论文标题
在氦气闪光和锂增强的团块中加热波加热
Wave heating during the helium flash and lithium-enhanced clump stars
论文作者
论文摘要
相对于红色巨型分支（TRGB）的恒星，锂中的红色团星已经增强，这在当前恒星模型中是出乎意料的。在TRGB上，星星经历了氦气闪光灯，在此期间，氦气燃烧短暂产生了$ 10^9 \，l_ \ odot $ of Power $ of of Power un，并在恒星的核心内驱动对流。氦燃烧的外壳激发了大的内部重力波的大量通量。在这里，我们调查了这些波是否可以沉积足够的热量以破坏燃烧氢的壳，在那里产生对流区，从而驱动卡梅隆 - 福勒工艺以增强表面$^{7} \ mathrm {li} $。我们以详细的恒星进化模型进行研究，发现虽然$ \ sim 10^6 \，l_ \ odot $附近的波浪沉积物，尽管通常会产生对流区，但结果对流并没有足够高，可以与信封合并以与信封相融合，因此无法解释$^7} \ ni} \ ni} $ {limmmm {lim}
Red Clump stars have been found to be enhanced in lithium relative to stars at the tip of the Red Giant Branch (TRGB), which is unexpected in current stellar models. At the TRGB, stars undergo the helium flash, during which helium burning briefly generates roughly $10^9 \, L_\odot$ of power and drives vigorous convection within the star's core. The helium-burning shell excites large fluxes of internal gravity waves. Here we investigate whether or not these waves can deposit enough heat to destabilize the hydrogen-burning shell, generate a convection zone there, and thereby drive the Cameron-Fowler process to enhance surface $^{7}\mathrm{Li}$. We study this with detailed stellar evolution models, and find that while the waves deposit $\sim 10^6 \, L_\odot$ near the hydrogen-burning shell, and while this generally does produce a convection zone, the resulting convection does not reach high enough to merge with the envelope, and so cannot explain enhancements to surface $^{7}\mathrm{Li}$.
