Volume 456, Number 1, September II 2006
|Page(s)||269 - 282|
|Section||Stellar structure and evolution|
|Published online||23 August 2006|
Non-gray rotating stellar models and the evolutionary history of the Orion Nebular Cluster
Depto. de Física, Universidade Federal de Minas Gerais, CP 702, 30161-970 Belo Horizonte, MG, Brazil e-mail: [nlandin;lpv]@fisica.ufmg.br
2 Osservatorio Astronomico di Roma, via Frascati 33, 00040 MontePorzio Catone, Italy e-mail: [ventura;dantona]@mporzio.astro.it
3 Depto. de Engenharia Eletrônica, Universidade Federal de Minas Gerais, CP 702, 30161-970 Belo Horizonte, MG, Brazil e-mail: email@example.com
Accepted: 12 May 2006
Context.Rotational evolution in the pre-main sequence is described with new sets of pre-MS evolutionary tracks including rotation, non-gray boundary conditions (BCs) and either low (LCE) or high convection efficiency (HCE).
Aims.Using observational data and our theoretical predictions, we aim at constraining (1) the differences obtained for the rotational evolution of stars within the ONC by means of these different sets of new models; (2) the initial angular momentum of low mass stars, by means of their templates in the ONC.
Methods.We discuss the reliability of current stellar models for the pre-MS. While the 2D radiation hydrodynamic simulations predict HCE in pre-MS, semi-empirical calibrations either seem to require that convection is less efficient in pre-MS than in the following MS phase (lithium depletion) or are still contradictory (binary masses). We derive stellar masses and ages for the ONC by using both LCE and HCE.
Results.The resulting mass distribution for the bulk of the ONC population is in the range 0.2-0.4 for our new non-gray models and, as in previous analyse, in the range 0.1-0.3 for models having gray BCs. In agreement with Herbst et al. (2002) we find that a large percentage (~70%) of low-mass stars (M 0.5 for LCE; M 0.35 for HCE) in the ONC appears to be fast rotators ( days). Three possibilities are open: 1) ~70% of the ONC low mass stars lose their disk at early evolutionary phases; 2) their “locking period” is shorter; 3) the period evolution is linked to a different morphology of the magnetic fields of the two groups of stars. We also estimate the range of initial angular momentum consistent with the observed periods.
Conclusions.The comparisons made indicate that a second parameter is needed to describe convection in the pre-MS, possibly related to the structural effect of a dynamo magnetic field.
Key words: stars: evolution / stars: interiors / stars: rotation / stars: Hertzsprung-Russell (HR) and C-M diagrams
© ESO, 2006
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