Modeling of magnetized star forming cores and gravitational lenses

磁化恒星形成核心和引力透镜的建模

• 批准号: 312217-2012
• 负责人: Fiege, Jason
• 金额: $ 1.46万
• 依托单位: University of Manitoba
• 依托单位国家: 加拿大
• 项目类别: Discovery Grants Program - Individual
• 财政年份: 2013
• 资助国家: 加拿大
• 起止时间: 2013-01-01 至 2014-12-31
• 项目状态: 已结题
• 来源: https://www.nserc-crsng.gc.ca/ase-oro/Details-Detailles_eng.asp?id=526440
• 关键词: Modeling; magnetized; star; forming; cores

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.

这项研究的主要组成部分将模拟恒星形成分子云核心和细丝中的磁场几何形状和双极外流。我们将开发一种新的多目标方法来模拟亚毫米极化图，通过建立磁化核心的参数化模型，模拟极化图，并同时拟合强度，极化角和极化分数的地图。我们将把这些模型应用于JCMT档案中的核心和灯丝的极化图（由马修斯等人重新简化，2009年，ApJS，182，143），并扩展到包括一种新型的非参数模型，它将表征复杂和/或湍流区域中的磁场。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外流的几何模型，我们将能够建立第一个全球性的恒星形成区域的模型，约束外流的几何形状和它们的方向相对于核心的磁场。我们将把我们的方法应用于新的JCMT数据从古尔德的皮带调查，因为它变得可用。这项研究的预期成果将包括：1）对已充分研究的恒星形成区的磁场进行最佳表征; 2）第一个全球性的磁场和外流模型，它将限制外流相对于核心磁场的方向; 3）更完整地理解极化模型中的数学简并; 4）提高了对恒星形成区域中湍流磁场与有序磁场作用的理解。