N131: A dust bubble born from the disruption of a gas filament
N131: A dust bubble born from the disruption of a gas filament
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DOI：
10.1051/0004-6361/201526296
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发表时间：
2015-10
影响因子：
6.5
通讯作者：
Chuan-peng Zhang;Guangxing Li;F. Wyrowski;Jun-jie Wang;Jinghua Yuan;Jin-Long Xu;Y. Gong;C. C. Yeh-C.
中科院分区：
文献类型：
--
作者：
Chuan-peng Zhang;Guangxing Li;F. Wyrowski;Jun-jie Wang;Jinghua Yuan;Jin-Long Xu;Y. Gong;C. C. Yeh-C.
上下文OB型恒星具有强烈的电离辐射，并驱动高能风。来自电离恒星的紫外线辐射可能会加热尘埃和可燃气体，从而卷起膨胀的气泡外壳。这个壳层可能是反馈的结果，导致了新一代的恒星。目标。N131是一个位于分子丝中的红外尘埃泡。我们研究了这个气泡的形成和破碎与多波长尘埃和气体的观测。方法.对于气泡N131，我们分析了存档的多波长观测，包括3.6，4.5，5.8，8.0，24，70，160，250，350，500 μm，1.1 mm和21 cm。此外，我们进行了新的观测CO（2-1），CO（1-0），和13 CO（1-0）与IRAM 30米望远镜。结果多波长尘埃和气体观测揭示了一个环状壳层，有致密的碎片，两个平行结构和次级气泡N131-A。气泡N131是一个罕见的物体，在其中心方向上有一个24 μm和21 cm的大孔。尘埃和气体团是紧凑的，可能已经在环状壳的内边缘被压缩，而它们是扩展的，可能预先存在于外边缘。柱密度，激发温度和速度显示出潜在的分层分布从内到外边缘的环状壳。我们还检测了N131 A二次气泡在其中心方向上的正面和背面。N131-A的莱曼连续谱电离光子通量相当于一颗O 9. 5星星。基于上述，我们认为N131气泡可能是由气泡内一组大质量恒星的强烈恒星风触发的。结论.我们提出了一个方案，其中气泡N131的形式从破坏的气体细丝的H II区域的膨胀，强大的恒星风，和碎片下的自引力。
Context. OB-type stars have strong ionizing radiation and drive energetic winds. The ultraviolet radiation from ionizing stars may heat dust and ionize gas to sweep up an expanding bubble shell. This shell may be the result of feedback leading to a new generation of stars. Aims. N131 is an infrared dust bubble residing in a molecular filament. We study the formation and fragmentation of this bubble with multiwavelength dust and gas observations. Methods. Towards the bubble N131, we analysed archival multiwavelength observations including 3.6, 4.5, 5.8, 8.0, 24, 70, 160, 250, 350, 500 μm, 1.1 mm, and 21 cm. In addition, we performed new observations of CO (2–1), CO (1–0), and 13 CO (1–0) with the IRAM 30 m telescope. Results. Multiwavelength dust and gas observations reveal a ring-like shell with compact fragments, two filamentary structures, and the secondary bubble N131-A. Bubble N131 is a rare object with a large hole at 24 μm and 21 cm in the direction of its centre. The dust and gas clumps are compact and might have been compressed at the inner edge of the ring-like shell, while they are extended and might be pre-existing at the outer edge. The column density, excitation temperature, and velocity show a potentially hierarchical distribution from the inner to outer edge of the ring-like shell. We also detected the front and back sides of the secondary bubble N131A in the direction of its centre. The derived Lyman-continuum ionizing photon flux within N131-A is equivalent to an O9.5 star. Based on the above, we suggest that the bubble N131 might be triggered by the strong stellar winds from a group of massive stars inside the bubble. Conclusions. We propose a scenario in which the bubble N131 forms from the disruption of a gas filament by the expansion of the H II region, strong stellar winds, and fragments under self-gravity.