论文标题
在光盘腔中重新访问迁移，以解释温暖的木星的高偏心率
Revisiting migration in a disc cavity to explain the high eccentricities of warm Jupiters
论文作者
论文摘要
热巨人系外行星的偏心率的分布通常是通过行星 - 行星相互作用来解释的，尽管没有身体上的论点有利于这种相互作用的无处不在。没有提出简单的通用解释来解释这些行星的高平均偏心率。在本文中，我们重新审视了一个简单，合理的解释，以说明温暖的木星的怪异：在原球盘中的腔内迁移。这种情况允许激发外偏共振，这是一种用于较高质量行星的工作机制，导致偏心率的增长，同时阻止其他偏离潮湿的偏心性。我们通过不同的数值模拟来测试这个想法，这表明围绕太阳恒星围绕木星质量行星的偏心率可以增加到0.4，这是从完全没有行星 - 碟片相互作用来实现的值。这种高的偏心率与温暖土星至木星质量系外行星的中位偏心率相当。我们还讨论了这种机制对系外行星观测的影响。这种情况可能会对圆盘寿命和内圆盘散布的物理产生强烈的后果，这可能会受到气体巨头的偏心分布的约束。
The distribution of eccentricities of warm giant exoplanets is commonly explained through planet--planet interactions, although no physically sound argument favours the ubiquity of such interactions. No simple, generic explanation has been put forward to explain the high mean eccentricity of these planets. In this paper, we revisit a simple, plausible explanation to account for the eccentricities of warm Jupiters: migration inside a cavity in the protoplanetary disc. Such a scenario allows to excite the outer eccentric resonances, a working mechanism for higher mass planets, leading to a growth in the eccentricity while preventing other, closer resonances to damp eccentricity. We test this idea with diverse numerical simulations, which show that the eccentricity of a Jupiter-mass planet around a Sun-like star can increase up to 0.4, a value never reached before with solely planet--disc interactions. This high eccentricity is comparable to, if not larger than, the median eccentricity of warm Saturn- to Jupiter-mass exoplanets. We also discuss the effects such a mechanism would have on exoplanet observations. This scenario could have strong consequences on the discs lifetime and the physics of inner disc dispersal, which could be constrained by the eccentricity distribution of gas giants.
