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Title:
Comparing models of rapidly rotating relativistic stars constructed by two numerical methods
Authors:
Stergioulas, Nikolaos; Friedman, John L.
Affiliation:
AA(University of Wisconsin, Milwaukee, Wisconsin, US), AB(University of Wisconsin, Milwaukee, Wisconsin, US)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 444, no. 1, p. 306-311 (ApJ Homepage)
Publication Date:
05/1995
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Computational Astrophysics, Computerized Simulation, Numerical Analysis, Relativistic Velocity, Stellar Models, Stellar Rotation, Computer Programs, Efficiency, Equations Of State, Neutron Stars, Stability
DOI:
10.1086/175605
Bibliographic Code:
1995ApJ...444..306S

Abstract

We present the first direct comparison of codes based on two different numerical methods for constructing rapidly rotating relativistic stars. A code based on the Komatsu-Eriguchi-Hachisu (KEH) method (Komatsu et al. 1989), written by Stergioulas, is compared to the Butterworth-Ipser code (BI), as modified by Friedman, Ipser, & Parker. We compare models obtained by each method and evaluate the accuracy and efficiency of the two codes. The agreement is surprisingly good, and error bars in the published numbers for maximum frequencies based on BI are dominated not by the code inaccuracy but by the number of models used to approximate a continuous sequence of stars. The BI code is faster per iteration, and it converges more rapidly at low density, while KEH converges more rapidly at high density; KEH also converges in regions where BI does not, allowing one to compute some models unstable against collapse that are inaccessible to the BI code. A relatively large discrepancy recently reported (Eriguchi et al. 1994) for models based on Friedman-Pandharipande equation of state is found to arise from the use of two different versions of the equation of state. For two representative equations of state, the two-dimensional space of equilibrium configurations is displayed as a surface in a three-dimensional space of angular momentum, mass, and central density. We find, for a given equation of state, that equilibrium models with maximum values of mass, baryon mass, and angular momentum are (generically) either all unstable to collapse or are all stable. In the first case, the stable model with maximum angular velocity is also the model with maximum mass, baryon mass, and angular momentum. In the second case, the stable models with maximum values of these quantities are all distinct. Our implementation of the KEH method will be available as a public domain program for interested users.

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