Convective Overshooting in Low-mass Stars Using the k-ω Model

The mixing of convective overshoot is quite uncertain in low-mass stars. To study the mixing in the convective core and beyond the convective boundary for low-mass stars, we use the k-omega model, which is proposed by Li. We determine that the distance of the overshooting region is about 0.072H(p) in the 1.3 M-circle dot star. There are two parts in the overshooting region, one is the completely mixing region of about 0.027H(p), and the other is the partial mixing region of about 0.045H(p). Next, we study the semiconvection for low-mass stars. We find that the semiconvection near the convective core boundary can be removed when we use the k-omega model. Then, we calibrate the f(ov) for classical overshooting by using the k-omega model. As a result, we find that a suitable value of f(ov) is about 0.008 for the mass range of 1.0-1.8 M-circle dot stars.