Physics
Scientific paper
Mar 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999phdt........15w&link_type=abstract
Thesis (PhD). STATE UNIVERSITY OF NEW YORK AT STONY BROOK, Source DAI-B 61/01, p. 315, Jul 2000, 300 pages.
Physics
Scientific paper
This thesis attempts to address the physics of binary neutron star systems in the Newtonian limit and beyond. I have been involved with the building of three separate numerical codes to model Newtonian and Newtonian + 2.5Post-Newtonian radiation reaction mergers of binary neutron star systems as well fully-relativistic studies of isolated neutron stars. In chapter 2, we confirm the dynamical instability of Lai, Rasio and Shapiro and indicate that the results due to New and Tohline are not as inconsistent as has been indicated. We also describe our new results related to our radiation reaction simulations. Specifically, we indicate that the majority of gravitational radiation emitted pre-merger arises from the low density regions of the stars and the tidal arms. In addition, the time to merger for aCM <~ 5.0R* binary configurations is between one-half and one Keplerian orbital period. Significant efforts have been made to produce a conservative numerical formalism for these studies which can maintain several stable orbits in the Newtonian regime and that work may be found in chapter 2. Chapter 3 illustrates our studies in the full- relativistic regime with the usage of the Boná- Masso and modified Shibata-Nakamura formulations of Einstein's equations. While the Boná-Masso formulation would appear unstable the purely spacetime evolutions with the modified Shibata-Nakamura formulation have produced TOV simulations upwards of 9 ms. While our coupled spacetime + hydro simulations do not exceed 0.9 ms, there is indication that long-term evolutions may be possible with the development of more advanced gauge and boundary choices than those used for our studies.
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