  The most energetic GRB-supernovae probably derive from rotating stellar mass
black holes. Based on BeppoSax data, we identify a mechanism for exploding a
remnant stellar envelope by disk winds. A specific signature is high frequency
modulations in the accompanying prompt GRB emission from dissipation in high
energy emissions along the black hole spin axis due, in part, to forced
turbulence in the inner disk or torus mediated by frame dragging. A majority of
long GRBs are found to have significant autocorrelation below 10 Hz with chirps
extending up to 1000 Hz. Their comoving Fourier spectra satisfy a power law
with index $\alpha\simeq-0.82$ up to about one hundred Hz and comoving chirp
spectra show broken power laws with $\alpha\simeq-0.65$ up to 10 Hz,
$\alpha\simeq-0.25$ up to a few hundred Hz and $\alpha\simeq0$ beyond. These
high frequency signatures are the most direct signature of long-lived
turbulence down to the ISCO of rotating black holes, pointing directly
accompanying long duration bursts in gravitational wave emission.
