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{H}{{p}} in the 1.3 M ⊙ star. There are two parts in the overshooting region, one is the completely mixing region of about 0.027{H}{{p}}, and the other is the partial mixing region of about 0.045{H}{{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-ω model. Then, we calibrate the {f}ov} for classical overshooting by using the k-ω 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 ⊙ stars.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- July 2019
- DOI:
- 10.3847/1538-4357/ab262f
- Bibcode:
- 2019ApJ...879...86G
- Keywords:
-
- convection;
- stars: evolution;
- stars: low-mass