Table 1:
Critical temperature (in K) below which a condensed phase exists at P = 0, for several magnetic field strength B _{12} = B / 10^{12} 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. [31, 32] including pairing correlations (their P2 model). The boundary conditions are the same as those of Negele and Vautherin [303]. 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. |

Table 5:
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. [69] based on diagrammatic calculations (shown in Figure 46) and RG – pairing gap of Schwenk et al. [366] based on the Renormalization Group approach (shown in Figure 46). is given in MeV. , , and are given in fm ^{–1}. |

Table 6:
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 . |

http://www.livingreviews.org/lrr-2008-10 |
This work is licensed under a Creative Commons License. Problems/comments to |