通过热闪方案模拟富氦次矮星（简要版本）
Modeling He-rich subdwarfs through the hot-flasher scenario (brief version)
摘要：
我们提出了一维数值模拟，旨在研究热闪光的情况下形成的富氦亚矮星。序列计算了广泛的金属丰度和He核心闪光在不同点的后RGB的演变（即不同的残余质量）。我们跟踪了从ZAMS到热闪事件，再到各种热闪事件的亚矮星阶段的完整演化过程。这使我们能够为不同的金属丰度和所有风味的热闪光者提供一组均匀的丰度。我们通过分析对流混合中的一些标准假设的预测表面丰度的影响和元素扩散的影响来扩展我们的工作范围。我们发现，热闪光的情况下是一个可行的解释形成的He-SDO星。我们的研究结果还表明，元素扩散可能会产生（热闪蒸后）富氦气氛转化为氦缺乏的。如果是这样的话，那么热闪光的情况是能够再现的He-sdO恒星的观察到的属性和分布。
英文摘要：
We present 1D numerical simulations aimed at studying the hot-flasher scenario for the formation of He-rich subdwarf stars. Sequences were calculated for a wide range of metallicities and with the He core flash at different points of the post-RGB evolution (i.e. different remnant masses). We followed the complete evolution from the ZAMS, through the hot-flasher event, and to the subdwarf stage for all kinds of hot-flashers. This allows us to present a homogeneous set of abundances for different metallicities and all flavors of hot-flashers. We extend the scope of our work by analyzing the effects in the predicted surface abundances of some standard assumptions in convective mixing and the effects of element diffusion. We find that the hot-flasher scenario is a viable explanation for the formation of He-sdO stars. Our results also show that element diffusion may produce the transformation of (post hot-flasher) He-rich atmospheres into He-deficient ones. If this is so, then the hot-flasher scenario is able to reproduce both the observed properties and distribution of He-sdO stars.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
