论文标题
S型共生二进制文件III中的风质传递。确认来自Nebular [OIII]λ5007线的EG仙女座的风聚焦
Wind mass transfer in S-type symbiotic binaries III. Confirmation of a wind focusing in EG Andromedae from the nebular [OIII]λ5007 line
论文作者
论文摘要
语境。来自共生二进制的酷巨人的风结构提供了重要的信息，以了解风向大量转移到其白矮人的同伴及其加油。目标。在本文中，我们指出了共生二进制恒星中红色巨人（RG）周围中性风带的非球形分布，例如。方法。我们通过分析了H $α$的单个组件的通量和径向速度的周期性轨道变化和[OIII] $λ$ 5007的线路（R $ $ \ sim $ 11 000）和高分辨率（R $ \ sim $ 38 000）光谱。结果。近轨平面区域中性风带的不对称塑形由以下方式指示：（i）沿轨道沿轨道的H $α$核心发射通量的不对称过程； （ii）在轨道相$φ= 0.1 $周围存在其次级最大值，这可能是由折射效应引起的； （iii）h $α$宽翼排放的特性，由拉曼散射在h $^0 $原子上。从极地方向到轨道平面的风被基本压缩，这受到[OIII] $λ$ 5007线发射区的位置，该线在其杆周围的RG附近。 $ \ lyssim 10 ^{ - 8} $ msun/yr的相应质量损失率是$ \ gtrsim 10 $的一个因素，低于$ \ $ \ $ \ \ \ \ \ 10 ^{ - 7} $ msun/yr的平均速率，源自来自RG的Ionions Wind。此外，它比瑞利散射中近轨道平面区域中测得的数量级低两个。结论。 Nebular [OIII] $λ$ 5007线的惊人特性在EG中提供了独立的指示，表明风集中在轨道平面上。
Context. The structure of the wind from the cool giants in symbiotic binaries carries important information for understanding the wind mass transfer to their white dwarf companions and its fuelling. Aims. In this paper, we indicate a non-spherical distribution of the neutral wind zone around the red giant (RG) in the symbiotic binary star, EG And. Methods. We achieved this aim by analysing the periodic orbital variations of fluxes and radial velocities of individual components of the H$α$ and [OIII]$λ$5007 lines observed on our high-cadence medium (R $\sim$ 11 000) and high-resolution (R $\sim$ 38 000) spectra. Results. The asymmetric shaping of the neutral wind zone at the near-orbital-plane region is indicated by: (i) the asymmetric course of the H$α$ core emission fluxes along the orbit; (ii) the presence of their secondary maximum around the orbital phase $φ= 0.1$, which is possibly caused by the refraction effect; and (iii) the properties of the H$α$ broad wing emission originating by Raman scattering on H$^0$ atoms. The wind is substantially compressed from polar directions to the orbital plane as constrained by the location of the [OIII]$λ$5007 line emission zones in the vicinity of the RG at/around its poles. The corresponding mass-loss rate from the polar regions of $\lesssim 10 ^{-8}$ Msun/yr is a factor of $\gtrsim 10$ lower than the average rate of $\approx 10^{-7}$Msun/yr derived from nebular emission of the ionised wind from the RG. Furthermore, it is two orders of magnitude lower than that measured in the near-orbital-plane region from Rayleigh scattering. Conclusions. The startling properties of the nebular [OIII]$λ$5007 line in EG And provides an independent indication of the wind focusing towards the orbital plane.
