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The rotational evolution of a young stellar population can give informationsabout the rotation pattern of more evolved clusters. Combined with rotationalperiod values of thousands of young stars and theoretical propositions aboutthe redistribution and loss of stellar angular momentum, it allows us to tracethe rotational history of stars according to their mass. We want to investigatehow internal and environmental changes on single stars can change therotational evolution of a young stellar population. We run Monte Carlosimulations of a young cluster composed by solar mass stars of 0.5, 0.8 and 1.0M$_\odot$ from 1 to 550 Myr taking into account observational and theoreticalparameters. In order to compare our results with the observations we runKolmogorov-Smirnov tests. Our standard model is able to reproduce some clustersyounger than h Per and marginally M37, which is 550 Myr old. Varying the diskfraction or the initial period distribution did not improve the results.However, when we run a model with a finer mass grid the Pleiades can be alsoreproduced. Changing the initial mass distribution to be similar to theempirical ONC mass function also gives good results. Modeling the evolution ofa young synthetic cluster from pre-main sequence to early main sequenceconsidering physical mechanisms of extraction and exchange of angular momentumcan not be achieved successfully for all clusters for which we have enoughrotational data. Clusters of about the same age present different rotationalbehaviors due perhaps to differences in their initial conditions.

Monte-Carlo simulations of evolving rotational distributions of low-mass stars in young open clusters. Testing the influence of initial conditions