论文标题
磁盘星系中的星形形成及其与数值模拟中螺旋结构的关系
Star formation in disk galaxies and its relation with spiral structure in numerical simulations
论文作者
论文摘要
螺旋星系的螺旋结构可以通过不同的观察示踪剂，例如星际介质中的灰尘，离子化区域中的自由电子，分子气或Hα区域的原子氢。在这项工作中，我们使用具有磁性水力动力学（MHD）的N体模拟研究磁盘星系气体成分中的螺旋模式和恒星形成活性。我们解决的一些问题包括：如何通过气体的不同特性观察到星系？当我们使用气体的不同特性跟踪银河系的螺旋结构会发生变化吗？模拟中的螺旋臂是否会根据我们“看”的属性改变其形状和宽度？我们可以以某种方式对胳膊的形状进行建模以始终如一地测量其宽度吗？该模型适用于所有属性吗？为了回答这些问题，我们开发了一种磁盘星系中螺旋结构的识别和提取的方法。使用此过程的结果，我们通过气体的不同特性进一步研究了螺旋模式的特征，并特别注意恒星形成活动及其沿螺旋结构的行为。
The spiral structure of a spiral galaxy can be seen through different observational tracers such as the dust in the interstellar medium, the free electrons in ionized regions, the molecular gas, or the atomic hydrogen in Hα regions. In this work, we use an N-body simulation with Magnetohydrodynamics (MHD) to investigate the spiral pattern and the star formation activity in the gas component of a disk galaxy. Some of the questions that we tackle include: how are galaxies observed through the different properties of the gas? Does the spiral structure of the galaxy change when we trace it with the different properties of the gas? Do the spiral arms in the simulation change its shape and width depending on what property we are "looking" through? Can we somehow model the shape of the arms to measure their width consistently? Does this model apply to all the properties? To answer these questions, we developed a method for the identification and extraction of the spiral structure in a disk galaxy. Using the results of this procedure, we further investigate the features of the spiral pattern through the different properties of the gas, with special attention to the star formation activity and how it behaves along and across the spiral structure.
