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Résumé |
Understanding nuclear structure and dynamics at finite temperatures is of
crucial importance in both nuclear physics and nuclear astrophysics since the
nuclei in the universe appear at finite temperatures; examples include the late
stages of core-collapse supernovae and neutron star mergers [1]. Up until now,
the nuclear energy density functional (NEDF) theory has become the standard tool
to explore nuclear properties across the entire nuclide chart. However, the
majority of large-scale calculations conducted so far have focused on nuclear
properties at zero temperatures, overlooking the relevance of nuclei at finite
temperatures. To address this, we have recently developed the relativistic
finite temperature Hartree-Bogoliubov (FT-RHB), which also includes treatment of
thermal scattering of nucleons in the continuum. Then, we mapped the nuclear
landscape at temperatures up to around 20 billion kelvins [2,3].\newline
In this talk, I will present our findings on the temperature dependence of
various nuclear properties as well as the nuclear drip lines, and discuss the
significant impact of temperature on these properties by comparing the results
with the calculations at zero temperature. Our findings shed light on the
nuclear landscape for hot nuclei, indicating that nuclear drip lines should be
considered as limits that change dynamically with temperature.\\
1. F. Osterfeld, Rev. Mod. Phys. 64, 491 (1992). \newline
2. A. Ravlić, E. Yüksel, T. , N. Paar, Nat. Commun. 14 (1), 4834 (2023).\newline
3. A. Ravlić, E. Yüksel, T. Nikšić, N. Paar, Phys. Rev. C 109, 014318 (2024). |
