Dynamic portrait of the planetary 2/1 mean‐motion resonance – II. Systems with a more massive inner planet
Dynamic portrait of the planetary 2/1 mean‐motion resonance – II. Systems with a more massive inner planet
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DOI：
10.1111/j.1365-2966.2008.13867.x
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发表时间：
2008-11
影响因子：
4.8
通讯作者：
T. Michtchenko;C. Beaugé;S. Ferraz-Mello
中科院分区：
文献类型：
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作者：
T. Michtchenko;C. Beaugé;S. Ferraz-Mello
我们分析的全球结构的平面行星2/1平均运动共振的情况下，外行星是更大的质量比它的内同伴的相空间。在共振域内，我们证明了存在两族周期轨道，一个与共振角的平动有关（σ族），另一个与近心点差的循环运动有关（β族）.众所周知的拱点共转共振（ACR）表现为两个族之间的交叉点。一个复杂的网络的二次共振也检测到低偏心率，其强度和位置取决于个人的质量和空间尺度的系统。动态地图的建设为各种值的总角动量的稳定运动的偏心率，确定可能的配置适合于系外行星系统的家庭的演变。对于中低偏心率，ACR外存在几种不同的稳定模式。然而，对于较大的偏心率，所有稳定的解决方案都与振荡周围的固定解决方案。最后，我们提出了这些稳定的家庭和共振捕获的过程之间的可能联系，确定最可能的路线从长期区域的共振域，并讨论如何最终的共振配置可能会受到影响的混沌层周围的共振区域的扩展。
We analyse the global structure of the phase space of the planar planetary 2/1 mean-motion resonance in cases where the outer planet is more massive than its inner companion. Inside the resonant domain, we show the existence of two families of periodic orbits, one associated to the librational motion of resonant angle (σ -family) and the other related to the circulatory motion of the difference in longitudes of pericentre (�� -family). The well-known apsidal corotation resonances (ACR) appear as intersections between both families. A complex web of secondary resonances is also detected for low eccentricities, whose strengths and positions are dependent on the individual masses and spatial scale of the system. The construction of dynamical maps for various values of the total angular momentum shows the evolution of the families of stable motion with the eccentricities, identifying possible configurations suitable for exoplanetary systems. For low‐moderate eccentricities, several different stable modes exist outside the ACR. For larger eccentricities, however, all stable solutions are associated to oscillations around the stationary solutions. Finally, we present a possible link between these stable families and the process of resonance capture, identifying the most probable routes from the secular region to the resonant domain, and discussing how the final resonant configuration may be affected by the extension of the chaotic layer around the resonance region.