论文标题
巨型气态团块的迁移和外太阳系的结构
Migration of giant gaseous clumps and structure of the outer Solar system
论文作者
论文摘要
关于远型河形对象和彗星特性的分布的新数据表明，在原球磁盘外部的外部，动力学过程的重要性在太阳系的观察到的结构形成中。在本文中，我们研究了由于引力不稳定性和间隔磁盘的碎裂，对外太阳系中小体群体的轨道分布而导致的巨型气态团块的可能作用。基本上，我们研究了Vorobyov和Elbakyan（2018）以前发现的巨型团块的迁移和重力相互作用的特征。我们的建模表明，由巨型团块的重力影响产生的小物体分布的主要特征与观察到的远跨北极物体的轨道分布一致。与单个巨型团块相关的研究动态过程是非常短的事件（不超过数十万年）。影响小物体轨道分布的主要因素是与巨大团块的紧密相遇。小体（彗星）的很大一部分很快被转移到具有较大偏心率的远处轨道上，这使他们可以避免相互碰撞。
New data on the distribution of distant trans-Neptunian objects and on the properties of comets indicate the importance of dynamical processes in the outer part of the protoplanetary disk in the formation of the observed structure of the Solar system. In this paper, we examined the possible action of giant gaseous clumps, resulting from gravitational instability and fragmentation of circumstellar disks, on the orbital distribution of the population of small bodies in the outer Solar system. Basically, we studied those features of migration and gravitational interaction of giant clumps that were found previously by Vorobyov and Elbakyan (2018). Our modeling showed that the main features of the distribution of small bodies resulting from the gravitational influence of giant clumps are consistent with the observed orbital distribution of distant trans-Neptunian objects. The studied dynamical process associated with a single giant clump is very short-time event (no more than several tens of thousands of years). The main factor affecting the orbital distribution of small bodies is close encounters with giant clumps. A significant part of small bodies (comets) is very quickly transferred to distant orbits with large eccentricities, which allows them to avoid mutual collisions.
