Common envelope evolution on the asymptotic giant branch: unbinding within a decade?
Common envelope evolution on the asymptotic giant branch: unbinding within a decade?
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DOI：
10.1093/mnras/staa1273
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发表时间：
2020-04
影响因子：
4.8
通讯作者：
L. Chamandy;E. Blackman;A. Frank;J. Carroll-Nellenback;Yisheng Tu
中科院分区：
文献类型：
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作者：
L. Chamandy;E. Blackman;A. Frank;J. Carroll-Nellenback;Yisheng Tu
共同包层演化是许多高能天体物理现象的重要起源阶段，但人们对这一阶段的认识还很不够。虽然3D全球流体动力CE模拟已经变得越来越普遍，在最近几年，那些涉及渐近巨星分支（AGB）的主要是稀缺的，由于从更大的动力学范围相比，红巨星分支（RGB）的主要计算成本高。但是，与AGB祖先的CE演化是值得模拟的，因为这些事件是大多数双极行星状星云（PNE）的可能祖先，也是CE物理学的重要观测试验场。在这里，我们提出了一个高分辨率的全球模拟CE演变涉及一个AGB的主要和$1\，\mathrm {M}_\odot$中学，进化为$20$的轨道革命。在这些轨道的最后16 $期间，包络以大约0.1 $-0.2\，\mathrm {M}_\odot\，\mathrm{yr}^{-1}$的几乎恒定的速率解束缚。如果保持这个速度，信封将在不到10\，\marthm {yr}$的时间内被解开。这种不受约束的主导来源是一致的inspiral的，我们评估的影响，周围的介质是subdominant。我们将这次运行与以前的运行进行比较，以前的运行使用从相同的2\，\mathrm {M}_\odot$星星演化而来的RGB相位原色，以评估原色演化状态的影响。当适当缩放时，两次运行非常相似，但有一些重要的差异。
Common envelope (CE) evolution is a critical but still poorly understood progenitor phase of many high-energy astrophysical phenomena. Although 3D global hydrodynamic CE simulations have become more common in recent years, those involving an asymptotic giant branch (AGB) primary are scarce, due to the high computational cost from the larger dynamical range compared to red giant branch (RGB) primaries. But CE evolution with AGB progenitors is desirable to simulate because such events are the likely progenitors of most bi-polar planetary nebulae (PNe), and prominent observational testing grounds for CE physics. Here we present a high resolution global simulation of CE evolution involving an AGB primary and $1\,\mathrm{M}_\odot$ secondary, evolved for $20$ orbital revolutions. During the last $16$ of these orbits, the envelope unbinds at an almost constant rate of about $0.1$-$0.2\,\mathrm{M}_\odot\,\mathrm{yr}^{-1}$. If this rate were maintained, the envelope would be unbound in less than $10\,\mathrm{yr}$. The dominant source of this unbinding is consistent with inspiral; we assess the influence of the ambient medium to be subdominant. We compare this run with a previous run that used an RGB phase primary evolved from the same $2\,\mathrm{M}_\odot$ main sequence star to assess the influence of the evolutionary state of the primary. When scaled appropriately, the two runs are quite similar, but with some important differences.