  For detection of neutrinos from galactic supernovae, the planned
Hyper-Kamiokande detector will be the first detector that delivers both a high
event rate (about one third of the IceCube rate) and event-by-event energy
information. In this thesis, we use a three-dimensional computer simulation by
the Garching group to find out whether this additional information can be used
to improve the detection prospects of fast time variations in the neutrino
flux.
  We find that the amplitude of SASI oscillations of the neutrino number flux
is energy-dependent. However, in this simulation, the larger amplitude in some
energy bins is not sufficient to counteract the increased noise caused by the
lower event rate. Finally, we derive a condition describing when it is
advantageous to consider an energy bin instead of the total signal and show
that this condition is satisfied if the oscillation of the mean neutrino energy
is increased slightly.
