**AAS Meeting #193 - Austin, Texas, January 1999**

*Session 42. Gamma-Rays/Gravitation*

Display, Thursday, January 7, 1999, 9:20am-6:30pm, Exhibit Hall 1
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## [42.12] Numerical Evolutions of Relativistic Neutron Stars

*Edward Y.M. Wang (State Univ. of New York at Stony Brook), Alan C. Calder (National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign), F. Douglas Swesty (Department of Astronomy and National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign)*

The coalescence of compact binary systems is expected to be
the main source for the observed gravitational radiation to
be detected by gravitational wave observatories. A number of
these observatories, including LIGO, are expected to become
operational early in the next century. There are
expectations that a few merging binary neutron star systems
are to be observed by LIGO and her counterparts every year.
The focus of our work is to model the coalescence of these
systems so as to study the gravitational radiation emitted,
and in particular, to predict the the waveforms expected to
be observed from such astrophysical events. Past work has
involved the evolution of binary neutron star systems in the
Newtonian limit and the Newtonian plus (2.5 Post-Newtonian
order) radiation reaction limit. Here we present preliminary
results which are relevant to our goal of numerically
modeling fully-relativistic compact binary mergers in 3D. We
present a new numerical formalism for evolving such systems,
a 3D relativistic spacetime and hydrodynamics code called
ZEPHYR, with a description of the algorithms implemented,
and a variety of testbed problems attempted. Our numerical
formalism utilizes the recent Bona-Masso formulation of
Einstein's equations as a hyperbolic system of coupled
first-order differential equations. Future studies and
descriptions of other astrophysical systems which can be
modeled similarly will be discussed in addition.

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