  We compute the binding energy and angular momentum of a test-particle at the
last stable circular orbit (LSO) on the equatorial plane around a general
relativistic, rotating neutron star (NS). We present simple, analytic, but
accurate formulas for these quantities that fit the numerical results and which
can be used in several astrophysical applications. We demonstrate the accuracy
of these formulas for three different equations of state (EOS) based on nuclear
relativistic mean-field theory models and argue that they should remain still
valid for any NS EOS that satisfy current astrophysical constraints. We compare
and contrast our numerical results with the corresponding ones for the Kerr
metric characterized by the same mass and angular momentum.
