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

Abstract 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–ω model, which is proposed by Li. We determine that the distance of the overshooting region is about 0.072 in the 1.3 M ⊙ star. There are two parts in the overshooting region, one is the completely mixing region of about , and the other is the partial mixing region of about 0.045 . 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–ω model. Then, we calibrate the for classical overshooting by using the k–ω model. As a result, we find that a suitable value of is about 0.008 for the mass range of 1.0–1.8 M ⊙ stars.