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arXiv 2109.00514astro-ph.GAnlin.CD
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生长恒星棒的轨道演化：垂直ILR区的棒支撑轨道

Orbit evolution in growing stellar bars: Bar-supporting orbits at the vertical ILR region

Thanos Manos, Charalampos Skokos, Panos Patsis

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19 pages, 19 figures, revised and accepted for publication version in MNRAS (minor change in the original title)
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摘要：

我们研究了旋转三维杆的内Lindblad共振区域的轨道形状的演化，其质量随时间增长。我们评估随时间变化的模型，在5陀螺仪期间，轨道的重要性，已知的初始条件发挥了重要作用，在支持花生状结构的自治系统。这些轨道是中心族的周期轨道（x1）和它的垂直扰动，它的标准三维分叉的轨道在区域（x1v1和x1v2），以及在其附近的轨道。这些轨道的规则或混沌特性的知识也是必不可少的，因为它使我们能够估计它们对旋转杆的支撑的贡献，更重要的是，使其成为可能的动力学机制。这是通过GALI2指数计算的。我们发现，存在于自治的情况下，轨道模式，坚持更长的时间在更大规模的酒吧模型，甚至更是这样的模型中，我们所采用的银河系潜力的中心椭球体组件变得相当微不足道。我们发现的花生支撑轨道，有一个定期或在大多数情况下，弱混沌字符。在某些情况下，自治模型中的轨道开始接近不稳定的周期轨道，当它的质量随时间增加时，它的行为是规则的，并支持杆。我们的非自治模型在某个时刻的轨道动力学近似，可以被认为是在那个时刻附近的相应冻结系统的近似。

英文摘要：

We investigate the evolution of orbital shapes at the Inner Lindblad Resonance region of a rotating three-dimensional bar, the mass of which is growing with time. We evaluate in time-dependent models, during a 5 Gyr period, the importance of orbits with initial conditions known to play a significant role in supporting peanut-like structures in autonomous systems. These orbits are the central family of periodic orbits (x1) and vertical perturbations of it, orbits of its standard three-dimensional bifurcations at the region (x1v1 and x1v2), as well as orbits in their neighbourhood. The knowledge of the regular or chaotic character of these orbits is essential as well, because it allows us to estimate their contribution to the support of a rotating bar and, more importantly, the dynamical mechanisms that make it possible. This is calculated by means of the GALI2 index. We find that orbital patterns existing in the autonomous case, persist for longer times in the more massive bar models, and even more so in a model in which the central spheroid component of our adopted galactic potential becomes rather insignificant. The peanut-supporting orbits which we find, have a regular or, in most cases, a weakly chaotic character. There are cases in which orbits starting close to unstable periodic orbits in an autonomous model behave as regular and support the bar when its mass increases with time. An approximation for the orbital dynamics of our non-autonomous models at a certain time, can be considered that of the corresponding frozen system around that time.

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