论文标题
在金牛座分子云中，磁场和表面亮度梯度之间的相对方向
The relative orientation between the magnetic field and gradients of surface brightness within thin velocity slices of 12CO and 13CO emission from the Taurus molecular cloud
论文作者
论文摘要
我们使用12CO和13CO天线温度的薄速度切片的空间梯度来检查星际磁场在金牛座分子云中调节湍流方向的作用。我们的分析解释了源是光谱的热噪声引起的梯度的随机误差。比较了与天线温度梯度向量正常的矢量的方向与根据Planck 353〜GHz极化数据计算得出的磁场方向。这些相对取向用投影的瑞利统计量和平均结果向量进行了参数化。对于12CO，云面积的28％和39％分别表现出牢固或强烈的垂直相对取向。对于较低的不透明度13CO排放，分别在7％和43％的云区域中发现了强距离和强烈的垂直方向。对于这两种同位素学，强烈平行或垂直的比对仅限于湍流水平较低的局部区域。如果相对方向是与Alfgenic Mach数字的观察性替代，那么我们的结果意味着整个云中Alfgenic Mach数的局部变化。
We examine the role of the interstellar magnetic field to modulate the orientation of turbulent flows within the Taurus molecular cloud using spatial gradients of thin velocity slices of 12CO and 13CO antenna temperatures. Our analysis accounts for the random errors of the gradients that arise from the thermal noise of the spectra. The orientations of the vectors normal to the antenna temperature gradient vectors are compared to the magnetic field orientations that are calculated from Planck 353~GHz polarization data. These relative orientations are parameterized with the projected Rayleigh statistic and mean resultant vector. For 12CO, 28 percent and 39 percent of the cloud area exhibit strongly parallel or strongly perpendicular relative orientations respectively. For the lower opacity 13CO emission, strongly parallel and strongly perpendicular orientations are found in 7 percent and 43 percent of the cloud area respectively. For both isotopologues, strongly parallel or perpendicular alignments are restricted to localized regions with low levels of turbulence. If the relative orientations serve as an observational proxy to the Alfvenic Mach number then our results imply local variations of the Alfvenic Mach number throughout the cloud.
