  Neutron stars are among the densest known objects in the universe and an
ideal laboratory for the strange physics of super-condensed matter. While the
simultaneously measurements of mass and radius of non-rotating neutron stars
may impose constraints on the properties of the dense nuclear matter, the
observation and study of maximally-rotating ones, close to the mass-shedding
limit, may lead to significantly further constraints. Theoretical predictions
allow neutron stars to rotate extremely fast (even more than $2000 \ {\rm
Hz}$). However, until this moment, the fastest observed rotating pulsar has a
frequency of $716 \ {\rm Hz}$, much lower compared to the theoretical
predictions. There are many suggestions for the mechanism which lead to this
situation. In any case, the theoretical study of uniformly rotating neutron
stars, along with the accurate measurements, may offer rich information
concerning the high density part of the equation of state. In addition, neutron
stars through their evolution, may provide us with a criteria to determine the
final fate of a rotating compact star. Sensitivity of bulk neutron stars
properties on the equation of state at the mass-shedding limit are the main
subject of the present study.
