共生恒星v1016 cygni中vi λ 1032, 1038散射的吸积流和不同的拉曼谱线

IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS
Jeong-Eun Heo, Hee-Won Lee
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引用次数: 12

摘要

共生恒星V1016 Cygni是一个分离的双星系统,由一颗热白矮星和一颗损失质量的Mira变星组成,在6825 a和7082 a附近显示出非常广泛的发射特征,这是拉曼散射的Ovi ?1032 1038是氢原子。在用Bohyunsan光学梯队光谱仪获得的V1016 Cyg的高分辨率光谱中,这些广泛的特征表现出双峰分布,其中红色峰比蓝色峰强。然而,当两个拉曼特征在多普勒因子空间中表现出相同的红峰强度时,7082特征的蓝峰相对弱于6825特征。假设白矮星周围的吸积流是双峰分布的原因,我们将这种分布的差异归因于Ovi ??1032 1038在吸积流中。利用蒙特卡罗技术给出了白矮星附近的Ovi 1032和Ovi 1038的局部发射率图。我们还提出了一个地图,表明不同的通量比Ovi ??1032和1038。结果表明,在拉曼特征中心槽的发射区,其通量比达到最大值2,而内部红色发射区的通量比几乎为1。蓝色发射区和外部红色发射区表现出1.5左右的中间比值。我们得出结论,两个拉曼Ovi特征轮廓的差异强烈暗示白矮星周围的吸积流,这是方位不对称的。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
ACCRETION FLOW AND DISPARATE PROFILES OF RAMAN SCATTERED O VI λλ 1032, 1038 IN THE SYMBIOTIC STAR V1016 CYGNI
The symbiotic star V1016 Cygni, a detached binary system consisting of a hot white dwarf and a mass-losing Mira variable, shows very broad emission features at around 6825 A and 7082 A, which are Raman scattered Ovi ?? 1032, 1038 by atomic hydrogen. In the high resolution spectrum of V1016 Cyg obtained with the Bohyunsan Optical Echelle Spectrograph these broad features exhibit double peak profiles with the red peak stronger than the blue counterpart. However, their profiles differ in such a way that the blue peak of the 7082 feature is relatively weaker than the 6825 counterpart when the two Raman features are normalized to exhibit an equal red peak strength in the Doppler factor space. Assuming that an accretion flow around the white dwarf is responsible for the double peak profiles, we attribute this disparity in the profiles to the local variation of the flux ratio of Ovi ?? 1032, 1038 in the accretion flow. A Monte Carlo technique is adopted to provide emissivity maps showing the local emissivity of Ovi ?1032 and Ovi ?1038 in the vicinity of the white dwarf. We also present a map indicating the differing flux ratios of Ovi ?? 1032 and 1038. Our result shows that the flux ratio reaches its maximum of 2 in the emission region responsible for the central trough of the Raman feature and that the flux ratio in the inner red emission region is almost 1. The blue emission region and the outer red emission region exhibit an intermediate ratio around 1.5. We conclude that the disparity in the profiles of the two Raman Ovi features strongly implies accretion flow around the white dwarf, which is azimuthally asymmetric.
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来源期刊
Journal of the Korean Astronomical Society
Journal of the Korean Astronomical Society 地学天文-天文与天体物理
CiteScore
1.30
自引率
10.00%
发文量
0
审稿时长
>12 weeks
期刊介绍: JKAS is an international scientific journal publishing papers in all fields of astronomy and astrophysics. All manuscripts are subject to the scrutiny of referees. Manuscripts submitted to JKAS must comply with the ethics policy of JKAS. Six regular issues are published each year on February 28, April 30, June 30, August 31, October 31, and December 31. One year''s issues compose one volume.
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