Abstract

Neutron star is an important object for us to verify the equation of state of hadronic matter. For a specific choice of equations of state, mass and radius of a neutron star are determined, for which there are constraints from observations. According to some previous studies, since the strong magnetic field acts as a repulsive force, there is a possibility that neutron stars with strong magnetic fields may have relatively heavier masses than other non-magnetized neutron stars. In this paper, the structure of a neutron star with a strong internal magnetic field is investigated by changing its internal functional form to see how much the neutron star can be massive and also how radius of a neutron star can be within a certain range.

Highlights

  • To study a neutron star (NS) is an interesting and important subject in nuclear physics as it is a unique object of superdense hadronic matter, where its central density might be several times larger than the nuclear saturation density

  • Equation of state (EoS) for the nuclear matter that depends on the energy density functional is often utilized to discuss various properties of NSs, for instance, the mass–radius (MR) relation

  • Each EoS curve must go through these areas if they satisfy the observational constraints

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Summary

Introduction

To study a neutron star (NS) is an interesting and important subject in nuclear physics as it is a unique object of superdense hadronic matter, where its central density might be several times larger than the nuclear saturation density. This leads to a reduction in the Fermi pressure to soften the EoS and to a reduction in the predicted maximum mass less than 2 M. To obtain NS masses more than 2 M is one of the goals to be achieved for the optimal EoSs. There are some characteristic NSs: millisecond-pulsar, which has a short rotational period of less than 10 ms, and magnetar, which has a powerful magnetic field on its surface. These EoSs have similar saturation properties at nuclear saturation density This RMF includes a strong magnetic field, which has a functional form of baryon number density ρ.

Equation of State
Magnetic Fields
EoS of Hadronic Matter with Magnetic Fields
Comparison of the Case without Magnetic Fields
Changing α and γ Parameters of the Magnetic Field Function

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