Modeling of magnetized star forming cores and gravitational lenses

这项研究的主要组成部分将模拟磁场几何形状和形成恒星的分子云核心和细丝中的双极流出。我们将开发一种新的多目标方法，通过建立磁化磁芯的参数化模型，模拟极化图，同时拟合强度图、极化角图和极化分数图来模拟亚毫米极化图。我们将把这些模型应用到JCMT档案（由Matthews等人重新简化，2009,ApJS, 182, 143）的磁芯和细丝的极化图中，并扩展到包括一种新的非参数模型，该模型将表征复杂和/或湍流区域的磁场。此外，我们还计划修改现有的软件来模拟CO排放，以模拟双极流出。通过指定一个简单的双极流出的几何模型，我们将能够建立第一个恒星形成区域的全球模型，该模型约束了流出的几何形状及其相对于核心磁场的方向。我们将把我们的方法应用于来自古尔德带调查的新的JCMT数据，因为它变得可用。本研究的预期结果将包括：1)在研究充分的恒星形成区域中获得最佳的磁场表征；2)第一个磁场和外流的全球模型，该模型将约束相对于地核磁场的外流方向；3)对极化模型的数学简并性有了更全面的认识；4)提高了对恒星形成区域中湍流磁场与有序磁场的作用的理解。

The dominant component of this research will model magnetic field geometries and bipolar outflows in star-forming molecular cloud cores and filaments. We will develop a new multi-objective method to model submillimetre polarization maps by building a parametrized model of a magnetized core, simulating the polarization map, and simultaneously fitting to maps of intensity, polarization angles, and polarization fraction. We will apply these models to polarization maps of cores and filaments from the JCMT archive (re-reduced by Matthews et al. 2009, ApJS, 182, 143), and extended to include a new type of non-parametric model, which will characterize magnetic fields in complicated and/or turbulent regions. In addition, we also plan to modify existing software to model CO emission to model bipolar outflows. By specifying a simple geometric model of bipolar outflows, we will be able to build the first global models of star-forming regions that constrain outflow geometries and their orientations with respect to the core's magnetic field. We will apply our method to new JCMT data from the Gould's Belt Survey as it becomes available. The anticipated outcome of this research will include: 1) The best available characterization of magnetic fields in well studied star-forming regions; 2) The first global models of fields and outflows, which will constrain the direction of outflows relative to core magnetic fields; 3) More complete understanding of mathematical degeneracy in polarization models; and 4) Improved understanding of the roles of turbulent vs. orderly magnetic fields in star-forming regions.