 models predict a greater degree of convergence in the rotation periods at the age of M00 than is observed. The models also under-predict the periods of the slowest rotators in M00. When using $(V-I_{C})_{0}$, the models for stars with $0.0 < (V-I_{C})_{0} < 0.0$ ($0.00 M_{\odot} < M < 0.00 M_{\odot}$) fit the M00 observations, but fail to fit the younger clusters. T