Magnetized Fermi Gas in the Outer Shell of Neutron Stars

傅寬裕(K. Y. Fu)

Chinese Journal of Physics

13卷2期（1975 / 10 / 01）

183 - 187

英文

The stress anisotropy and the degenerate behaviors of a magnetized Fermi gas in the outer shell of neutron stars have been investigated. The main purpose of this investigation is to study the influence of the magnetized Fermi gas on the equilibrium structure of neutron stars during their cooling process. In the approximation of degeneracy limit, the normal stresses have discontinuous derivatives with respect to the chemical potential, and the chemical potential decreases as the temperature approaches zero. These results demonstrate either a rapid decrease of the pressure or a discontinuity of the pressure gradient in the outer shell of neutron stars as they are cooling down. This leads us to propose that the starquake, which is adopted to account for the pulsar ”glitches”, can be triggered in the outer shell of neutron stars. For this triggering process to be effective, we need a magnetic field of strength ≥10^(14) gauss for the Vela ones.