Rotational properties and blocking effects in <i>N</i> = 152 isotones <sup>254</sup>No, <sup>255</sup>Lr, and <sup>256</sup>Rf -

\begin{document}$ N=152 $\end{document} isotones ²⁵⁴No, ²⁵⁵Lr, and ²⁵⁶Rf are investigated using the cranked shell model (CSM), with pairing correlations treated via the particle-number-conserving (PNC) method. The experimentally kinematic moments of inertia are reproduced well by the PNC-CSM calculations, and the contributions to

\begin{document}$ J^{(1)} $\end{document}

from neutrons exhibit remarkable similarities. Compared to ²⁵⁴No, the observed identity of

\begin{document}$ J^{(1)} $\end{document}

in ²⁵⁶Rf is a result of the negligible contribution to

\begin{document}$ J^{(1)} $\end{document}

from the two additional protons partially occupying the

\begin{document}$ \pi [514]7/2 $\end{document}

,

\begin{document}$ \pi [521]1/2 $\end{document}

, and

\begin{document}$ \pi [624]9/2 $\end{document}

orbitals. The increase in

\begin{document}$ J^{(1)} $\end{document}

observed in the odd-A nucleus ²⁵⁵Lr, compared to those of the neighboring even-even isotones ²⁵⁴No and ²⁵⁶Rf, is attributed to the contribution of the proton

\begin{document}$ j^{(1)}([521]1/2) $\end{document}

owing to the blocking of the nucleon on the proton

\begin{document}$ \pi [521]1/2 $\end{document}

orbital. Compared to the case of the heavier isotones ²⁵⁵Lr and ²⁵⁶Rf, the different behavior of the

\begin{document}$ B(E2) $\end{document}

value above

\begin{document}$ \hbar\omega \sim 0.20 $\end{document}

MeV in ²⁵⁴No is predicted to be due to the level

\begin{document}$ \pi [514]7/2 $\end{document}

crossing

\begin{document}$ \pi [521]1/2 $\end{document}

."> Rotational properties and blocking effects in <i>N</i> = 152 isotones <sup>254</sup>No, <sup>255</sup>Lr, and <sup>256</sup>Rf -

[1]
A. Ghiorso, S. G. Thompson, G. H. Higginset al., Phys. Rev.95, 293 (1954)
[2]
P. T. Greenlees, J. Rubert, J. Piotet al., Phys. Rev. Lett.109, 012501 (2012)
[3]
R. D. Herzberg and P. T. Greenlees, Prog. Part. Nucl. Phys.61, 674 (2008)
[4]
I. Ahmad, F. G. Kondev, E. F. Mooreet al., Phys. Rev. C71, 054305 (2005)
[5]
S. Ketelhut, P. T. Greenlees, D. Ackermannet al., Phys. Rev. Lett.102, 212501 (2009)
[6]
I. Ahmad, M. P. Carpenter, R. R. Chasmanet al., Phys. Rev. C44, 1204 (1991)
[7]
R. D. Herzberg, P. T. Greenlees, P. A. Butleret al., Nature442, 896 (2006)
[8]
J. Y. Zeng, Y. A. Lei, T. H. Jinet al., Phys. Rev. C50, 746 (1994)
[9]
J. Y. Zeng, T. H. Jin, and Z. J. Zhao, Phys. Rev. C50, 1388 (1994)
[10]
Z. H. Zhang, X. T. He, J. Y. Zenget al., Phys. Rev. C85, 014324 (2012)
[11]
Y. C. Li and X. T. He, Sci. China: Phys., Mech. Astron.59, 672011 (2016)
[12]
X. T. He and Y. C. Li, Phys. Rev. C98, 064314 (2018)
[13]
Z. H. Zhang, Phys. Rev. C98, 034304 (2018)
[14]
R.-D. Herzberg, N. Amzal, F. Beckeret al., Phys. Rev. C65, 014303 (2001)
[15]
P. Möller, J. R. Nix, W. D. Myerset al., At. Data Nucl. Data Tables59, 185 (1995)
[16]
S. X. Liu, J. Y. Zeng, and E. G. Zhao, Phys. Rev. C66, 024320 (2002)
[17]
R. R. Chasman, I. Ahmad, A. M. Friedmanet al., Rev. Mod. Phys.49, 833 (1977)