The effects of convective overshooting on naked helium stars  

作　　者：Jing-Zhi Yan Chun-Hua Zhu Zhao-Jun Wang Guo-Liang Lü 

机构地区：[1]School of Physical Science and Technology,Xinjiang University

出　　处：《Research in Astronomy and Astrophysics》2016年第9期75-82,共8页天文和天体物理学研究（英文版）

基　　金：supported by the Xinjiang Science Fund for Distinguished Young Scholars under Grant Nos. 2013721014 and 2014721015;the National Natural Science Foundation of China under Grant Nos. 11473024, 11363005 and 11163005

摘　　要：Using stellar evolutionary models, we investigate the effects of convective overshooting on naked helium stars. We find that a larger value of overshooting parameter δov results in a larger convective core, which prolongs the lifetimes of naked helium stars on the helium main sequence and leads to higher effective temperatures and luminosities. For naked helium stars with masses lower than about 0.8 Mo, they hardly become giant stars as a result of a weak burning shell. However, naked helium stars with masses between about 0.8 M⊙ and 1.1 M⊙ can evolve into giant branch phases, and finally become carbon oxygen white dwarfs.Using stellar evolutionary models, we investigate the effects of convective overshooting on naked helium stars. We find that a larger value of overshooting parameter δov results in a larger convective core, which prolongs the lifetimes of naked helium stars on the helium main sequence and leads to higher effective temperatures and luminosities. For naked helium stars with masses lower than about 0.8 Mo, they hardly become giant stars as a result of a weak burning shell. However, naked helium stars with masses between about 0.8 M⊙ and 1.1 M⊙ can evolve into giant branch phases, and finally become carbon oxygen white dwarfs.

关 键 词：STARS evolution- stars interiors- stars fundamental parameters 

分 类 号：P152[天文地球—天文学]