论文标题
LaMost调查中的Li-Fir巨人。 iii。 Li富巨人的统计分析
Li-rich Giants in LAMOST Survey. III. The statistical analysis of Li-rich giants
论文作者
论文摘要
Li-Righ巨人的难题仍未解决，与标准恒星模型的预测相矛盾。尽管确切的进化阶段在李富巨人的知识中起着关键作用，但具有有限数量的李素巨人的巨人，以高质量的星号参数来清楚地区分出色的进化阶段。基于Lamost数据版本7（DR7），我们应用了数据驱动的神经网络方法来得出巨型恒星的参数，该参数包含最大数量的Li富巨人。红色巨星分为红色巨型分支（RGB），主要红色团块（PRC）和次要红色团块（SRC）的三个阶段，这些阶段依赖于估计的小型震中参数。在对液体巨大巨人的属性（即恒星质量，碳，氮，富含液体的分布和频率）的统计分析中，我们发现：（1）大多数Li-rich RGB星星被建议是Li-Rich Prech Pre-RGB星星的后代和/或吞噬了Planet companies companser或septellar或seltellar companires companies and the的后代； （2）富含Li的SRC恒星可能是高质量Li富含RGB恒星的Li耗尽的自然结果。 （3）氦气闪光灯附近的内部混合过程可以解释统治着富含李的巨人的李富集的现象。基于Li-rich和正常PRC恒星之间的[C/N]分布的比较，富含Li的过程可能取决于恒星质量。
The puzzle of Li-rich giant is still unsolved, contradicting the prediction of the standard stellar models. Although the exact evolutionary stages play a key role in the knowledge of Li-rich giants, a limited number of Li-rich giants have been taken with high-quality asteroseismic parameters to clearly distinguish the stellar evolutionary stages. Based on the LAMOST Data Release 7 (DR7), we applied a data-driven neural network method to derive the parameters for giant stars, which contain the largest number of Li-rich giants. The red giant stars are classified into three stages of Red Giant Branch (RGB), Primary Red Clump (PRC), and Secondary Red Clump (SRC) relying on the estimated asteroseismic parameters. In the statistical analysis of the properties (i.e. stellar mass, carbon, nitrogen, Li-rich distribution, and frequency) of Li-rich giants, we found that: (1) Most of the Li-rich RGB stars are suggested to be the descendants of Li-rich pre-RGB stars and/or the result of engulfment of planet or substellar companions; (2) The massive Li-rich SRC stars could be the natural consequence of Li depletion from the high-mass Li-rich RGB stars. (3) Internal mixing processes near the helium flash can account for the phenomenon of Li-rich on PRC that dominated the Li-rich giants. Based on the comparison of [C/N] distributions between Li-rich and normal PRC stars, the Li-enriched processes probably depend on the stellar mass.
