Erratum: Proto-neutron star structure within an extended lowest-order constrained variational method at finite temperature [Phys. Rev. C 92, 035806 (2015)]

Figure 6

Revised version of Fig. 6 in the original paper. (a) Free energy per baryon of the symmetric nuclear matter as a function of density for different values of temperature with and without the TBF. (b) The same as panel (a) but for the pure neutron matter.

Figure 7

Revised version of Fig. 7 in the original paper. (a) The temperature of the PNS matter as a function of baryon density for different values of entropy per baryon obtained with and without the TBF for $Y_e=0.3$. (b) The same as panel (a) but for $Y_e=0.4$.

Figure 10

Revised version of Fig. 10 in the original paper. Relative population of the constituents of the PNS core calculated by using the AV18 $+$ TBF potential and for $Y_e=0.3$ and $S/A=1$. (b) The same as panel (a) but for $S/A=2$.

Figure 11

Revised version of Fig. 11 in the original paper. Relative population of the constituents of the PNS core calculated by using the AV18 $+$ TBF potential and for $Y_e=0.4$ and $S/A=1$. (b) The same as panel (a) but for $S/A=2.$

Figure 12

Revised version of Fig. 12 in the original paper. (a) The EOS of the proto-neutron star with $Y_e=0.3$ calculated with and without the TBF for some fixed values of the entropy per baryon. (b) The same as panel (a) but for $Y_e=0.4$.

Figure 13

Revised version of Fig. 13 in the original paper. (a) The mass-radius relation of the proto-neutron star with $Y_e=0.3$ calculated with and without the TBF for some fixed values of the entropy per baryon. (b) The same as panel (a) but for $Y_e=0.4$.