关于特洛伊行星的增长和稳定性
On the growth and stability of Trojan planets
摘要：
我们研究了那些低质量特洛伊行星的稳定性，这些行星形成于原行星盘中，随后吸积气体成为气体巨星。我们计算它们的演化之前，期间和之后的气体盘分散。一个二维流体动力学代码结合N体求解器是用来发展系统的磁盘和行星。气盘扩散模拟在一个简单的方式，通过假设全球指数衰减的光盘质量，导致停滞的迁移后，半长轴已约从其初始值的一半。我们考虑特洛伊对不同的初始质量和气体吸积率和不同的质量和粘度的气体盘模型。一个N-体代码，适用于模拟磁盘的力量，是用来检查大规模的迁移和形成非常短的周期特洛伊行星。对于我们在流体动力学模拟中考虑的行星对和圆盘模型的每种组合，每个特洛伊系统在圆盘分散之前、期间和之后保持稳定。在没有气体的情况下，这些系统的长期稳定性使用N体模拟进行了测试，所有系统在等于10^9年的演化时间内保持稳定。在所有情况下，偏心率都很低（e<0.02）。L4/L5拉格朗日点的天平动幅度的增加伴随着向内的迁移，在非常大规模的迁移特洛伊系统可能会被破坏之前，光盘分散的发病。特洛伊对的稳定性在快速的I型迁移，在过渡到II型迁移与伴随的间隙形成的气体盘，并在气体损失时，光盘分散，表明孤立的特洛伊行星系统是非常稳定的。如果它们的形成存在一个共同的机制，我们认为它们可以很容易地在自然界中观察到。
英文摘要：
We investigate the stability of those low-mass Trojan planets that form in a protoplanetary disc and subsequently accrete gas to become gas giants. We calculate their evolution before, during, and after gas disc dispersal. A two-dimensional hydrodynamics code combined with an N-body solver is used to evolve the system of disc and planets. Gas disc dispersal is simulated in a simple manner by assuming global exponential decay of the disc mass, leading to the stalling of migration after semi-major axes have approximately halved from their initial values. We consider Trojan pairs with different initial masses and gas accretion rates and gas disc models with different masses and viscosities. An N-body code, adapted to model disc forces, is used to examine large-scale migration and the formation of very short period Trojan planets. For each combination of planetary pair and disc model that we consider in our hydrodynamic simulations, each Trojan system remains stable before, during, and after disc dispersal. The long-term stability of these systems in the absence of gas is tested using N-body simulations, and all systems remain stable for those evolution times equal to 10^9 years. Eccentricities remain low (e<0.02) in all cases. Increases in the amplitude of libration about the L4/L5 Lagrange points accompany the inward migration, and during very large-scale migration Trojan systems may be disrupted prior to the onset of disc dispersal. The stability of Trojan pairs during rapid type I migration, during the transition to type II migration with the accompanying gap formation in the gas disc, and during gas loss when the disc disperses, indicates that isolated Trojan planet systems are very stable. If a common mechanism exists for their formation, we suggest they may be readily observed in nature.
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。
