Critical temperature (in K) below which a condensed phase exists at P = 0, for several magnetic field strength B12 = B / 1012 G and matter composition. From .
Sequence of nuclei in the ground state of the outer crust of neutron star calculated by Rüster et al.  using experimental nuclear data (upper part), and the theoretical mass table of the Skyrme model BSk8 (lower part).
Sequence of nuclear clusters in the ground state of the inner crust calculated by Negele & Vautherin . Here N is the total number of neutrons in the Wigner–Seitz sphere (i.e., it is a sum of the number of neutrons bound in nuclei and of those forming a neutron gas, per nucleus). Isotopes are labelled with the total number of nucleons in the Wigner–Seitz sphere.
Sequence of nuclear clusters in the ground state of the inner crust calculated by Baldo et al. [31, 32] including pairing correlations (their P2 model). The boundary conditions are the same as those of Negele and Vautherin . Similarly, is the total number of neutrons in the Wigner–Seitz sphere. The isotopes are labelled with the total number of nucleons in the Wigner–Seitz sphere, as in Table 3.
Parameters for the analytic formula Equation (134) of a few representative pairing gaps in pure neutron matter: BCS-BCS pairing gap shown in Figure 45, Brueckner – pairing gap of Cao et al.  based on diagrammatic calculations (shown in Figure 46) and RG – pairing gap of Schwenk et al.  based on the Renormalization Group approach (shown in Figure 46). is given in MeV. , , and are given in fm–1.
Main neutrino emission processes in neutron star crusts. Symbols: stands for a photon or a plasmon; stands for a nucleus with charge number and mass number ; lepton symbol ; neutron quasiparticle (neutron-like elementary excitation) in superfluid neutron gas is denoted by .
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