论文标题
在重生的行星星云中，共同的信封进化 - 塑造A30的H缺陷射出
Common envelope evolution in born-again planetary nebulae -- Shaping the H-deficient ejecta of A30
论文作者
论文摘要
在类似太阳能恒星的演变中，重生的行星星云（PNE）是极为罕见的情况。人们普遍认为，他们的中心恒星（CSPN）经历了非常晚的热脉冲（VLTP），在进化的富含H的PN中弹出H缺陷材料。鉴于此事件的短持续时间和CSPN的快速后续演变，质量弹出的细节尚不清楚。我们介绍了围绕年龄的PN（即A30）的H缺陷材料的第一个形态基因模型。最近获得了新的SanPedroMártir观测值，以绘制A30的内部区域，该区域通过软件形状与HST WFC3图像一起解释。最能重现观测值的形状形态模型是由倾斜的$ 37^\ circ $相对于视线和一对正交的双极弹出组成的。我们证实了以前的建议，即接近CSPN的结构具有最高的膨胀速度，即，磁盘的膨胀速度比更远的双极特征更快。我们建议，在VLTP事件之后，可以通过公共信封阶段来解释当前的物理结构和A30周围H缺陷团块的当前物理结构和丰度差异。我们提出的方案也与其他已知的重生pne（A58，A78，Hubi1和Sakurai的对象）进行了比较。
Born-again planetary nebulae (PNe) are extremely rare cases in the evolution of solar-like stars. It is commonly accepted that their central stars (CSPN) experienced a very late thermal pulse (VLTP), ejecting H-deficient material inside the evolved H-rich PN. Given the short duration of this event and the fast subsequent evolution of the CSPN, details of the mass ejection are unknown. We present the first morpho-kinematic model of the H-deficient material surrounding a born-again PN, namely A30. New San Pedro Mártir observations with the Manchester Echelle Spectrograph were recently obtained to map the inner region of A30 which are interpreted by means of the software SHAPE in conjunction with HST WFC3 images. The SHAPE morpho-kinematic model that best reproduces the observations is composed by a disrupted disk tilted $37^\circ$ with respect to the line of sight and a pair of orthogonal opposite bipolar ejections. We confirm previous suggestions that the structures closer to the CSPN present the highest expansion velocities, that is, the disrupted disk expands faster than the farther bipolar features. We propose that the current physical structure and abundance discrepancy of the H-deficient clumps around the CSPN of A30 can be explained by a common envelope phase following the VLTP event. Our proposed scenario is also compared with other known born-again PNe (A58, A78, HuBi1 and the Sakurai's Object).
