Volume 554, June 2013
|Number of page(s)||14|
|Section||Stellar structure and evolution|
|Published online||03 June 2013|
Impact of internal gravity waves on the rotation profile inside pre-main sequence low-mass stars
1 Geneva Observatory, University of Geneva, Chemin des Maillettes 51, 1290 Versoix, Switzerland
2 IRAP, CNRS UMR 5277, Université de Toulouse, 14 Av. E. Belin, 31400 Toulouse, France
3 LUPM, Université Montpellier II, CNRS, UMR 5299, Place E. Bataillon, 34095 Montpellier, France
4 Calcul Québec, Université de Montréal (DGTIC), C.P. 6128, succ. Centre-ville, Montréal (Québec) H3C 3J7, Canada
Received: 11 February 2013
Accepted: 4 April 2013
Aims. We study the impact of internal gravity waves (IGW), meridional circulation, shear turbulence, and stellar contraction on the internal rotation profile and surface velocity evolution of solar metallicity low-mass pre-main sequence stars.
Methods. We compute a grid of rotating stellar evolution models with masses between 0.6 and 2.0 M⊙ taking these processes into account for the transport of angular momentum, as soon as the radiative core appears and assuming no more disk-locking from that moment on. IGW generation along the PMS is computed taking Reynolds-stress and buoyancy into account in the bulk of the stellar convective envelope and convective core (when present). Redistribution of angular momentum within the radiative layers accounts for damping of prograde and retrograde IGW by thermal diffusivity and viscosity in corotation resonance.
Results. Over the whole mass range considered, IGW are found to be efficiently generated by the convective envelope and to slow down the stellar core early on the PMS. In stars more massive than ~1.6 M⊙, IGW produced by the convective core also contribute to angular momentum redistribution close to the ZAMS.
Conclusions. Overall, IGW are found to significantly change the internal rotation profile of PMS low-mass stars.
Key words: stars: evolution / stars: interiors / stars: low-mass / stars: rotation
© ESO, 2013
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