猎户座的面纱：四边形星团前面的PDR的磁场强度和其他性质
Orion's Veil: Magnetic field strengths and other properties of a PDR in front of the Trapezium Cluster
摘要：
我们提出了一个分析的物理条件在猎户座面纱，一个主要的原子PDR，就在前面（约2 pc）的梯形恒星。我们获得了21厘米HI和18厘米OH VLA塞曼效应数据。这些数据产生了面纱原子和分子区域的视线磁场强度Blos的图像。我们发现，在面纱的大部分区域，原子气体中的Blos通常为-50至-75微高斯（25”分辨率）;在分子气体中的一个位置，Blos为-350微高斯（40”分辨率）。面纱有两个主要的HI速度分量。磁性和运动学数据表明，这些组件之间的密切联系。它们可能代表弱D电离前沿前的激波两侧的气体。Veil HI组件中的磁场比ISM中N（H）和n（H）相当的其他位置强3-5倍。HI组分是磁亚临界的（磁主导的），像CNM一样，尽管它们的密度约为1 dex。Veil HI组件中的强场可能是由扩散气体中的低湍流条件引起的，该扩散气体导致了OMC-1。强磁场也可能与自恒星形成以来在面纱中发展的静磁平衡有关。我们认为猎户座-S分子核心的位置，提出了一个位置背后的主要猎户座H+区域。
英文摘要：
We present an analysis of physical conditions in the Orion Veil, a largely atomic PDR that lies just in front (about 2 pc) of the Trapezium stars. We have obtained 21 cm HI and 18 cm OH VLA Zeeman effect data. These data yield images of the line-of-sight magnetic field strength Blos in atomic and molecular regions of the Veil. We find Blos is typically -50 to -75 microgauss in the atomic gas across much of the Veil (25" resolution); Blos is -350 microgauss at one position in the molecular gas (40" resolution). The Veil has two principal HI velocity components. Magnetic and kinematical data suggest a close connection between these components. They may represent gas on either side of a shock wave preceding a weak-D ionization front. Magnetic fields in the Veil HI components are 3-5 times stronger than they are elsewhere in the ISM where N(H) and n(H) are comparable. The HI components are magnetically subcritical (magnetically dominated), like the CNM, although they are about 1 dex denser. Strong fields in the Veil HI components may have resulted from low turbulence conditions in the diffuse gas that gave rise to OMC-1. Strong fields may also be related to magnetostatic equilibrium that has developed in the Veil since star formation. We consider the location of the Orion-S molecular core, proposing a location behind the main Orion H+ region.
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