论文标题
核心氦气闪光期间，通过快速信封膨胀的发作
Onset of common envelope evolution during a core helium flash by rapid envelope expansion
论文作者
论文摘要
我们建议，低质量恒星的红色巨型分支（RGB）的核心氦气闪光灯的剧烈对流会激发能量，这些波浪将能量带到信封上，并将其充气几年，以增加极端水平分支（EHB； SDB和SDO）的数量，而相对于规范的二进制二进制二进制二进制的二进制二进制二进制的恒星。使用开源Mesa-Binary，我们遵循许多初始恒星质量为1.6mo的偏心二进制系统的演变。波带到包膜的能量会导致信封在RGB尖端的膨胀。膨胀的RGB恒星吞噬了许多次要恒星，以启动否则就不会发生的CEE。如果次级恒星设法去除大多数RGB包膜，则主要的演变成质量约为0.47mo的EHB恒星。但是，我们预计在大多数情况下，次级恒星没有时间在闭合轨道上。它宁愿在一个大轨道上结束，并留下足够巨大的包膜，以使主要恒星随后沿渐近巨型分支进化并吞噬次级恒星，从而形成了非球形行星星云。
We suggest that the vigorous core convection during core helium flash on the tip of the red giant branch (RGB) of low mass stars excites waves that carry energy to the envelope and inflate it for few years to increase the number of extreme horizontal branch (EHB; sdB and sdO) stars with masses of ~0.47Mo with respect to canonical binary evolution. Using the open-source MESA-binary we follow the evolution of a number of eccentric binary systems with an initial primary stellar mass of 1.6Mo. The energy that the waves carry to the envelope leads to envelope expansion at the tip of the RGB. The inflated RGB star engulfs many secondary stars to start a CEE that otherwise would not occur. If the secondary star manages to remove most of the RGB envelope the primary evolves to become an EHB star with a mass of ~0.47Mo. However, we expect that in most cases the secondary star does not have time to spiral-in to close orbits. It rather ends at a large orbit and leaves a massive enough envelope for the primary star to later evolve along the asymptotic giant branch and to engulf the secondary star, therefore forming a non-spherical planetary nebula.
