Deformed neutron stars
arxiv(2024)
Abstract
We present solutions for non-spherically symmetric neutron stars. We begin by
deriving the Tolman-Oppenheimer-Volkoff equations from a parameterized metric
that takes into account the deformation of the star due to differences in
equatorial and polar pressures, expressed in terms of a parameter D, which is
the ratio between polar and equatorial radius. The stellar structure is solved
using the GM1 equation of state and the Tolman-Oppenheimer-Volkoff equations
for deformed objects are numerically integrated using the fourth-order
Runge-Kutta method for different values of the parameter D. We show that larger
values of D > 1, that describe prolate neutron stars, yield smaller values of
mass and radius, while for smaller values of D < 1, describing oblate neutron
stars, larger values for mass and radius are attained. From the confrontation
of our model theoretical predictions with recent observational data on pulsars,
it is possible to constrain the values of the parameter D.
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