The Spatially Resolved Bipolar Nebula of Sakurai’s Object. II. Mapping the Planetary Nebula Expansion
The Spatially Resolved Bipolar Nebula of Sakurai’s Object. II. Mapping the Planetary Nebula Expansion
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樱井天体的空间分辨双极星云 II。
DOI：
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发表时间：
2014
影响因子：
4.9
通讯作者：
M. Richter
中科院分区：
文献类型：
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作者：
K. Hinkle;R. Joyce;T. Matheson;J. Lacy;M. Richter
樱井天体 (V4334 Sgr) 中氦壳燃烧的最后闪光 (FF) 喷射物的观测结果为 2015 年至 2019 年，即发现后约 20-24 年的时期。 K 处的自适应光学图像追踪膨胀的碎片。虽然大部分喷射物质量为~200 K 尘埃，但一小部分（~0.4%）尘埃质量为~760 K。760 K 连续谱在近红外图像中占主导地位。 He i 10830 Å 中的空间光谱图像显示，位置角为 21° ± 5° 处有一个直径约 16 的双极行星状星云，西南向我们移动，东北向远离我们。在综合光下观察，星云几乎是圆形的。近红外连续谱图像显示喷射物径向远离明亮的中心点源。高分辨率中红外光谱揭示了在灰尘连续体的吸收中看到的膨胀速度为 270 ± 5 km s−1 的分子烃谱线。碳氢化合物源自 FF 中生产的材料。双极星云和碎片云是在高度倾斜的盘模型的背景下讨论的。将 V4334 Sgr 放置在厚盘群中，测量了自行的运动。没有证据表明热白矮星沃尔夫-拉叶（[WR]）风已经出现；未检测到 [WR] 光谱特征。讨论了双星伴星参与演化的可能性。
Observations of the ejecta from the final flash (FF) of helium shell burning in Sakurai’s Object (V4334 Sgr) are presented for 2015–2019, a period ∼20–24 yr after discovery. Adaptive optics images at K s trace the expanding debris. While most of the ejecta mass is in ∼200 K dust, a small fraction, ∼0.4%, of the dust mass is at ∼760 K. The 760 K continuum dominates the near-IR images. Spatial-spectral images in He i 10830 Å show an ∼16 diameter bipolar planetary nebula at position angle 21° ± 5° with the SW moving toward us and the NE moving away. Seen in integrated light, the nebula is nearly circular. Near-IR continuum images show ejecta moving radially away from a bright central point source. High-resolution mid-IR spectra reveal molecular hydrocarbon lines with an expansion velocity of 270 ± 5 km s−1 seen in absorption against the dust continuum. The hydrocarbons originate in material produced in the FF. The bipolar nebula and debris clouds are discussed in the context of a highly inclined disk model. The proper motion has been measured placing V4334 Sgr in the thick disk population. There is no evidence that a hot white dwarf Wolf–Rayet ([WR]) wind has emerged; no [WR] spectral features were detected. The possibility of a binary companion involved in the evolution is discussed.
多极行星状星云的风壳相互作用模型
影响因子：
4.8
作者：
W. Steffen;N. Koning;A. Esquivel;G. Garcia-Segura;M. T. Garcia-Diaz;J. Lopez;M. Magnor
通讯作者：
M. Magnor
影响因子：
4.8
作者：
Yangyuxin Zou;A. Frank;Zhuo Chen;T. Reichardt;O. De Marco-O.-De Marco-2124556154;E. Blackman;J. Nordhaus;B. Balick;J. Carroll-Nellenback;L. Chamandy;Baowei Liu
通讯作者：
Yangyuxin Zou;A. Frank;Zhuo Chen;T. Reichardt;O. De Marco-O.-De Marco-2124556154;E. Blackman;J. Nordhaus;B. Balick;J. Carroll-Nellenback;L. Chamandy;Baowei Liu