Speaker
Description
The dynamical role of the spin-orbit (SO) coupling is a crucial, but not fully understood, aspect in the description of heavy-ion collisions. We investigate this influence using three-dimensional Time-Dependent Hartree-Fock (TDHF) calculations with the SKY3D code. This study simulates heavy-ion collisions ($Z=6-36$, with neutron numbers $N$ from $Z-4$ to $Z+4$) at a center-of-mass kinetic energy of $E_{\rm cm} = A + e Z^2 / 4R$, with the nuclear radius defined as $R = 1.2 A^{1/3}$ fm. We focus on the effect of the SO coupling on the collective oscillation of the dinuclear system formed during the collision. From the oscillation period $T$, we extract the corresponding restoring force coefficient, $k$, defined as $k = 4\pi^2 \mu / T^2$, where $\mu$ is the reduced mass of the system. Our analysis reveals that $k$ is strongly correlated with the total number of nucleons, $A$. For lighter systems (small $A$), the restoring force is stronger when the SO interaction is included. In contrast, for heavier systems (large $A$), the calculation without the SO force produces a stronger restoring force. In particular, a distinct peak in the restoring force coefficient is observed around $A \approx 60$ in simulations performed without the SO interaction. By examining a broad mass range, we aim to identify clear signatures of the SO interaction in the dynamical situation. This work aims to enhance the understanding of both spin-dependent dynamics and nuclear energy density functionals.
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