All Figures

Figure 1: Rotation profiles as a function of the lagrangian mass in solar units for models with (continuous lines) and without magnetic field (dashed lines). The dotted line indicates the initial solid body rotation on the ZAMS. The other lines correspond to an age of respectively 1, 2, 3, 4 and 4.57 Gyr. increases at the centre during the evolution on the main-sequence. No magnetic braking at the surface is included.

Open with DEXTER


In the text

	Figure 2: Same as Fig. 1 but with an initial velocity of 20 km s-1. The dotted line indicates the initial solid body rotation on the ZAMS. The other lines correspond to an age of respectively 0.1, 0.5, 1, 2, 3 and 4.57 Gyr. The surface angular velocity decreases when the star evolves due to the magnetic braking at the surface.
Open with DEXTER


In the text

	Figure 3: Rotation profile for a model with rotation only (dashed line) and with both rotation and magnetic field (dotted line) at the age of the Sun. The initial velocity is 50 km s-1. The points with their respective error bars correspond to the angular velocities in the solar radiative zone deduced from GOLF+MDI and LOWL data (Couvidat et al. 2003).
Open with DEXTER


In the text

	Figure 4: Diffusion coefficients in the model with both rotation and magnetic fields and  km s-1 at the age of the Sun.
Open with DEXTER


In the text