ARE THE KEPLER NEAR-RESONANCE PLANET PAIRS DUE TO TIDAL DISSIPATION?
ARE THE KEPLER NEAR-RESONANCE PLANET PAIRS DUE TO TIDAL DISSIPATION?
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DOI：
10.1088/0004-637x/774/1/52
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发表时间：
2013-07
期刊：
影响因子：
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通讯作者：
M. Lee;D. Fabrycky;D. Fabrycky;D. Lin;D. Lin
中科院分区：
文献类型：
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作者：
M. Lee;D. Fabrycky;D. Fabrycky;D. Lin;D. Lin
开普勒使命发现的多行星系统显示出过多的行星对，它们的周期比刚好与2：1和3：2等一阶共振的精确可分辨性相差甚远。原则上，如果轨道偏心率足够小，这些行星对可以有与共振振动相关的两个共振角，因为一阶共振的宽度在极小的偏心率的极限下发散。我们认为一个广泛举行的情况下，对行星被捕获到一阶共振迁移由于行星盘的相互作用，随后成为脱离共振，由于潮汐耗散的行星。在这种情况下，我们发现一个约束的比例，行星的潮汐耗散函数和勒夫数，这意味着一些开普勒行星可能是固体。然而，潮汐不足以将许多行星对移动到观测到的分离位置，这表明还有其他耗散过程在起作用。
The multiple-planet systems discovered by the Kepler mission show an excess of planet pairs with period ratios just wide of exact commensurability for first-order resonances like 2:1 and 3:2. In principle, these planet pairs could have both resonance angles associated with the resonance librating if the orbital eccentricities are sufficiently small, because the width of first-order resonances diverges in the limit of vanishingly small eccentricity. We consider a widely held scenario in which pairs of planets were captured into first-order resonances by migration due to planet–disk interactions, and subsequently became detached from the resonances, due to tidal dissipation in the planets. In the context of this scenario, we find a constraint on the ratio of the planet's tidal dissipation function and Love number that implies that some of the Kepler planets are likely solid. However, tides are not strong enough to move many of the planet pairs to the observed separations, suggesting that additional dissipative processes are at play.