  It is shown that protostrange stars (PSSs) can be convective and that there
are two possible scenarios describing their turbulence. Besides the local
turbulence on the scale which is less than the mean free path of neutrinos,
large-scale (~1 km) convection also may occur with properties that are similar
to those of convection in protoneutron stars (PNSs). We thus suggest that
strange stars can also create dynamo-originated magnetic fields during the
deleptonization episode soon after a supernova explosion. Further detailed
investigations are needed to see whether or not strange stars and neutron stars
can be distinguished according to the differences in dynamo actions in strange
quark matter and in neutron matter. The magnetic fields of strange stars and
neutron stars may also behave very differently during the accretion-phase when
the fields decay.
