Monte-Carlo simulations of evolving rotational distributions of low-mass
  stars in young open clusters. Testing the influence of initial conditions
  The rotational evolution of a young stellar population can give informations
about the rotation pattern of more evolved clusters. Combined with rotational
period values of thousands of young stars and theoretical propositions about
the redistribution and loss of stellar angular momentum, it allows us to trace
the rotational history of stars according to their mass. We want to investigate
how internal and environmental changes on single stars can change the
rotational evolution of a young stellar population. We run Monte Carlo
simulations of a young cluster composed by solar mass stars of 0.5, 0.8 and 1.0
M$_\odot$ from 1 to 550 Myr taking into account observational and theoretical
parameters. In order to compare our results with the observations we run
Kolmogorov-Smirnov tests. Our standard model is able to reproduce some clusters
younger than h Per and marginally M37, which is 550 Myr old. Varying the disk
fraction 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 also
reproduced. Changing the initial mass distribution to be similar to the
empirical ONC mass function also gives good results. Modeling the evolution of
a young synthetic cluster from pre-main sequence to early main sequence
considering physical mechanisms of extraction and exchange of angular momentum
can not be achieved successfully for all clusters for which we have enough
rotational data. Clusters of about the same age present different rotational
behaviors due perhaps to differences in their initial conditions.
