共生星宝瓶座R的双极喷流：使用高分辨率HST WFC3/UVIS照相机对其形态的研究
The bipolar jet of the symbiotic star R Aquarii: A study of its morphology using the high-resolution HST WFC3/UVIS camera
摘要：
R Aqr是一个共生双星系统，由一颗脉动周期为387天的米拉变星和一颗热伴星组成，后者可能是一颗带有吸积盘的白矮星。这个双星系统是一个突出的双极气体外流的来源。我们使用哈勃太空望远镜的高空间分辨率和敏感图像来识别和研究形成R Aqr喷流复杂形态的不同结构成分。方法.我们呈现了2013/14年根据[OIII] 5007，[OI] 6300，[NII] 6583和Ha发射线获得的R Aqr喷流的新的高分辨率HST WFC 3/UVIS窄带图像。这些图像还使我们能够以几种线比（如[OIII]/[OI]和[NII]/[OI]）生成射流的详细地图，这些线比对流出温度及其氢电离分数敏感。新的排放图连同档案HST数据被用来推导和分析的自行突出的排放功能，可以跟踪超过20年的HST观测。这些图像揭示了喷流的精细气体结构，从中心区域到几十角秒的距离，以及在最里面的区域，在恒星源周围的几角秒内。它们首次揭示了直的高度准直的喷流分量，该分量可以在东北方向上追踪到900 AU。[OIII]、[OI]和[NII]中的图像清楚地显示了射流束中的螺旋图案，这可能来自射流的小尺度进动。高度准直的射流伴随着由低激发气体填充的大开度角流出。计算了射流结构的位置角和张开角。我们的一些突出的排放结的自行测量确认的情况下，气体加速外流的传播过程中。
英文摘要：
R Aqr is a symbiotic binary system consisting of a Mira variable with a pulsation period of 387 days and a hot companion which is presumably a white dwarf with an accretion disk. This binary system is the source of a prominent bipolar gaseous outflow. We use high spatial resolution and sensitive images from the Hubble Space Telescope to identify and investigate the different structural components that form the complex morphology of the R Aqr jet . Methods. We present new high-resolution HST WFC3/UVIS narrow-band images of the R Aqr jet obtained in 2013/14 in the light of the [OIII] 5007, [OI] 6300, [NII] 6583, and Ha emission lines. These images also allow us to produce detailed maps of the jet flow in several line ratios such as [OIII]/[OI] and [NII]/[OI] which are sensitive to the outflow temperature and its hydrogen ionisation fraction. The new emission maps together with archival HST data are used to derive and analyse the proper motion of prominent emitting features which can be traced over 20 years with the HST observations. The images reveal the fine gas structure of the jet out to distances of a few ten arcseconds from the central region, as well as in the innermost region, within a few arcseconds around the stellar source. They reveal for the first time the straight highly-collimated jet component which can be traced to up to 900 AU in the NE direction. Images in [OIII], [OI], and [NII] clearly show a helical pattern in the jet beams which may derive from the small-scale precession of the jet. The highly-collimated jet is accompanied by a wide opening angle outflow which is filled by low excitation gas. The position angles of the jet structures as well as their opening angles are calculated. Our measurements of the proper motions of some prominent emission knots confirm the scenario of gas acceleration during the propagation of the outflow.
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