御夫座轮的数值模拟-一个新的环形星系
Numerical modelling of Auriga's Wheel - a new ring galaxy
摘要：
我们模拟御夫座之轮的形成-最近发现的碰撞环星系。御夫座之轮有许多有趣的特征，包括一座恒星桥，连接邻近的椭圆星系和环形星系，以及环内膨胀和旋转成分的证据。利用N-body/SPH模型，我们研究了椭圆星系与晚型盘星系之间的碰撞。一个近直接碰撞，与一个温和的倾斜盘，被发现合理地再现一般系统形态？50百万年后的碰撞。碰撞必须有一个相对较低的速度（最初~150 km s^{-1}），以形成观察到的桥梁，同时匹配星系分离。我们的最佳匹配模型表明，总盘星系的质量是椭圆星系的5倍。我们发现环的膨胀速度对椭圆的质量敏感，而对相遇速度不敏感。我们将我们的模拟发展到当前时代之外，以研究星系对的未来命运。在我们的模型中，原子核朝着恒星桥的方向远离环平面。核心最终与椭圆星系合并~100百万年后的现在。环继续膨胀约2亿年，然后塌缩回来。两个星系的初始相对速度很低，最终将导致完全合并。
英文摘要：
We model the formation of Auriga's Wheel - a recently discovered collisional ring galaxy. Auriga's Wheel has a number of interesting features including a bridge of stars linking the neighbouring elliptical to the ring galaxy, and evidence for components of expansion and rotation within the ring. Using N-body/SPH modelling, we study collisions between an elliptical galaxy and a late-type disk galaxy. A near direct collision, with a mildy inclined disk, is found to reasonably reproduce the general system morphology ~50 Myr following the collision. The collision must have a relatively low velocity (initially ~150 km s^{-1}) in order to form the observed bridge, and simultaneously match the galaxies separation. Our best-match model suggests the total disk galaxy is ~5 times more massive than the elliptical. We find that the velocity of expansion of the ring is sensitive to the mass of the elliptical, while insensitive to the encounter velocity. We evolve our simulation beyond the current epoch to study the future destiny of the galaxy pair. In our model, the nucleus moves further away from the plane of the ring in the direction of the stellar bridge. The nucleus eventually merges with the elliptical galaxy ~100 Myr after the present time. The ring continues to expand for ~200 Myr before collapsing back. The low initial relative velocity of the two galaxies will eventually result in a complete merger.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
