论文标题
K Supergiant失控星高清137071
The K supergiant runaway star HD 137071
论文作者
论文摘要
很少有人知道红色超级逃亡者的示例，所有这些例子都从更大的O型前体中降下，但是没有来自质量较低的B型前体，尽管B型恒星中的失控统计数据表明K型Runaways必须相对多。我们研究HD 137071，这是一颗被认为是正常K型红色巨人的恒星。它通过Gaia测得的视差和衍生的光度表明它实际上是一个超级巨人，而其派生到银河平面的距离及其空间速度相对于当地的静止标准，其空间速度为54.1 km s $^{ - 1} $也表明它也是逃跑之星。然而，即使在盖亚时代，在确定凉爽超级巨人的三角透视上的固有局限性也需要准确的光谱分类来确认。我们可靠地将HD 137071分类为K4II恒星，以建立其与极端人群I的成员资格，这与使用Gaia DR2 DR2视差测量得出的亮度一致。 GAIA DR2目录的运动学数据证实了其高空间速度及其失控的性质。将光谱分类与天体信息，一种最先进的银河电位模型以及高质量恒星的进化模型相结合，我们追踪了HD 137071的运动回到银河平面的接近性，并推测了两种拟议机制中的飞行恒星的生产中的两种拟议机制可能负责HD 137071的高速级别的高速级别。二进制系统大约32 Myr发生了超新星爆炸的二进制系统。
Very few examples are known of red supergiant runaways, all of them descending from the more massive O-type precursors, but none from the lower mass B-type precursors, although runaway statistics among B-type stars suggest that K-type runaways must be relatively numerous. We study HD 137071, a star that has been considered so far as a normal K-type red giant. Its parallax measured by Gaia and the derived luminosity suggest that it is actually a supergiant, whereas its derived distance to the galactic plane and its spatial velocity of 54.1 km s$^{-1}$ with respect to the local standard of rest suggest that it is also a runaway star. However, intrinsic limitations in determining the trigonometric parallaxes of cool supergiants, even in the Gaia era, require accurate spectral classifications for confirmation. We reliably classify HD 137071 as a K4II star establishing its membership to the extreme Population I, which is in agreement with the luminosity derived using the Gaia DR2 parallax measurement. Kinematical data from the Gaia DR2 catalog confirm its high spatial velocity and its runaway nature. Combining the spectral classification with astrometric information, a state-of-the-art galactic potential model, and evolutionary models for high-mass stars we trace the motion of HD 137071 back to the proximities of the galactic plane and speculate on which of the two proposed mechanisms for the production of runaway stars may be responsible for the high velocity of HD 137071. The available data favor the formation of HD 137071 in a massive binary system where the more massive companion underwent a supernova explosion about 32 Myr ago.
