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Causality alone suffices to set a lower bound on the period of rotation ofrelativistic stars as a function of their maximum observed mass. That is, byassuming a one-parameter equation of state (EOS) that satisfies v_sound < c andthat allows stars with masses as large as the largest observed neutron-starmass, M_sph^max, we find P[ms] > 0.282 + 0.196 ( M_sph^max/M_odot-1.442). Thelimit does not assume that the EOS agrees with a known low-density form forordinary matter, but if one adds that assumption, the minimum period is raisedby a few percent. Thus the current minimum period of uniformly rotating stars,set by causality, is 0.28ms (0.29ms for stars with normal crust). Theminimizing EOS yields models with a maximally soft exterior supported by amaximally stiff core. An analogous upper limit set by causality on the maximummass of rotating neutron stars requires a low-density match and the limitdepends on the matching density, epsilon_m. We recompute it, obtaining aslightly revised value, M_rot^max \sim 6.1( 2 * 10^14 g/cm^3 epsilon_m )^1/2M_odot.Comment: 28 pages, LaTeX2e, 8 Postscript figures, submitted to Ap

Upper Limits Set by Causality on the Rotation and Mass of Uniformly Rotating Relativistic Stars