Analytical approximation of the exterior gravitational field of rotating neutron stars
arXiv:1102.5252 · doi:10.1088/0264-9381/28/15/155015
Abstract
It is known that Bäcklund transformations can be used to generate stationary axisymmetric solutions of Einstein's vacuum field equations with any number of constants. We will use this class of exact solutions to describe the exterior vacuum region of numerically calculated neutron stars. Therefore we study how an Ernst potential given on the rotation axis and containing an arbitrary number of constants can be used to determine the metric everywhere. Then we review two methods to determine those constants from a numerically calculated solution. Finally, we compare the metric and physical properties of our analytic solution with the numerical data and find excellent agreement even for a small number of parameters.
9 pages, 10 figures, 3 tables
References in corpus (2)
Cited by in corpus (8)
- Rotating Stars in Relativity
- What can quasi-periodic oscillations tell us about the structure of the corresponding compact objects?
- An all-purpose metric for the exterior of any kind of rotating neutron star
- Universal Relations and Alternative Gravity Theories
- Unified description of astrophysical properties of neutron stars independent of the equation of state
- Calculation of multipole moments of axistationary electrovacuum spacetimes
- Slowly-rotating compact objects: the nonintegrability of Hartle-Thorne particle geodesics
- An approximate global solution of Einstein's equation for a rotating compact source with linear equation of state