Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aipc..586..808s&link_type=abstract
RELATIVISTIC ASTROPHYSICS: 20th Texas Symposium. AIP Conference Proceedings, Volume 586, pp. 808-810 (2001).
Astronomy and Astrophysics
Astrophysics
Neutron Stars, Spectroscopic Binaries, Close Binaries, Hydrodynamics, Mathematical Procedures And Computer Techniques, Post-Newtonian Approximation, Perturbation Theory, Related Approximations
Scientific paper
In recent years there have been numerous attempts to model the relativistic coalescence of two neutron stars in a binary system. Because of the difficulties associated with solving the Einstein equations numerically, many attempts have been made to model the coalescence via post-Newtonian (PN) numerical hydrodynamic models. Perhaps the two most popular methods have centered around the use of the slow-motion quadrupole approximation or the 2.5PN approximation of Blanchet. Damour, and Schäfer (1990). A typical result of the simulations is the gravitational luminosity as a function of time during the coalescence. However, the complexities of the numerical simulation often make it difficult to understand the PN effects. To this end we are developing a semi-analytic model of the PN driven coalescence that can help us better understand the behavior of the radiation-reaction forces. This model is based on the use of γ=2 Newtonian polytropes to approximate the structure of more realistic neutron stars. .
Calder Alan C.
Swesty Frank Douglas
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