  Neutron star mergers can form a hypermassive neutron star (HMNS) remnant,
which may be the engine of a short gamma ray burst (SGRB) before it collapses
to a black hole, possibly several hundred milliseconds after the merger. During
the lifetime of a HMNS, numerical relativity simulations indicate that it will
undergo strong oscillations and emit GWs with frequencies of a few kilohertz,
which are unfortunately too high for detection to be probable with Advanced
LIGO. Here we discuss the current and future prospects for detecting these
oscillations as modulation of the SGRB. The understanding of the physical
mechanism responsible for the HMNS oscillations will provide information on the
equation of state of the hot HMNS, and the observation of these frequencies in
the SGRB data would give us insight into the emission mechanism of the SGRB.
