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首页> 外文期刊>The Astrophysical journal >RAMAN-SCATTERED He Ⅱ λ6545 LINE IN THE SYMBIOTIC STAR V1016 CYGNI
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RAMAN-SCATTERED He Ⅱ λ6545 LINE IN THE SYMBIOTIC STAR V1016 CYGNI

机译：象征星V1016 CYGNI中的拉曼散射HeⅡλ6545线

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We present a spectrum of the symbiotic star V1016 Cyg observed with the 3.6 m Canada-France-Hawaii Telescope, in order to illustrate a method to measure the covering factor of the neutral scattering region around the giant component with respect to the hot emission region around the while dwarf component. In the spectrum, we find broad wings around Hα and a broad emission feature around 6545 A that is blended with the [N Ⅱ] λ6548 line. These two features are proposed to be formed by Raman scattering by atomic hydrogen, where the incident radiation is proposed to be UV continuum radiation around Lyβ in the former case and the He Ⅱ λ1025 emission line arising from n= 6 → n = 2 transitions for the latter feature. We remove the Hα wings by a template Raman scattering wing profile and subtract the [N Ⅱ] λ6548 line using the 3 times stronger [N Ⅱ] λ6583 feature in order to isolate the He Ⅱ Raman-scattered 6545 A line. We obtain the flux ratio F_(6545)/F_(6560) = 0.24 of the He Ⅱ λ6560 emission line and the 6545 A feature for V1016 Cyg. Under the assumption that the He Ⅱ emission from this object is isotropic, this ratio is converted to the ratio Φ_(6545)/Φ_(1025) = 0.17 of the number of the incident photons and that of the scattered photons. This implies that the scattering region with H Ⅰ column density N_(H Ⅰ) ≥ 10~(20) cm~(-2) covers 17% of the emission region. By combining the presumed binary period of ～ 100 yr for this system we infer that a significant fraction of the slow stellar wind from the Mira component is ionized and that the scattering region around the Mira extends a few tens of AU, which is closely associated with the mass loss process of the Mira component. It is argued that the Raman-scattered He Ⅱ λ6545 line is an important and useful tool to investigate the mass-loss process occurring in the late stage of stellar evolution.
机译：我们展示了用3.6 m加拿大-法国-夏威夷望远镜观测到的共生恒星V1016 Cyg的光谱，以说明一种相对于周围热发射区测量巨组分周围的中性散射区的覆盖因子的方法而矮人的组成部分。在光谱中，我们发现围绕Hα的宽翼和大约6545 A的宽发射特征与[NⅡ]λ6548谱线混合在一起。这两个特征被认为是由原子氢的拉曼散射形成的，在前一种情况下，入射辐射被认为是Lyβ周围的紫外线连续辐射，而由于n = 6→n = 2跃迁而引起的HeⅡλ1025发射谱线。后一个功能。我们通过模板拉曼散射机翼轮廓去除Hα机翼，并使用3倍强的[NⅡ]λ6583特征减去[NⅡ]λ6548谱线，以分离HeⅡ拉曼散射的6545 A谱线。我们获得HeⅡλ6560发射谱线的通量比F_（6545）/ F_（6560）= 0.24和V1016 Cyg的6545 A特征。在该物体的HeⅡ发射是各向同性的假设下，该比率转换为入射光子数和散射光子数的比值Φ_（6545）/Φ_（1025）= 0.17。这意味着HⅠ柱密度N_（HⅠ）≥10〜（20）cm〜（-2）的散射区覆盖了发射区的17％。通过结合该系统的假定的约100年的二进位周期，我们可以推断出，来自Mira分量的大部分恒星慢风被电离，并且Mira周围的散射区域扩展了几十个AU，这与Mira组件的质量损失过程。有人认为，拉曼散射的HeⅡλ6545谱线是研究恒星演化后期发生的质量损失过程的重要和有用的工具。

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