List of Tables

Table 1:
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 [287].
Table 2:
Sequence of nuclei in the ground state of the outer crust of neutron star calculated by Rüster et al. [357] using experimental nuclear data (upper part), and the theoretical mass table of the Skyrme model BSk8 (lower part).
Table 3:
Sequence of nuclear clusters in the ground state of the inner crust calculated by Negele & Vautherin [303]. 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.
Table 4:
Sequence of nuclear clusters in the ground state of the inner crust calculated by Baldo et al. [3132] including pairing correlations (their P2 model). The boundary conditions are the same as those of Negele and Vautherin [303]. Similarly, N 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.
Table 5:
Parameters for the analytic formula Equation (134View Equation) of a few representative 1S0 pairing gaps in pure neutron matter: BCS-BCS pairing gap shown in Figure 45View Image, Brueckner – pairing gap of Cao et al. [69] based on diagrammatic calculations (shown in Figure 46View Image) and RG – pairing gap of Schwenk et al. [366] based on the Renormalization Group approach (shown in Figure 46View Image). Δ0 is given in MeV. k1, k2, k3 and kmax are given in fm–1.
Table 6:
Main neutrino emission processes in neutron star crusts. Symbols: γ stands for a photon or a plasmon; (A, Z ) stands for a nucleus with charge number Z and mass number A; lepton symbol x = e,μ,τ; neutron quasiparticle (neutron-like elementary excitation) in superfluid neutron gas is denoted by ^n.