A Secular Resonant Origin for the Loneliness of Hot Jupiters
A Secular Resonant Origin for the Loneliness of Hot Jupiters
复制标题
热木星孤独的长期共振起源
DOI：
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发表时间：
2017
期刊：
影响因子：
--
通讯作者：
K. Batygin
中科院分区：
文献类型：
--
作者：
C. Spalding;K. Batygin
尽管进行了几十年的调查，但位于天文单位十分之几范围内的巨型行星的起源仍然不清楚。传统上，这些物体被认为是在随后向内迁移之前形成的。然而，随着近距离巨行星的原地形成模型的出现，迁移的必要性最近受到了质疑。对近距离巨星凌日亚样本的观测特征表明，轨道周期长于大约10天的“暖”木星比周期较短的“热”木星更容易拥有近距离的、共同凌日的行星伴侣，后者通常是孤独的。这一发现此前被解释为证据表明，平稳的早期迁移或原地形成导致了温暖的木星托管系统，而更猛烈的盘后迁移路径塑造了炎热的木星托管系统。在这项工作中，我们证明了这两类行星都可能是通过早期迁移或原位聚集而产生的，但热木星的孤独感增强是由于与恒星四极矩的长期共振相互作用造成的。这种相互作用会倾斜外部较小质量行星的轨道，将它们从探测到高温木星的凌日观测中剔除。相比之下，温暖的木星宿主系统由于宿主恒星的四极势相对于行星-圆盘相互作用的影响较弱，所以保持了它们的共面性。通过这种方式，热木星和暖木星被置于一个统一的理论框架中，该框架可以很容易地利用即将到来的任务(如TESS)的数据来验证或证伪。
Despite decades of inquiry, the origin of giant planets residing within a few tenths of an astronomical unit from their host stars remains unclear. Traditionally, these objects are thought to have formed further out before subsequently migrating inwards. However, the necessity of migration has been recently called into question with the emergence of in situ formation models of close-in giant planets. Observational characterization of the transiting subsample of close-in giants has revealed that “warm” Jupiters, possessing orbital periods longer than roughly 10 days more often possess close-in, co-transiting planetary companions than shorter period “hot” Jupiters, that are usually lonely. This finding has previously been interpreted as evidence that smooth, early migration or in situ formation gave rise to warm Jupiter-hosting systems, whereas more violent, post-disk migration pathways sculpted hot Jupiter-hosting systems. In this work, we demonstrate that both classes of planet may arise via early migration or in situ conglomeration, but that the enhanced loneliness of hot Jupiters arises due to a secular resonant interaction with the stellar quadrupole moment. Such an interaction tilts the orbits of exterior, lower-mass planets, removing them from transit surveys where the hot Jupiter is detected. Warm Jupiter-hosting systems, in contrast, retain their coplanarity due to the weaker influence of the host star’s quadrupolar potential relative to planet–disk interactions. In this way, hot Jupiters and warm Jupiters are placed within a unified theoretical framework that may be readily validated or falsified using data from upcoming missions, such as TESS.
DOI：
10.1146/annurev-astro-081811-125523
发表时间：
2012-03
影响因子：
33.3
作者：
W. Kley;R. Nelson
通讯作者：
W. Kley;R. Nelson