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. [31, 32] including pairing correlations (their P2 model). The boundary conditions are the same as those of Negele and Vautherin [303]. Similarly, ![]() |
Table 5:
Parameters for the analytic formula Equation (134 ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
Table 6:
Main neutrino emission processes in neutron star crusts. Symbols: ![]() ![]() ![]() ![]() ![]() ![]() |
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