NGC2363的恒星超星系团A中的宽H α，[O III ]线翼和湍流混合层假说
The broad H-alpha, [O III] line wings in stellar supercluster A of NGC2363 and the turbulent mixing layer hypothesis
摘要：
上下文超星系团A位于河外HII区NGC 2363，它的高超音速气体被认为是微弱的宽发射线，全宽为零，强度为7000 km/s。目标。我们探讨的可能性，所观察到的广泛的配置文件是一个高速集群风与密集的光电离团块的相互作用的结果。方法.所考虑的几何形状是近静态的光致电离凝结，在其表面的湍流混合层出现的结果，与热风的相互作用。湍流的近似处理采用Canto & Raga的混合长度方法。代码映射Ic用于导出描述流动的平均量并计算湍流层内的线发射率。对线源的三维速度投影进行了解析计算。结果似乎需要高达~ 4300 km/s的快速夹带风才能再现宽H-α和[O III]剖面的微弱机翼。然而，3500公里/秒的较慢风速仍然可以再现大部分的宽分量，并且确实比特别的高斯廓线提供更好的拟合。结论.在3D径向加速（远离超星系团A）的排放气体提供了一个合理的一阶拟合的宽线分量。如所观察到的，对于[N II]和[S II]线没有预测广泛的组分。所需的风速高得令人不安，可能必须考虑其他方法，使排放气体的加速度达到4000 km/s。
英文摘要：
Context. SuperclusterA in the extragalactic HII region NGC2363 is remarkable for the hypersonic gas seen as faint extended broad emission lines with a full width zero intensity of 7000km/s. Aims. We explore the possibility that the observed broad profiles are the result of the interaction of a high velocity cluster wind with dense photoionized clumps. Methods. The geometry considered is that of near static photoionized condensations at the surface of which turbulent mixing layers arise as a result of the interaction with the hot wind. The approximative treatment of turbulence is carried out using the mixing length approach of Canto & Raga. The code mappings Ic is used to derive the mean quantities describing the flow and to compute the line emissivities within the turbulent layers. The velocity projection in three dimensions of the line sources is carried out analytically. Results. A fast entraining wind of up to ~4300km/s appears to be required to reproduce the faint wings of the broad H-alpha and [O III] profiles. A slower wind of 3500km/s, however, can still reproduce the bulk of the broad component and does provide a better fit than an ad hoc Gaussian profile. Conclusions. Radial acceleration in 3D (away from supercluster A) of the emission gas provides a reasonable first order fit to the broad line component. No broad component is predicted for the [N II] and [S II] lines, as observed. The wind velocity required is uncomfortably high and alternative processes that would provide comparable constant acceleration of the emission gas up to 4000km/s might have to be considered.
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