K2-19系统中的共振与其报告的高偏心率不一致
Resonance in the K2-19 system is at odds with its high reported eccentricities
摘要：
K2-19拥有一个行星系，由两颗外行星b和c组成，大小分别为$7.0\pm 0.2~R_\oplus$和$4.1\pm0.2~R_\oplus$，还有一颗内行星d，半径为$1.11\pm 0.05 R_\oplus$。最近对渡越时间变化（TTV）的分析表明，b和c接近但不是3：2平均运动共振（MMR），因为经典共振角循环。这样的结构挑战了我们对行星形成的理解。事实上，行星通过原行星盘的迁移应该导致被MMR捕获。在这里，我们表明，行星实际上是锁定在3：2共振，尽管传统的共振角和对齐的近点的循环。然而，我们表明，这样的轨道配置不能维持超过数亿年，由于潮汐耗散经历的行星d。潮汐耗散仍然有效，因为行星b和c长期强迫最内侧的行星离心率。虽然观测结果强烈排除了三颗行星接近圆形轨道的轨道解，但仍然有可能是第四颗行星影响了TTV，使得四颗行星系统与潮汐约束一致。
英文摘要：
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.
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