对于GJ 436 b的近扰情况，
The case for a close-in perturber to GJ 436 b
摘要：
凌日行星的数量越来越多，增加了发现其凌日时间、持续时间和深度变化的可能性，这些变化可能表明系统中还有其他行星。食双星的经验确实表明，这种变化是可以预料的。寻找扰动行星的第一个明显的候选者是GJ 436，它在偏心轨道上拥有一颗海王星质量的热凌日行星。Ribas等人（2008年）认为，这种偏心率和轨道倾角的可能变化可能是由于近距离轨道上的小行星扰动造成的。一个5M的地球行星的径向速度信号接近2：1的平均运动共振似乎提供了完美的候选人。最近新的径向速度被认为是这种信号的假。在这里，我们把所有可用的信息的背景下，我们评估的可能性，一个小扰动GJ 436 b解释其偏心率和可能的倾角变化。特别是，我们讨论了过境时间变化数据提供的约束。我们的结论是，考虑到目前的数据，近距离扰动的情况下仍然提供了一个合理的解释观测到的轨道和物理性质的GJ 436 b。
英文摘要：
The increasing number of transiting planets raises the possibility of finding changes in their transit time, duration and depth that could be indicative of further planets in the system. Experience from eclipsing binaries indeed shows that such changes may be expected. A first obvious candidate to look for a perturbing planet is GJ 436, which hosts a hot transiting Neptune-mass planet in an eccentric orbit. Ribas et al. (2008) suggested that such eccentricity and a possible change in the orbital inclination might be due to a perturbing small planet in a close-in orbit. A radial velocity signal of a 5 M_earth planet close to the 2:1 mean-motion resonance seemed to provide the perfect candidate. Recent new radial velocities have deemed such signal spurious. Here we put all the available information in context and we evaluate the possibility of a small perturber to GJ 436 b to explain its eccentricity and possible inclination change. In particular, we discuss the constraints provided by the transit time variation data. We conclude that, given the current data, the close-in perturber scenario still offers a plausible explanation to the observed orbital and physical properties of GJ 436 b.
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