再一次行星状星云HuBi 1的形成和命运
Formation and fate of the born-again planetary nebula HuBi 1
摘要：
我们提出了第一个3D辐射流体动力学模拟的形成和演化的再次行星状星云（PNe），特别强调的情况下，HuBi 1，由内而外的PN。我们使用经过广泛测试的GUACHO程序模拟HuBi 1的形成，采用我们小组从观测中获得的质量损失和恒星风终极速度估计。我们发现，如果HuBi 1的内壳层是由一个爆炸性的甚晚热脉冲（VLTP）喷射的材料与$\sim$ 300 km s $^{-1}$的速度形成的，这个结构的年龄是一致的$\simeq$ 200 yr的多历元窄带成像。我们的模拟预测，作为VLTP期间恒星风速度和光子电离通量的急剧减少的结果，外部富氢星云的速度和压力结构受到影响，产生湍流电离结构周围的内壳。这些确实在加那利大望远镜MEGARA光学观测中发现。此外，我们证明了目前相对较低的电离光子通量从中央恒星的HuBi 1是不能够完全覆盖的内壳层，这有利于以前的建议，它的激发是由冲击占主导地位。我们的模拟表明，HuBi 1的贫氢喷出物的动能至少是进化后的再次PNe A30和A78中的团块和细丝的30倍，使其成为一个真正独特的VLTP事件。
英文摘要：
We present the first 3D radiation-hydrodynamic simulations on the formation and evolution of born-again planetary nebulae (PNe), with particular emphasis to the case of HuBi1, the inside-out PN. We use the extensively-tested GUACHO code to simulate the formation of HuBi1 adopting mass-loss and stellar wind terminal velocity estimates obtained from observations presented by our group. We found that, if the inner shell of HuBi1 was formed by an explosive very late thermal pulse (VLTP) ejecting material with velocities of $\sim$300 km s$^{-1}$, the age of this structure is consistent with that of $\simeq$200 yr derived from multi-epoch narrow-band imaging. Our simulations predict that, as a consequence of the dramatic reduction of the stellar wind velocity and photon ionizing flux during the VLTP, the velocity and pressure structure of the outer H-rich nebula are affected creating turbulent ionized structures surrounding the inner shell. These are indeed detected in Gran Telescopio Canarias MEGARA optical observations. Furthermore, we demonstrate that the current relatively low ionizing photon flux from the central star of HuBi1 is not able to completely ionize the inner shell, which favors previous suggestions that its excitation is dominated by shocks. Our simulations suggest that the kinetic energy of the H-poor ejecta of HuBi1 is at least 30 times that of the clumps and filaments in the evolved born-again PNe A30 and A78, making it a truly unique VLTP event.
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