Modelling the angular momentum evolution of low-mass stars with core-envelope decoupling
Received 5 June 1997 / Accepted 22 January 1998
We present a model of angular momentum evolution for stars in the mass range 0.5 - 1.1 , during their early stages of evolution. The model is based upon the following hypothesis: a constant surface rotational period during star-disk interaction, angular momentum loss through magnetic wind, and differential rotation parameterized with a constant coupling time. We investigate the effect of the different parameters, the initial velocity at the T Tauri age, the disk lifetime, the magnetic braking law, and we discuss the effect of introducing a core-envelope decoupling. The angular momentum transfer is parameterized by the use of a coupling time scale , which controls the exchanges of angular momentum between the - fast-rotating - radiative core and the convective envelope, both supposed to rotate as solid bodies. We present evolutionary tracks of a single star through the pre-main sequence and the main-sequence, for different masses and different coupling time-scales. We conclude that rapid rotators require solid-body rotation, and ZAMS slow rotator require a strong differential decoupling with a characteristic coupling time about 100 Myr.
Key words: stars: rotation stars: late-type stars: pre-main sequence stars: interiors
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© European Southern Observatory (ESO) 1998
Online publication: April 20, 1998