Pressure vs. energy density (ε) relations for various β-stable EOSs derived in different thermodynamical stellar conditions. Left (right) panel: we use a logarithmic (linear) scale. The BL T = 0 (black continuous line) taken from Bombaci & Logoteta (2018) is shown for reference. We note that for the BL EOS for nuclear densities below 0.08 fm⁻³, the Sly4 EOS (Haensel & Pichon 1994; Douchin & Haensel 2001) has been adopted (Endrizzi et al. 2018). The BLh with T = 0.1 MeV is represented by the black dashed line. Red and blue curves refer to the following cases: isoentropic EOS with S/A = 1 and S/A = 2 without neutrino trapping (red dashed lines) and isoentropic EOS with S/A = 1 and S/A = 2 with neutrino trapping (blue continuous and dashed lines). For the low-density part of the BLh EOSs, we employ the TM1 model (Sugahara & Toki 1994). Temperatures (T) in the figure are in MeV. (See text for further details).