[en] Condensed matter at very high pressure is viewed as a collection of squeezed atoms, which are described in terms of a statistical model. A very strong magnetic field is supposed to be present, and temperature effects are taken into account, but exchange is neglected, because at nonzero temperature its effect tends to be canceled by long-range correlations. The free energy of such an atom can be calculated explicitly as a function of the appropriate variables, after which the thermodynamic properties are derived by standard methods. For canonical pulsars, with an iron crust having already cooled down to about 10⁵ K, and surface magnetic fields of the order of 10¹² G, temperature corrections turn out to be negligible. However, they represent sizable effects in the case of very young and hot pulsars