The Influence of the Magnetic Field on the Properties of Neutron Star Matter
نویسندگان
چکیده
In the mean field approximation of the relativistic σ-ω-ρ model, the magnetic fields are incorporated, and its influence on the properties of n-p-e neutron star matter are studied. When the strength of the magnetic field is weaker than ∼ 10G, the particle fractions and chemical potentials, matter energy density and pressure hardly change with the magnetic field; when the strength of the magnetic field is stronger than ∼ 10G, the above quantities change with the magnetic field evidently. Furthermore, the pressure is studied in both thermodynamics and hydrodynamics. The difference between these two ways exits in the high density region, that is, the thermal self-consistency may not be satisfied in this region if the magnetic field is considered.
منابع مشابه
Different Magnetic Field Distributions in Deformed Neutron Stars
In this work, we review the formalism which would allow us to model magnetically deformed neutron stars. We study the effect of different magnetic field configurations on the equation of state (EoS) and the structure of such stars. For this aim, the EoS of magnetars is acquired by using the lowest order constraint variational (LOCV) method and employing the AV18 potential....
متن کاملNon-Relativistic Limit of Neutron Beta-Decay Cross-Section in the Presence of Strong Magnetic Field
One of the most important reactions of the URCA that lead to the cooling of a neutron star, is neutron beta-decay ( ). In this research, the energy spectra and wave functions of massive fermions taking into account the Anomalous Magnetic Moment (AMM) in the presence of a strong changed magnetic field are calculated. For this purpose, the Dirac-Pauli equation for charged and neutral fermions is ...
متن کاملEffect of Isovector-scalar Meson on Neutron Star Matter in Strong Magnetic Fields
We study the effects of isovector-scalar meson δ on the equation of state (EOS) of neutron star matter in strong magnetic fields. The EOS of neutron-star matter and nucleon effective masses are calculated in the framework of Lagrangian field theory, which is solved within the mean-field approximation. From the numerical results one can find that the δ-field leads to a remarkable splitting of pr...
متن کاملSpin and Isospin Asymmetry, Equation of State and Neutron Stars
In the present work, we have obtained the equation of state for neutron star matter considering the in uence of the ferromagnetic and antiferromagnetic spin state. We have also investigated the structure of neutron stars. According to our results, the spin asymmetry stiens the equation of state and leads to high mass for the neutron star.
متن کاملMagnetic and spin evolution of isolated neutron stars with the crustal magnetic field
We consider the magnetic and spin evolution of isolated neutron stars assuming that the magnetic field is initially confined to the crust. The evolution of the crustal field is determined by the conductive properties of the crust which, in its turn, depend on the thermal history of the neutron star. Due to this fact, a study of the magnetic field decay may be a powerful diagnostic of the proper...
متن کامل