Observations demonstrate that the surface abundance of ##IMG## [http://ej.iop.org/images/2041-8205/901/1/L18/apjlabb45fieqn1.gif] {${}^{7}\mathrm{Li}$} in low-mass stars changes dramatically between the tip of the red giant branch and the red clump. This naturally suggests an association with the helium core flash, which occurs between these two stages. Using stellar evolution models and a simple, ad hoc mixing prescription, we demonstrate that the ##IMG## [http://ej.iop.org/images/2041-8205/901/1/L18/apjlabb45fieqn2.gif] {${}^{7}\mathrm{Li}$} enhancement can be explained by a brief chemical mixing event that occurs at the time of the first, strongest He subflash. The amount of ##IMG## [http://ej.iop.org/images/2041-8205/901/1/L18/apjlabb45fieqn3.gif] {${}^{7}\mathrm{Be}$} already present above the H-burning shell just before the flash, once it mixes into the cooler envelope and undergoes an electron capture conve...

中文翻译：

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氦闪光引起的混合事件可以解释红色团星的锂丰度

观察表明，## IMG ## [http://ej.iop.org/images/2041-8205/901/1/L18/apjlabb45fieqn1.gif] {$ {} ^ {7} \ mathrm {低质量恒星中的Li} $}在红色巨型分支的尖端和红色丛之间急剧变化。这自然暗示与氦核闪光有关，这发生在这两个阶段之间。使用恒星演化模型和简单的临时混合处方，我们证明了## IMG ## [http://ej.iop.org/images/2041-8205/901/1/L18/apjlabb45fieqn2.gif] { $ {} ^ {7} \ mathrm {Li} $}的增强可以通过短暂的化学混合事件来解释，该事件发生在第一次，最强的He亚闪时。## IMG ##的数量[http://ej.iop.org/images/2041-8205/901/1/L18/apjlabb45fieqn3.gif] {$ {} ^ {7} \ mathrm {Be} $}在闪光灯之前已经存在于H燃烧壳上方，