  We present and evaluate several strategies to search for prompt,
low-frequency radio emission associated with gravitational wave transients
using the Murchison Widefield Array (MWA). As we are able to repoint the MWA on
timescales of tens of seconds, we can search for the dispersed radio signal
that has been predicted to originate along with or shortly after a neutron
star-neutron star merger. We find that given the large, 600 deg^2 instantaneous
field-of-view of the MWA we can cover a significant fraction of the predicted
gravitational wave error region, although due to the complicated geometry of
the latter we only cover >50% of the error region for approximately 5% of
events, and roughly 15% of events will be located <10 deg from the MWA pointing
center such that they will be covered in the radio images. For optimal
conditions our limiting flux density for a 10-s long transient would be 0.1 Jy,
increasing to about 1 Jy for a wider range of events. This corresponds to
luminosity limits of 1e38-1e39 erg/s based on expectations for the distances of
the gravitational wave transients, which should be sufficient to detect or
significantly constrain a range of models for prompt emission.
