Axial Symmetric Solutions to Einstein's Field Equations for Deformed Neutron Stars

ORAL

Abstract

Traditional models of neutron stars are constructed under of assumption that they are perfect spheres. This is not correct, however, if the matter inside of neutron stars is described by an non-isotropic model for the equation of state. Examples of such stars are magnetars and neutron stars that would contain color-superconducting quark matter. In this work, we derive the stellar structure equations which describe the properties of non-isotropic neutron stars. The equations are solved numerically in two dimensions. We calculate stellar properties such as masses and radii along with pressure and density profiles and investigate any changes from conventional spherically symmetric neutron stars.

*This work was supported through the National Science Foundation under grants PHYS-1411708 and DUE-1259951. Additional computing resources were provided by the CSRC at SDSU and the Department of Sciences at Wentworth Institute of Technology.

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Authors

  • Omair Zubairi

    • Department of Sciences, Wentworth Institute of Technology

  • Fridolin Weber

    • Department of Physics, San Diego State University & Center for Astrophysics and Space Sciences, University of California, San Diego
    • Department of Physics, San Diego State University and Center for Space Sciences, University of California, San Diego