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

被引：9
|
作者：
Guo, Fei [1 ,2 ,3 ]
Li, Yan [1 ,2 ,3 ,4 ]
机构：
[1] Chinese Acad Sci, Yunnan Observ, POB 110, Kunming 650011, Yunnan, Peoples R China
[2] Univ Chinese Acad Sci, Beijing 100049, Peoples R China
[3] Chinese Acad Sci, Ctr Astron Megasci, 20A Datun Rd, Beijing 100012, Peoples R China
[4] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, POB 110, Kunming 650011, Yunnan, Peoples R China
来源：
ASTROPHYSICAL JOURNAL | 2019年 / 879卷 / 02期
关键词：
convection; stars: evolution; stars: low-mass; STELLAR EVOLUTION;
D O I：
10.3847/1538-4357/ab262f
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
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.
引用
收藏
页数：6
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