The following four runs were computed using a Lagrangian Smoothed Particle 
Hydrodynamics (SPH) code, developed by Frederic Rasio and Joshua Faber.

In all calculations shown here, we used 50,000 equal-mass particles per 
neutron star.  Both stars had the same mass in these calculations.  
Wave forms are computed for an observer looking down the rotation
axis of the binary.  The equation of state for the NS is taken to be a 
polytrope with adiabatic index Gamma.  

We assume for these results that M_NS=1.4 M_sun=2.8E33 gm and R_NS=13km.
Technically, the results also apply for all systems such that
(G*M_NS)/(R_NS*c^2)=0.16, so long as the following scalings are used

t_new=t_old*(r/13km)^1.5*(m/1.4M_sun)^-0.5
h_new=h_old*(r/13km)^-1*(m/1.4M_sun)^2

Our Post-Newtonian results use the PN formalism of Blanchet, Damour, and 
Schafer (1990, see below), which includes both lowest-order 1PN effects,
as well as 2.5PN radiation reaction.  Our Newtonian results use the 2.5 PN 
Radiation Reaction effects as well, but include no 1PN corrections.  These 
calculations have appeared in the following set of papers:

J.A. Faber and F.A. Rasio, Phys. Rev. D, 62, 064012 (2000)
J.A. Faber, F.A. Rasio, and J.B. Manor, Phys. Rev. D,  63, 044012 (2001)
J.A. Faber and F.A. Rasio, submitted to PRD, gr-qc/0201040 (2002)

The formalism used is derived from:

L. Blanchet, T. Damour, and G. Schafer, MNRAS, 242, 289 (1990).

The four runs shown here have the following paramters:

File         Grav.      Mass Ratio      Gamma   r_0/R_NS        Initial spin

gw3n3.dat       N       1.0             3.0     3.1             Synchronized
gw3n2.dat       N       1.0             2.0     2.9             Synchronized
gw3p3.dat       PN      1.0             3.0     4.0             Irrotational
gw3p2.dat       PN      1.0             2.0     4.0             Irrotational

The format of the (ascii) files is as follows:  3 columns:
time (sec)      rh+ (cm)        rhx (cm)