Self consistent models of deformed neutron stars in the framework of general relativity

10th Biennial Conference on Classical and Quantum Relativistic Dynamics of Particles and Fields

Zubairi, Omair^1 ; Weber, Fridolin^2,3

Department of Sciences, Wentworth Institute of Technology, 550 Huntington Ave, Boston

MA

02115, United States^1

Department of Physics, San Diego State University, 5500 Campanile Drive, San Diego

CA

92182, United States^2

Center for Astrophysics and Space Sciences, University of California, San Diego, 9500 Gilman Drive, San Diego

CA

92093, United States^3

关键词: Energy density profile;    Equation of state;    General Relativity;    Isotropic models;    Self-consistent model;    Spherical models;    Spherical symmetry;    Stellar structure;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/845/1/012005/pdf
DOI  :  10.1088/1742-6596/845/1/012005

来源: IOP

【 摘 要 】

Generally, over the last 75 years, since the publication of the well known papers from from R. C. Tolman (Tolman 1939) and J. R. Oppenheimer and G. M. Volkoff (Oppenheimer and Volkoff 1939), standard models of non-rotating neutron stars are modeled with the assumption that they are perfect spheres. This assumption of perfect spherical symmetry is not correct if the matter inside of neutron stars is described by a non-isotropic equation of state (EoS). Particular classes of neutron stars such as Magnetars and neutron stars that contain color superconducting quark matter cores are expected to be deformed making them oblong spheroids. In this paper, we examine the deformity of these non-spherical neutron stars by deriving the stellar structure equations in the framework of general relativity. Using a non-isotropic model for the equation of state, these stellar structure equations are solved numerically in two dimensions. We then calculate stellar properties such as masses and radii along with pressure and energy-density profiles and investigate any changes from conventional spherical models.