  We compute the temperature profiles of accretion discs around rapidly
rotating strange stars, using constant gravitational mass equilibrium sequences
of these objects, considering the full effect of general relativity. Beyond a
certain critical value of stellar angular momentum ($J$), we observe the radius
($r_{\rm orb}$) of the innermost stable circular orbit (ISCO) to increase with
J (a property seen neither in rotating black holes nor in rotating neutron
stars). The reason for this is traced to the crucial dependence of $dr_{\rm
orb}/dJ$ on the rate of change of the radial gradient of the Keplerian angular
velocity at $r_{\rm orb}$ with respect to $J$. The structure parameters and
temperature profiles obtained are compared with those of neutron stars, as an
attempt to provide signatures for distinguishing between the two. We show that
when the full gamut of strange star equation of state models, with varying
degrees of stiffness are considered, there exists a substantial overlap in
properties of both neutron stars and strange stars. However, applying accretion
disc model constraints to rule out stiff strange star equation of state models,
we notice that neutron stars and strange stars exclusively occupy certain
parameter spaces. This result implies the possibility of distinguishing these
objects from each other by sensitive observations through future X-ray
detectors.
