论文标题
Stingray行星星云及其中央恒星V839 ARAE的惊人快速发展
Startlingly Fast Evolution of the Stingray Planetary Nebula and its Central Star, V839 Arae
论文作者
论文摘要
行星星云（PN）称为黄貂鱼（PN G331.3 $ - $ 12.1）突然在1980年代突然打开，其中心星（V839 ARA）开始了快速进化，大小，表面温度和表面上的幅度很大，表面重力和表面重力很大，也许是较晚的热脉冲，也许是在Hertzssprundzssprund的一部分中引起了loop的一部分。有了这些快速的变化，我们在2016年使用了哈勃太空望远镜拍摄了图像。我们看不到1980年代的高速质量损失，要么接近中心恒星，要么是远离星星的团块或变化，远离恒星，或者是局部或一般性的弹性升高而导致的壳弹性弹性弹性的弹性升高，导致壳的震惊。我们认为，缺乏即将发出的材料是因为相对较小的总质量已经在1992年第一次解决成像之前就已经足够了PN，正是这种影响最初从1980年代开始将Stingray引起的冲击。我们还量化了黄貂鱼的复杂快速褪色，每个发射线和每个结构都具有不同的淡出速率，半衰期为3至29年。在一两个世纪的时间里，PN将逐渐消失。随着不同结构的这种复杂褪色，不可能得出PN的任何膨胀速率。从1996年到2016年，中央恒星的亮度大约是恒定的，但在$ V $ band中的差异从15.50到14.18 mag。
The planetary nebula (PN) called the Stingray (PN G331.3$-$12.1) suddenly turned on in the 1980s, and its central star (V839 Ara) started a fast evolution with large amplitudes in magnitude, surface temperature, and surface gravity, perhaps as part of a late thermal pulse causing a loop in the Hertzsprung-Russell (HR) diagram. With these fast changes, we have taken images with the Hubble Space Telescope in 2016. We do not see the massive high-velocity mass loss of the 1980s, either close in to the central star, or as clumps or changes in the nebula far from the star, or as localized or general increases in the emission-line flux caused by the shocks of the outflowing ejecta ramming into the slow-moving PN shell. We think that the lack of seeing the outgoing material is because the relatively modest total mass had already suffused the PN before the first resolved imaging in 1992, and it was the shocks from this impact that initially ionized the Stingray starting in the 1980s. We also quantify the complex fast fading of the Stingray, with each emission line and each structure having different fade rates, with half-lives ranging from 3 to 29 years. In a century or two, the PN will fade to invisibility. With this complex fading of different structures, it is impossible to derive any expansion rate for the PN. The central star had its brightness roughly constant from 1996 to 2016, but with substantial erratic variability from 15.50 to 14.18 mag in the $V$ band.
