Dynamically produced moving groups in interacting simulations
Dynamically produced moving groups in interacting simulations
复制标题
DOI：
10.1093/mnras/stab1431
复制
发表时间：
2019-11
期刊：
影响因子：
--
通讯作者：
P. Craig;S. Chakrabarti;H. Newberg;A. Quillen
中科院分区：
文献类型：
--
作者：
P. Craig;S. Chakrabarti;H. Newberg;A. Quillen
我们表明，平滑粒子流体动力学（SPH）模拟的矮星系与银河系般的磁盘相互作用产生移动的群体在模拟的恒星盘。我们比较了所观察到的磁盘移动集团在太阳附近的速度扰动产生的SPH模拟有和没有矮星系的相互作用。我们的模拟包括三种不同的情况：一种情况包括三个卫星-具有人马座状矮星系相互作用，以及大麦哲伦云和小麦哲伦云;另一种情况是在银河系平面内运行，以及零情况，即，一个没有矮星系相互作用的星系速度子结构的识别使用的算法来识别移动组的基础上在磁盘的平面中的速度过密度。随着相互作用模拟的发展，所识别的移动组的属性发生变化。相对于我们分析过的孤立模拟，在相互作用模拟中形成的移动群体的数量和分布有明显的差异。我们的分析表明，银河系中的一些移动群体可能是由于与扰动矮卫星的动力学相互作用而形成的。
We show that Smoothed Particle Hydrodynamics (SPH) simulations of dwarf galaxies interacting with a Milky Way-like disk produce moving groups in the simulated stellar disk. We compare the observed disk moving groups in the Solar neighborhood with velocity perturbations produced in SPH simulations with and without dwarf galaxy interactions. Our simulations include three different cases: one that includes three satellites -- with a Sagittarius-like dwarf galaxy interaction, as well as the Large and Small Magellanic Clouds; another that orbits in the plane of the Milky Way, and a null case, i.e., one with no dwarf galaxy interaction. The velocity sub-structures are identified using an algorithm to identify moving groups based on velocity over-densities in the plane of the disk. The properties of the identified moving groups change as the interacting simulations evolve. There are clear differences in the number and distribution of moving groups formed in the interacting simulations relative to the isolated simulation that we have analyzed. Our analysis suggests that some of the moving groups in the Milky Way may have formed due to dynamical interactions with perturbing dwarf satellites.