论文标题
近距离独立的白矮人 +棕色矮人二进制：进一步的证据证明了公共信封效率的低值
Close detached white dwarf + brown dwarf binaries: further evidence for low values of the common envelope efficiency
论文作者
论文摘要
共同的包膜演化是我们理解包含紧凑型物体的近距离恒星的基本要素，这些恒星包括IA型超新星的祖细胞，短伽马射线爆发和大多数恒星的引力波源。为了预测共同包膜演化的结果，我们仍然在很大程度上依赖于简化的能源保护方程。不幸的是，该公式在理论上包含一个相当差的效率参数（$α_ {\ Mathrm {ce}} $），更糟糕的是，还不清楚除了轨道能量（例如重组能量）之外的能源是否有助于信封弹性过程。在以前的作品中，我们重建了观察到的公共包膜二进制群体（PCEB）的演变，该杂志由白色矮人组成，这些白矮人与主序列星星伴侣组成，发现效率相当小（$α_{\ MATHRM {ce}}} \ simeq0.2-0.3 $），仅在额外的能量源中，这是很少的。在这里，我们使用了相同的重建工具来研究与棕色矮人伴侣观察到的PCEB样本的进化历史。 In contrast to previous works, we found that the evolution of observationally well characterized PCEBs with brown dwarf companions can be understood assuming a low common envelope efficiency ($α_{\mathrm{CE}}=0.24-0.41$), similar to that required to understand PCEBs with main sequence star companions, and that contributions from recombination energy are not required.我们得出的结论是，绝大多数PCEB从共同的包膜演化中形成，可以通过较小的效率进行参数化，而无需考虑其他能源。
Common envelope evolution is a fundamental ingredient in our understanding of the formation of close binary stars containing compact objects which includes the progenitors of type Ia supernovae, short gamma ray bursts and most stellar gravitational wave sources. To predict the outcome of common envelope evolution we still rely to a large degree on a simplified energy conservation equation. Unfortunately, this equation contains a theoretically rather poorly constrained efficiency parameter ($α_{\mathrm{CE}}$) and, even worse, it is unclear if energy sources in addition to orbital energy (such as recombination energy) contribute to the envelope ejection process. In previous works we reconstructed the evolution of observed populations of post common envelope binaries (PCEBs) consisting of white dwarfs with main sequence star companions and found indications that the efficiency is rather small ($α_{\mathrm{CE}}\simeq0.2-0.3$) and that extra energy sources are only required in very few cases. Here we used the same reconstruction tool to investigate the evolutionary history of a sample of observed PCEBs with brown dwarf companions. In contrast to previous works, we found that the evolution of observationally well characterized PCEBs with brown dwarf companions can be understood assuming a low common envelope efficiency ($α_{\mathrm{CE}}=0.24-0.41$), similar to that required to understand PCEBs with main sequence star companions, and that contributions from recombination energy are not required. We conclude that the vast majority of PCEBs form from common envelope evolution that can be parameterized with a small efficiency and without taking into account additional energy sources.
