  A torus develops a state of suspended accretion against a magnetic wall
around a rapidly rotating black hole formed in core-collapse hypernovae. It
hereby emits about 10% of the black hole spin-energy in gravitational radiation
from a finite number of multipole mass moments. We quantify the relation
between the frequency of quadrupole gravitational radiation and the energy
output $E_w$ in torus winds by $f_{gw}\simeq 470{Hz}(E_w/4\times
10^{52}{erg})^{1/2}(7M_\odot/M)^{3/2}$, where $M$ denotes the mass of the black
hole. We propose that $E_w$ irradiates the remnant stellar envelope from
within. We identify $E_w$ with energies $\sim 10^{52}$ erg inferred from X-ray
observations on matter injecta; and the poloidal curvature in the magnetic wall
with the horizon opening angle in baryon poor outflows that power true GRB
energies of $E_\gamma\simeq 3\times 10^{51}$ erg.
