The results of Fryer, Woosley, and Heger suggest that the collapse remnant (prior to black hole
formation) is susceptible to the development of a secular bar-mode instability. However, at , the GW
emission would be redshifted out of LIGO-II’s frequency range. At
,
, with a
corresponding frequency of
[86
, 88
]. Even if such a signal persists for a hundred cycles, it
probably would be undetectable by LIGO-II. Note that these signal strengths are orders of
magnitude lower than the qualitative estimates of signal strength given in Carr, Bond, and
Arnett [47].
LIGO-II may be able to detect the GW emission from binary clumps formed via a fragmentation
instability. If such a signal is emitted at and persists for 10 cycles,
would be
, over a
frequency range of
[86
, 88]. The likelihood of the development of a fragmentation instability
is diminished by the fact that the off-center density maxima present in the simulations of Fryer, Woosley,
and Heger are not very pronounced.
The “ring-down” of the black hole remnant will likely be strong because Fryer, Woosley, and Heger
observe a high accretion rate after collapse. FHH estimate that for a source located at , the GWs
would be redshifted out of LIGO-II’s bandwidth. However, for a source at
,
and
the frequency range is
. This signal may be marginally detectable with LIGO-II (see
Figure 2
).
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