Thermohaline mixing in low-mass giants
Thermohaline mixing has recently been proposed to occur in low mass red giants,with large consequences for the chemical yields of low mass stars. We investigate the role of thermohaline mixing during the evolution of stars between 1 M and 3M ,in comparison to other mixing processes acting in these stars. We confirm that thermohaline mixing has the potential to destroy most of the 3He which is produced earlier on the main sequence during the red giant stage. In our models we find that this process is working only in stars with initial mass M < 1.5 M. Moreover,we report that thermohaline mixing can be present during core helium burning and beyond in stars which still have a 3He reservoir. While rotational and magnetic mixing is negligible compared to the thermohaline mixing in the relevant layers,the interaction of thermohaline motions with differential rotation and magnetic fields may be essential to establish the time scale of thermohaline mixing in red giants.
stars:evolution stars:abundances stars:AGB and post-AGB stars:magnetic fields stars:rotation ISM:abundances
M.Cantiello N.Langer
Astronomical Institute Utrecht,Princetonplein 5,3584 CC Utrecht,The Netherlands
国际会议
The 252th Symposium of the International Astronomical Union(国际天文学联合会第252届研讨会)
海南三亚
英文
103-110
2008-04-06（万方平台首次上网日期，不代表论文的发表时间）