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In stellar environments nuclei appear at finite temperatures, becomingextremely hot in core-collapse supernovae and neutron star mergers. However,due to theoretical and computational complexity, most model calculations ofnuclear properties are performed at zero temperature, while those existing atfinite temperatures are limited only to selected regions of the nuclide chart.In this study we perform the global calculation of nuclear properties foreven-even $8 \leq Z \leq 104$ nuclei at temperatures in range $0\le T \le 2$MeV. Calculations are based on the finite temperature relativisticHartree-Bogoliubov model supplemented by the Bonche-Levit-Vautherin vaporsubtraction procedure. We find that near the neutron-drip line the continuumstates have significant contribution already at moderate temperature $T\approx1$ MeV, thus emphasising the necessity of the vapor subtraction procedure.Results include neutron emission lifetimes, quadrupole deformations, neutronskin thickness, proton and neutron pairing gaps, entropy and excitation energy.Up to the temperature $T\approx 1$ MeV nuclear landscape is influenced onlymoderately by the finite-temperature effects, mainly by reducing the pairingcorrelations. As the temperature increases further, the effects on nuclearstructures become pronounced, reducing both the deformations and the shelleffects.

Global properties of nuclei at finite-temperature within the covariant energy density functional theory