论文标题
二进制后星星中旋转和膨胀气体
Rotating and Expanding Gas in Binary Post-AGB Stars
论文作者
论文摘要
有一类二进制后AGB恒星（包括后AGB恒星在内的二进制系统），这些恒星周围环绕着开普勒磁盘和由于从磁盘中逸出的气体而导致的流出。迄今为止，有七个来源通过CO线的干涉毫米波（ALMA/NOEMA）进行了详细研究。对于红色矩形，IW Carinae，IRA，IRAS 08544-4431和AC Herculis的情况，发现具有开普勒动力学的磁盘中，大约有85％的整个Nebular质量大于85％。静脉质量的其余部分位于扩展的成分中。此流出可能是磁盘风，包括从旋转磁盘中逸出的材料组成。这些来源是磁盘主导的星云。 On the contrary, our maps and modeling of 89 Herculis, IRAS 19125+0343, and R Scuti, which allowed us to study their morphology, kinematics, and mass distribution, suggest that, in these sources, the outflow clearly is the dominant component of the nebula (around 75% of the total nebular mass), resulting in a new subclass of nebulae around binary post-AGB stars: the流出主导的来源。BesidesCo，到目前为止，这种类型的来源的化学实际上是未知的。我们还提出了在1.3、2、3、7和13 mM频段（望远镜时间约600 h）中进行非常深的单次无线电分子调查。我们的结果和检测使我们能够将源分类为O-或C-RICH。我们还得出结论，与AGB恒星相比，CO以外的检测到的分子物种的计算丰度特别低。在旋转磁盘是星云的主要成分的来源中，这一事实非常重要。
There is a class of binary post-AGB stars (binary system including a post-AGB star) that are surrounded by Keplerian disks and outflows resulting from gas escaping from the disk. To date, there are seven sources that have been studied in detail through interferometric millimeter-wave maps of CO lines (ALMA/NOEMA). For the cases of the Red Rectangle, IW Carinae, IRAS 08544-4431, and AC Herculis, it is found that around greater than 85% of the total nebular mass is located in the disk with Keplerian dynamics. The remainder of the nebular mass is located in an expanding component. This outflow is probably a disk wind consisting of material escaping from the rotating disk. These sources are the disk-dominated nebulae. On the contrary, our maps and modeling of 89 Herculis, IRAS 19125+0343, and R Scuti, which allowed us to study their morphology, kinematics, and mass distribution, suggest that, in these sources, the outflow clearly is the dominant component of the nebula (around 75% of the total nebular mass), resulting in a new subclass of nebulae around binary post-AGB stars: the outflow-dominated sources.Besides CO, the chemistry of this type of source has been practically unknown thus far. We also present a very deep single-dish radio molecular survey in the 1.3, 2, 3, 7, and 13 mm bands (around 600 h of telescope time). Our results and detections allow us to classify our sources as O- or C-rich. We also conclude that the calculated abundances of the detected molecular species other than CO are particularly low, compared with AGB stars. This fact is very significant in those sources where the rotating disk is the dominant component of the nebula.
