Abstract
As we know, the effect of strong magnetic field causes the anisotropy for the magnetized compact objects. Therefore, in this paper, we have studied the structure properties of anisotropic case of magnetized neutron star. We have derived the equation of state (EoS) of neutron star matter for two forms of magnetic fields, one uniform and one density dependent. We have solved the generalized Tolman–Oppenheimer–Volkoff equations to examine the maximum mass and corresponding radius, Schwarzschild radius, gravitational redshift, Kretschmann scalar, and Buchdahl theorem for this system. It was shown that the maximum mass and radius of neutron star are increasing functions of the magnetic field. Also redshift, strength of gravity, and Kretschmann scalar increase as the magnetic field increases. In addition, the dynamical stability of anisotrop neutron star has been investigated, and finally a comparison with the empirical results has been made.
Highlights
equation of state (EoS) in a strong uniform magnetic field is that the pressure is anisotropic [5,6]
In the present work, we consider the anisotropic case of magnetized neutron star which contains pure neutron matter to evaluate its structure properties. For this purpose we calculate the energy of neutron matter by the lowest order constrained variational (LOCV) method in the presence of magnetic field, and use it to obtain the EoS for this star [34– 36]
We calculated the equation of state of magnetized neutron star that contains pure neutron matter in the presence of an strong magnetic field
Summary
EoS in a strong uniform magnetic field is that the pressure is anisotropic [5,6]. It is proposed that the magnetic field arises naturally in neutron stars as a consequence of thermal effects occurring in their outer crusts. When the magnetic fields in a neutron star are strong, the effects of the magnetic field cause anisotropy in the components of the energy–momentum tensor, creating two components of pressure. The interest in studying the distribution of anisotropic relative matter in general relativity has been revived by Bowers and Liang [24]. They set up and solved the equations of hydrostatic equilibrium for a locally anisotropic, static, and spherically symmetric distribution of matter. They found a change in maximum mass M and surface redshift z. To solve the mathematical problem of developing anisotropic fluid sphere models for a coupled system of three independent nonlinear partial differential equations in five geometric and dynamic variables namely metric potentials (ν) and (λ) and density (ρ), radial pressure ( pr ) and tangential pressure
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