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首页> 外文期刊>The Astrophysical journal >X-RAY EMISSION FROM THE WIND-BLOWN BUBBLE IN THE PLANETARY NEBULA BD +30°3639
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X-RAY EMISSION FROM THE WIND-BLOWN BUBBLE IN THE PLANETARY NEBULA BD +30°3639

机译：行星状星云BD的风吹泡泡的X射线辐射+ 30°3639

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摘要

An X-ray spectrum of a wind-blown bubble in the planetary nebula BD +30°3639, acquired by the Advanced Satellite for Cosmology and Astrophysics (ASCA), shows the presence of hot (T = 3 X 10~6 K) gas dominated by the Ne Kα line complex. There is circumstantial evidence for the enhanced abundances of other H- and He-burning products, although O is not as abundant as in the extremely C-rich stellar wind of the W-R central star. The temperature of the hot gas is several times lower than expected behind the shock from the 700 km s~(-1) stellar wind. This might be caused by variations in the stellar wind speed and its chemical abundances induced by the central star evolution, and possibly aided by mixing of the stellar wind gas with the nebular material. Mixing is hinted by the discovery of small (0.2″) dusty clumps in the Hubble Space Telescope (HST) narrowband images of the nebula in [S III] λ532 and [O II] λ3727 emission lines. These clumps are projected against an axisymmetric, nearly square nebular shell and are most likely associated with the neutral and molecular envelope surrounding the wind-blown bubble and the wind-swept shell.
机译：先进的宇宙学和天体物理学卫星（ASCA）获得的BD + 30°3639行星云中的风吹气泡的X射线光谱表明存在热气体（T = 3 X 10〜6 K）由NeKα线络合物主导。尽管O不像W-R中心恒星的极富C的恒星风中的O那样丰富，但有间接证据表明其他H和He燃烧产物的丰度增加。在700 km s〜（-1）恒星风的冲击后，热气体的温度比预期的温度低几倍。这可能是由于恒星风速的变化及其由中央恒星演化引起的化学丰度引起的，并且可能是由于恒星风气体与星云物质的混合而产生的。在[S III]λ532和[O II]λ3727发射线中，在哈勃太空望远镜（HST）的窄带图像中发现了小的（0.2“）尘埃团提示了混合。这些团块投射在一个轴对称，近乎正方形的星状壳上，最有可能与包围着风吹泡泡和被风吹扫的壳的中性和分子包膜有关。

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