Gravitational Waves from Inspiralling Compact Binaries in ... - LUTH

Validity of Results
As one approaches the plunge boundary motion deviates
from slow precessing QK to zoom-whirl. Hence we need to
be be sufficiently away from the plunge boundary for validity
of QKR.
QKR assumes orbits are slowly precessing..Hence one needs
to set upper limit on periastron precession
G m n
c 3
If ξ ≡ j ≡ cJ /(µGm), the constraint on parameters ξ and
et becomes
ξ
(1 − e2 =
t ) 3/2
3 1
j
< 3.0 × 10 −3
This restriction is due to our use of GQKR. One may be able to
go beyond the limit by using instead the exact
Schwarzschild-like motion in the EOB metric.
BRI-IHP06-I – p.156/??