The wavetrains contained the the files "qewaves1.dat", "qewaves2.dat", and
"qewaves3.dat" were generated by applying the QE (quasi-equilibrium)
method to equal-mass neutron star binaries.  In all plots, time (t) is
measured in seconds, r*h (h being h_plus or h_cross) is measured in
centimeters, and the scale is set by setting the rest mass of each star to
1.5 solar masses.  One can obtain the waveforms for a binary composed of
stars of rest mass M by simply multiplying both t and r*h by (M /
1.5*M_solar).  All models were constructed from an n=1 polytropic eqn of
state in full general relativity. (For polytropes, the results scale
with mass; a given model is specified by the compaction of its isolated, 
spherical counterpart, M/R ). We always give wave amplitudes on the z-axis. 
To very good accuracy, h_plus and h_cross differ only by a phase 
in "qewaves1.dat" and "qewaves2.dat", so we provide only one waveform 
for each file.  That is,
these files have two columns, where the second could be h_plus or
h_cross:   time (sec)     rh (cm)

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"qewaves1.dat" shows the last 214 wave cycles of the adiabatic inspiral of
a corotating binary, a calculation discussed in detail in 

Duez, Baumgarte and Shapiro Phys. Rev. D.  63, 084030.  

The compaction of each star in isolation is M/R = 0.088.  We
do not compute the waveform from the plunge and merger of the stars.
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"qewaves2.dat" uses the same stars, but with irrotational velocity fields.
It shows last 339 wave cycles of the adiabatic inspiral phase.  This
result is discussed in more detail, as well as compared to the previous
result, in 

Duez, Uryu, Baumgarte, Shapiro and Shibata, Phys. Rev. D. 65 024016.

Figure 5 of this paper shows the waveform in this file "qewaves2.dat"
in the bottom frame, and the waveform in the file "qewaves1.dat" in
the top frame.
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"qewaves3.dat" shows the h_cross waveform for the late inspiral and
coalescence of two neutron stars each having a compaction M/R = 0.14 in
isolation.  The merger of the two stars leads to immediate black hole
formation.  The plunge and merger piece of the calculation is discussed in
Shibata and Uryu, Phys. Rev. D. 61, 064001.  The complete NS binary wavetrain, 
through late inspiral, plunge and initial coalescence, is constructed 
for the first time in numerical relativity in 
Duez et al. Phys.  Rev. D. 65 024016
cited above.  The waveform in this file is shown in Fig. 6 of that
paper.
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