, 030003 (2021)

  • [29]

    Alex E. S. Green, Phys. Rev.99, 1410 (1955)

  • [30]

    H. A. Bethe and R. F. Bacher, Rev. Mod. Phys.8, 82 (1936)

  • [31]

    N. Wang, M. Liu and X. Z. Wu, Phys. Rev. C81, 044322 (2010)

  • [32]

    N. Wang, M. Liu, X. Z. Wu,et al., Phys. Lett. B734, 215 (2014)

  • [33]

    P. Möller, J. R. Nix, W. D. Myers,et al., At. Data Nucl. Data Tables59(2), 185 (1995)

Baidu
map