Modelling the angular momentum evolution of low-mass stars with core-envelope decoupling

Details Modelling the angular momentum evolution of low-mass stars with core-envelope decoupling Modelling the angular momentum evolution of low-mass stars with core-envelope decoupling

May 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...333..629a&link_type=abstract

Astronomy and Astrophysics, v.333, p.629-643 (1998)

Astronomy and Astrophysics

Astrophysics

41

Scientific paper

We present a model of angular momentum evolution for stars in the mass range 0.5 - 1.1 M_(\odot), 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 tau_(c), 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.

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