  We perform fully general-relativistic simulations of binary strange star
mergers considering two different approaches for thermal effects. The first
uses a cold equation of state (EOS) derived from a modified version of the MIT
bag model which is then supplemented by a $\Gamma$-law correction. The second
approach employs a microphysical description of the finite-temperature effects.
We describe results obtained with the two treatments, highlighting the
influence of thermal effects. We find that the postmerger dynamics differs
significantly in the two cases, leading to quantitative differences in the
postmerger gravitational-wave spectrum and ejecta mass. The peak frequency of
the postmerger gravitational-wave emission is consistent with the established
quasi-universal relations for binary neutron star mergers and as a result, our
simulations cannot distinguish between mergers of neutron stars and those of
strange stars. Our models with realistic treatment of finite-temperature
effects produce a significant amount of ejecta $\gtrsim 0.02\ M_{\odot}$. The
resulting flux of strangelets near the Earth, computed assuming that all
neutron star mergers are in fact strange-stars mergers and that the binary
considered here is representative, is in tension with experimental upper
limits. As such, our results tentatively disfavor a scenario in which
strange-quark matter is the lowest energy state of matter.
