Antonov, A. N.Kadrev, D. N.Gaidarov, M. K.Sarriguren, P.Moya de Guerra, Elvira2023-06-172023-06-172017-02-142469-998510.1103/PhysRevC.95.024314https://hdl.handle.net/20.500.14352/17804© American Physical Society 2017 E. Moya de Guerra and O. Moreno acknowledge MINECO for partial financial support (FIS2014-51971-P) and IEM-CSIC for hospitality. O. Moreno acknowledges support from a Marie Curie International Outgoing Fellowship within the European Union Seventh Framework Programme, under Grant Agreement PIOF-GA-2011-298364 (ELECTROWEAK). M. R. M. thanks N. G. Sanchez for correspondence and conversations.The temperature dependence of the symmetry energy for isotopic chains of even-even Ni, Sn, and Pb nuclei is investigated in the framework of the local density approximation (LDA). The Skyrme energy density functional with two Skyrme-class effective interactions, SkM* and SLy4, is used in the calculations. The temperature-dependent proton and neutron densities are calculated through the HFBTHO code that solves the nuclear Skyrme-Hartree-Fock-Bogoliubov problem by using the cylindrical transformed deformed harmonic-oscillator basis. In addition, two other density distributions of Pb-208, namely the Fermi-type density determined within the extended Thomas-Fermi (TF) method and symmetrized-Fermi local density obtained within the rigorous density functional approach, are used. The kinetic energy densities are calculated either by the HFBTHO code or, for a comparison, by the extended TF method up to second order in temperature (with T-2 term). Alternative ways to calculate the symmetry energy coefficient within the LDA are proposed. The results for the thermal evolution of the symmetry energy coefficient in the interval T = 0-4 MeV show that its values decrease with temperature. The temperature dependence of the neutron and proton root-mean-square radii and corresponding neutron skin thickness is also investigated, showing that the effect of temperature leads mainly to a substantial increase of the neutron radii and skins, especially in the more neutron-rich nuclei, a feature that may have consequences on astrophysical processes and neutron stars.engjournal articlehttp://dx.doi.org/10.1103/PhysRevC.95.024314https://journals.aps.org/open access539.1Weak interaction ratesDensity profileShell nucleiGalaxiesMassBoundsTests.Física nuclear2207 Física Atómica y Nuclear