Thermal conductivity (upper panel) and heat capacity per baryon in units of k_B (lower panel) as functions of mass density at age t = 1 kyr for the same neutron star models as in Fig. 6. The crosses mark the melting points for the models with M = 1.4 M_⊙: to the left of them, the Coulomb plasma forms a liquid ocean. For the M = 1.8 M_⊙ model, the crust does not melt in the displayed density range, because it is relatively cold at this age (cf. Fig. 4). The vertical dotted lines mark the outer and inner boundaries of the inner crust.