GSH91.5+2-114 is a large HI shell located in the outer Galaxy at a kinematic distance of about 15 kpc. It was first identified in the Canadian Galactic Plane Survey (CGPS) by Pineault et al. (2002) as being possibly associated with objects possessing infrared colors which indicates strong stellar winds. The HI shell has no obvious continuum counterpart in the CGPS radio images at 408 and 1420 MHz or in the IRAS images. We found no evidence for early-type massive stars, most likely as a result of the large extinction that is expected for this large distance. An analysis of the energetics and of the main physical parameters of the HI shell shows that this shell is likely the result of the combined action of the stellar winds and supernova explosions of many stars. We investigate whether a number of slightly extended regions characterized by a thermal radio continuum and located near the periphery of the HI shell could be the result of star formation triggered by the expanding shell.
Probing gas kinematics and PDR structure around O-type stars in Sh 2-305 HII region
利用[CII] 158 $μ$ m谱线数据对银河系HII区Sh 2-305/S305进行了观测研究，这些数据被用来研究光离解区的气体动力学和结构。在[39.4，49.5] km s $^{-1}$的积分[CII]发射图在空间上追踪两个壳状结构（即，内和外中性壳），其总质量为$\sim$ 565 M $_\odot$。内中性壳层的中心有一颗O9.5V恒星，并有一个紧凑的环状外观。然而，外层的[CII]辐射更为广泛和弥散，在其中心有一颗O8.5V恒星，并围绕着内中性壳层。的速度通道图和位置-速度图证实了存在一个紧凑的[CII]壳嵌入在扩散外壳，和两个壳似乎扩大与$v_{\rm exp}\sim$ 1.3公里s $^{-1}$。外壳似乎比内壳更古老，暗示这些壳是顺序形成的。[CII]的配置文件被检查朝向S305，这是双峰或蓝偏，并有更明亮的红移分量。红移和蓝移分量分别在空间上跟踪内部和外部中性壳层几何形状。S305的电离区、中性区和分子区在O型恒星周围彼此相邻。研究了中性壳层周围规则分布的致密分子团和尘埃团（质量为$\sim$ 10-10 $^{3}$ M $_{\odot}$），它们可能是由于收集到的物质壳层中的引力不稳定性而产生的。
Density distribution function of a self-gravitating isothermal compressible turbulent fluid in the context of Molecular Clouds ensembles II: the contribution of the turbulent term and the potential of the outer shells
The interface between the outer heliosphere and the inner lism: Morphology of the local interstellar cloud, its hydrogen hole, stromgren shells, and $^{60}$Fe accretion
