论文标题
K2-19系统中的共鸣与报告的偏心率很高
Resonance in the K2-19 system is at odds with its high reported eccentricities
论文作者
论文摘要
K2-19拥有一个由两个外行星B和C组成的行星系统，大小为$ 7.0 \ pm 0.2〜r_ \ oplus $和$ 4.1 \ pm0.2〜r_ \ r_ \ oplus $，并且一个内心行星，D，半径为$ 1.11 \ pm 0.05 r_ \ oplus $。最近对传播变化（TTV）的最新分析表明，B和C在3：2平均运动共振（MMR）中却接近但不接近，因为经典的谐振角循环。这样的建筑挑战了我们对星球形成的理解。实际上，行星通过原星盘迁移应导致捕获到MMR中。在这里，我们表明，尽管传统的谐振角和对齐的围绕围绕围绕的循环循环，但实际上，行星实际上被锁定在3：2的共鸣中。但是，我们表明，由于行星d经历的潮汐耗散，这种轨道配置无法在数亿年内维护。由于行星B和C对世俗的强迫，潮汐耗散效率仍然有效。尽管观察结果强烈排除了三个行星在接近圆形轨道的轨道解，但仍然有可能第四行星影响TTV，以使四个行星系统与潮汐约束一致。
K2-19 hosts a planetary system composed of two outer planets, b and c, with size of $7.0\pm 0.2~R_\oplus$ and $4.1\pm0.2~R_\oplus$ , and an inner planet, d, with a radius of $1.11\pm 0.05 R_\oplus$. A recent analysis of Transit-Timing Variations (TTVs) suggested b and c are close to but not in 3:2 mean motion resonance (MMR) because the classical resonant angles circulate. Such an architecture challenges our understanding of planet formation. Indeed, planet migration through the protoplanetary disk should lead to a capture into the MMR. Here, we show that the planets are in fact, locked into the 3:2 resonance despite circulation of the conventional resonant angles and aligned periapses. However, we show that such an orbital configuration cannot be maintained for more than a few hundred million years due to the tidal dissipation experienced by planet d. The tidal dissipation remains efficient because of a secular forcing of the innermost planet eccentricity by planets b and c. While the observations strongly rule out an orbital solution where the three planets are on close to circular orbits, it remains possible that a fourth planet is affecting the TTVs such that the four planet system is consistent with the tidal constraints.
