Non-gray rotating stellar models and the evolutionary history of the Orion Nebular Cluster
| Autor: | L. T. S. Mendes, Francesca D'Antona, N. R. Landin, L. P. R. Vaz, Paolo Ventura |
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| Rok vydání: | 2006 |
| Předmět: |
Physics
education.field_of_study Angular momentum Mass distribution Population Astrophysics (astro-ph) FOS: Physical sciences Astronomy and Astrophysics Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Rotation Stars Space and Planetary Science Astrophysics::Solar and Stellar Astrophysics education Low Mass Stellar evolution Astrophysics::Galaxy Astrophysics Dynamo |
| DOI: | 10.48550/arxiv.astro-ph/0609292 |
| Popis: | Rotational evolution in the pre-main sequence (PMS) is described with new sets of PMS evolutionary tracks including rotation, non-gray boundary conditions (BCs) and either low (LCE) or high convection efficiency (HCE). 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 models; 2) the initial angular momentum of low mass stars, by means of their templates in the ONC. We discuss the reliability of current stellar models for the PMS. While the 2D radiation hydrodynamic simulations predict HCE in PMS, semi-empirical calibrations either seem to require that convection is less efficient in PMS than in the following MS phase or are still contradictory. We derive stellar masses and ages for the ONC by using both LCE and HCE. The resulting mass distribution for the bulk of the ONC population is in the range 0.2$-$0.3 {\msun} for our non-gray models and in the range 0.1$-$0.3{\msun} for models having gray BCs. In agreement with Herbst et al. (2002) we find that a large percentage ($\sim$70%) of low-mass stars (M\simlt 0.5{\msun} for LCE; M\simlt0.35{\msun} for HCE) in the ONC appears to be fast rotators (P$ Comment: 17 pages, 11 figures |
| Databáze: | OpenAIRE |
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