In this paper, we compare the waveforms from the post-Newtonian (PN) approach
with the numerical simulations of generic black-hole binaries which have mass
ratio qβΌ0.8, arbitrarily oriented spins with magnitudes S1β/m12ββΌ0.6
and S2β/m22ββΌ0.4, and orbit 9 times from an initial orbital separation of
rβ11M prior to merger. We observe a reasonably good agreement between
the PN and numerical waveforms, with an overlap of over 98% for the first six
cycles of the (β=2,m=Β±2) mode and over 90% for the (β=2,m=1) and
(β=3,m=3) modes.Comment: 4 pages, 2 figures, prepared for the proceedings of the 18th workshop
on general relativity and gravitation, Hiroshima, Japan, Nov.17 - Nov.21,
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