Wind mass transfer in S-type symbiotic binaries
Wind mass transfer in S-type symbiotic binaries
复制标题
S型共生双星中的风质量传递
DOI：
10.1051/0004-6361/202039103
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发表时间：
2020
影响因子：
6.5
通讯作者：
F. Teyssier
中科院分区：
文献类型：
--
作者：
N. Shagatova;A. Skopal;S. Shugarov;R. Komžík;E. Kundra;F. Teyssier
上下文共生双星中冷巨星的风的结构携带着重要的信息，可以帮助我们理解风向它们的白色矮星同伴的质量转移，它的燃料，以及共生恒星演化的不同阶段。
目标。本文指出了共生双星星星EG And中红巨星（RG）周围中性风区的非球形分布。我们特别集中在风集中对轨道平面和它的不对称性旁边的RG的轨道运动。
方法.我们通过分析在我们的高节奏中等（R = 11000）和高分辨率（R = 38000）光谱上观察到的Hα和[O III] λ5007线的各个分量的通量和径向速度的周期性轨道变化来实现这一目标。
结果中性风区在近轨道面区域的不对称形状表现为：（i）Hα核辐射通量沿着轨道的不对称过程;（ii）在轨道相位φ = 0.1附近出现次极大值，这可能是折射效应引起的;（iii）Hα宽翼辐射的性质，它起源于H 0原子上的拉曼散射。 风从极地方向向轨道平面基本上被压缩，这受到RG附近[O III] λ5007线发射区在其极点处/周围的位置的限制。极地地区相应的质量损失率为10−8 M yr−1，比RG电离风星云发射的10−7 M yr−1的平均值低10倍。此外，它是两个数量级低于在近轨道平面区域从瑞利散射测量。
结论. EG And星云[O III] λ5007线的惊人特性提供了一个独立的指示，表明风集中在轨道平面上-这是理解共生双星中有效风质量转移的关键。
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, its fuelling, and thus the path towards different phases of symbiotic-star evolution.
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. We concentrate in particular on the wind focusing towards the orbital plane and its asymmetry alongside the orbital motion of the RG.
Methods. We achieved this aim by analysing the periodic orbital variations of fluxes and radial velocities of individual components of the Hα and [O III] λ5007 lines observed on our high-cadence medium (R ∼ 11 000) and high-resolution (R ∼ 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 Hα 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 Hα broad wing emission originating by Raman scattering on H0 atoms. The wind is substantially compressed from polar directions to the orbital plane as constrained by the location of the [O III] λ5007 line emission zones in the vicinity of the RG at/around its poles. The corresponding mass-loss rate from the polar regions of ≲10−8 M⊙ yr−1 is a factor of ≳10 lower than the average rate of ≈10−7 M⊙ yr−1 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 [O III] λ5007 line in EG And provides an independent indication of the wind focusing towards the orbital plane – the key to understanding the efficient wind mass transfer in symbiotic binary stars.
经济实惠的埃歇尔光谱仪，配有 60 厘米望远镜
影响因子：
0.9
作者：
Pribulla;Hambálek;Kollár;Komžík;Kundra;Nedoroščík;Sekeráš;Vaňko
通讯作者：
Vaňko