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