In the work presented here, the impact of magnetic field on the dynamical evolution of cometary globules Sim 129 and Sim 130 in the Sh2-236 HII region and the ionized gas streaming out of their surfaces is investigated. The magnetic field morphology in the region associated with these globules is inferred using optical polarization measurements with the Sampurnanand Telescope at ARIES. The nebular emission is probed through radio continuum mapping at 1.4 GHz with the archival National Radio Astronomy Observatory (NRAO) Very Large Array (VLA) Sky Survey (NVSS) data. The correlation of these measurements suggests that photoevaporated gas from the surfaces of Sim 129 and Sim 130 accumulates in clouds and starts streaming along the magnetic field lines. The ¹²CO (J=1–0) molecular line observations are performed towards NGC 1893 from the 14-m single dish radio telescope in Taeduk Radio Astronomy Observatory (TRAO). The velocity dispersion in the ¹²CO (J=1–0) molecular line and the dispersion in polarization angles are considered in the Davis-Chandrasekhar-Fermi formulation to estimate the magnetic field strength towards two Sim nebulae. The average value of field strength is found to be ∼60 μG with uncertainty of 0.5 times the estimated value.

在这里介绍的工作中，研究了磁场对 Sh2-236 HII 区域中彗星球 Sim 129 和 Sim 130 的动力学演化以及从其表面流出的电离气体的影响。使用 ARIES 的 Sampurnanand 望远镜的光学偏振测量推断与这些球体相关区域的磁场形态。星云发射是通过 1.4 GHz 的射电连续谱图探测到的，使用存档的国家射电天文台 (NRAO) 甚大阵列 (VLA) 巡天 (NVSS) 数据。这些测量结果的相关性表明，来自 Sim 129 和 Sim 130 表面的光蒸发气体积聚在云中并开始沿着磁场线流动。在¹²从太德射电天文台 (TRAO) 的 14 米单碟射电望远镜对 NGC 1893 进行 CO (J=1-0) 分子线观测。在 Davis-Chandrasekhar-Fermi 公式中考虑了¹² CO (J=1-0) 分子线中的速度色散和极化角的色散，以估计朝向两个 Sim 星云的磁场强度。发现场强的平均值约为 60 μG，不确定性为估计值的 0.5 倍。