Institute for Astronomy, University of Vienna, Vienna, Austria.
Astrobiology. 2010 Jan-Feb;10(1):33-43. doi: 10.1089/ast.2009.0379.
The problem of the stability of planetary systems, a question that concerns only multiplanetary systems that host at least two planets, is discussed. The problem of mean motion resonances is addressed prior to discussion of the dynamical structure of the more than 350 known planets. The difference with regard to our own Solar System with eight planets on low eccentricity is evident in that 60% of the known extrasolar planets have orbits with eccentricity e > 0.2. We theoretically highlight the studies concerning possible terrestrial planets in systems with a Jupiter-like planet. We emphasize that an orbit of a particular nature only will keep a planet within the habitable zone around a host star with respect to the semimajor axis and its eccentricity. In addition, some results are given for individual systems (e.g., Gl777A) with regard to the stability of orbits within habitable zones. We also review what is known about the orbits of planets in double-star systems around only one component (e.g., gamma Cephei) and around both stars (e.g., eclipsing binaries).
本文讨论了行星系统稳定性这一问题，该问题仅涉及至少包含两颗行星的多行星系统。在讨论超过 350 颗已知行星的动力学结构之前，先讨论了平均运动共振问题。与我们太阳系中只有八颗低偏心率行星的情况相比，明显的不同之处在于，已知的 60%系外行星的轨道偏心率 e>0.2。我们从理论上强调了对具有类木星行星的系统中可能存在的类地行星的研究。我们强调，只有特定性质的轨道才能使行星在相对于宿主恒星的半长轴及其偏心率的可居住区内保持稳定。此外，还针对个别系统（例如 Gl777A）给出了关于可居住区内轨道稳定性的一些结果。我们还回顾了关于双星系统中只有一颗恒星（例如，γ Cephei）和两颗恒星（例如，食双星）周围行星轨道的已知情况。
