Pressure of Degenerate and Relativistic electrons in a superhigh magnetic field

Abstract

Based on our previous work, we deduce a general formula for pressure of degenerate and relativistic electrons,Pe, which is suitable for superhigh magnetic fields, discuss the quantization of Landau levels of electrons, and consider the quantum electrodynam-ic(QED) effects on the equations of states (EOSs) for different matter systems. The main conclusions are as follows:Pe is related to the magnetic field B, matter density ?, and electron fraction Ye ; the stronger the magnetic field, the higher the electron pressure becomes; the high electron pressure could be caused by high Fermi energy of electrons in a superhigh magnetic field; compared with a common radio pulsar, a magnetar could be a more compact oblate spheroid-like deformed neutron star due to the anisotropic total pressure; and an increase in the maximum mass of a magnetar is expected because of the positive contribution of the magnetic field energy to the EOS of the star.

26 Papers, 5 Figures, Published in Modern Physics Letters A ., Vol.28, No.36, p.1350138 (2013)

References in corpus (13)

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Cited by in corpus (8)

• Constraining the Braking Indices of Magnetars
• The Dipole Magnetic Field and Spin-down Evolutions of The High Braking Index Pulsar PSR J1640-4631
• Numerically Fitting The Electron Fermi Energy and The Electron Fraction in A Neutron Star
• Modified Fermi Energy of Electrons in a Superhigh Magnetic Field
• General Relativistic Calculations for White Dwarf Stars
• Strong screening effects on resonant nuclear reaction ${}^{23}$Mg $(p,\gamma )$ ${}^{24}$Al in the surface of magnetars
• On the pulsar spin frequency derivatives and the glitch activity
• The Low-Frequency Spectra of Radio Pulsars