The Lifshitz-Kosevich-Shoenberg theory of relativistic electronic gas in neutron stars

The Diamagnetic Phase Transition of Dense Electron Gas: Astrophysical Applications

“…Then, the above theory and calculations about the electron gas magnetization cannot be applied. In this case, matter behavior and the equation of state at the thermodynamical equilibrium or the nonequilibrium β-process have been studied in Lai & Shapiro (1991); Chamel et al (2012); Basilico et al (2015); Wang et al (2014), etc. In Wang et al (2014), we have analytically calculated the magnetization of the electron gas acted with strongly quantizing magnetic field.…”

“…In this case, matter behavior and the equation of state at the thermodynamical equilibrium or the nonequilibrium βprocess have been studied in Lai & Shapiro (1991), Chamel et al (2012), Basilico et al (2015), Wang et al (2014), etc. In Wang et al (2014), we have analytically calculated the magnetization of the electron gas acted with strongly quantizing magnetic field. The magnetization exhibits also the similar oscillatory behavior as that described by Equation (4).…”

“…Actually, Shoenberg (1984) suggested the largest quantum number r max >2. If r max 2, the diamagnetic phase does not really occur in spite of the similar oscillation property of Equation (4) (Wang et al 2014). Chamel et al (2012) has given the out crust structure and composition of a neutron star based on experimental data of atomic mass and complemented with theoretical prediction of the Hartree-Fock-Bogoliubov method (Goriely et al 2010).…”