Issue |
Astron. Astrophys. Suppl. Ser.
Volume 132, Number 3, November I 1998
|
|
---|---|---|
Page(s) | 431 - 454 | |
DOI | https://doi.org/10.1051/aas:1998304 | |
Published online | 15 November 1998 |
Construction of highly accurate models of rotating neutron stars – comparison of three different numerical schemes
1
Department of Earth Science and Astronomy, Graduate School of Arts and Sciences, University of Tokyo, Komaba, Meguro, Tokyo 153, Japan
2
Department of Physics, University of Wisconsin-Milwaukee, PO box 413, Milwaukee, WI 53201, U.S.A.
3
Département d'Astrophysique Relativiste et de Cosmologie, UPR 176 du CNRS, Observatoire de Paris, F-92195 Meudon Cedex, France
Send offprint request to: E. Gourgoulhon
Received:
15
April
1998
Accepted:
6
May
1998
We conduct a direct comparison of three different representative
numerical codes for constructing models of rapidly rotating neutron
stars in general relativity. Our aim is to evaluate the accuracy of
the codes and to investigate how the accuracy is affected by the
choice of interpolation, domain of integration and equation of
state. In all three codes, the same physical parameters,
equations of state and interpolation method are used. We
construct 25 selected models for polytropic equations of state and 22
models with realistic neutron star matter equations of state.
The three codes agree well with each other (typical agreement
is better than 0.1% to 0.01%) for most models, except for the extreme
assumption of uniform density stars. We conclude that the codes can
be used for the construction of highly accurate initial data configurations
for polytropes of index (which typically correspond to realistic
neutron stars), when the domain of integration includes
all space and for realistic equations with no phase transitions.
With the exception of the uniform density case, the obtained values of physical parameters
for the models considered in this paper can be regarded as "standard” and we display them
in detail for all models.
Key words: stars: neutron / stars: rotation / pulsars: general / relativity / methods: numerical
© European Southern Observatory (ESO), 1998