论文标题
HII区域N83和N84在小麦芽云中的形成，碰撞hi流。
The formation of the HII regions N83 and N84 in the Small Magellanic Cloud triggered by colliding HI flows
论文作者
论文摘要
LHA 115-N 83（N83）和LHA 115-N 84（N84）是与位于小麦哲伦云（SMC）的恒星形成早期阶段相关的HII区域。我们已经通过30英寸的高角度分辨率分析了澳大利亚平方英里阵列途径调查项目的新HI数据。我们发现，具有$ \ sim $ 40 km S $ s $ s $^{ - 1} $速度分离的两个云，与彼此相互融合的循环，并呈现出较大的循环/分散。在100个pc上揭示了10 $^{5} $ $ $ m _ {\ odot} $的块状云，这与HII区域也很好地纠正了，这两个互补组件之间存在一个互补组件之间的位置。 （Fukui等人2020年），提示我们构建了一个较大的系统，我们将两个组件相互碰撞，并触发了N83，N84和六个O型星星的形成，并在其时间范围内以几点不良为单位（$ \ sim $ \ sim $ 60 PC / 40 km S $^sopersonic）。红云的云，其中一些形成了O-Type星星在最后一个Myr中将HII区域电离。
LHA 115-N 83 (N83) and LHA 115-N 84 (N84) are HII regions associated with the early stage of star formation located in the Small Magellanic Cloud (SMC). We have analyzed the new HI data taken with the Galactic Australian Square Kilometre Array Pathfinder survey project at a high angular resolution of 30". We found that the two clouds, having $\sim$40 km s$^{-1}$ velocity separation, show complementary distribution with each other, and part of the HI gas is dispersed by the ionization. In addition, the Atacama Large Millimeter/submillimeter Array observations revealed clumpy CO clouds of 10$^{5}$ $M_{\odot}$ in total over an extent of 100 pc, which are also well correlated with the HII regions. There is a hint of displacement between the two complementary components, which indicate that the red-shifted HI cloud is moving from the north to the south by $\sim$100 pc. This motion is similar to what is found in NGC 602 (Fukui et al. 2020), suggesting a large scale systematic gas flow. We frame a scenario that the two components collided with each other and triggered the formation of N83, N84, and six O-type stars around them in a time scale of a few Myr ($\sim$60 pc / 40 km s$^{-1}$). The supersonic motion compressed the HI gas to form the CO clouds in the red-shifted HI cloud, some of which are forming O-type stars ionizing the HII regions in the last Myr. The red-shifted HI cloud probably flows to the direction of the Magellanic Bridge. The velocity field originated by the close encounter of the SMC with the Large Magellanic Cloud 200 Myr ago as proposed by Fujimoto & Noguchi (1990).
