TERRESTRIAL PLANET FORMATION DURING THE MIGRATION AND RESONANCE CROSSINGS OF THE GIANT PLANETS
TERRESTRIAL PLANET FORMATION DURING THE MIGRATION AND RESONANCE CROSSINGS OF THE GIANT PLANETS
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DOI：
10.1088/0004-637x/773/1/65
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发表时间：
2013-06
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影响因子：
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通讯作者：
P. S. Lykawka;Takashi Ito
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文献类型：
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作者：
P. S. Lykawka;Takashi Ito
新形成的巨行星可能在较小的物体（胚胎）吸积形成行星盘中的类地行星时迁移并越过了若干互平均运动共振（MMRs）。通过n体模拟，首次研究了木星和土星的星子驱动迁移的影响，以及它们相互1:2 MMR交叉对类地行星形成的影响。这些模拟考虑了MMR穿越和行星迁移的不同时间尺度。总共进行了68次高分辨率模拟，使用了2000个盘状星子，这比以前发表的结果有了显著的改进。即使将1:2 MMR交叉和行星迁移的影响考虑在内，金星和地球的类似物（考虑轨道和质量）也在几次运行中成功形成。此外，我们发现，在行星迁移期间，木星和土星更偏心的轨道（相对于今天）所带来的增强的横扫长期共振，使超过1.5-2 AU的星子轨道动态耗尽。然而，这种消耗并没有阻止大质量火星类似物（质量超过火星1.5倍的行星）的形成。虽然后期的MMR交叉（在100 - 30迈珥）可以移除这样的行星，但类似火星的小质量行星在过度激发态的轨道（高e和/或i）上存活下来，或者在这些系统中完全消失。我们得出结论，木星和土星的轨道迁移和互1:2 MMR的交叉不太可能为太阳系类地行星的形成提供合适的轨道条件。这表明，为了解释火星的小质量和火星和木星之间没有其他行星，外层小行星带一定是由于与木星/土星的相互作用而遭受了严重的枯竭，或者是另一种机制（例如，流氓超级地球）。
The newly formed giant planets may have migrated and crossed a number of mutual mean motion resonances (MMRs) when smaller objects (embryos) were accreting to form the terrestrial planets in the planetesimal disk. We investigated the effects of the planetesimal-driven migration of Jupiter and Saturn, and the influence of their mutual 1:2 MMR crossing on terrestrial planet formation for the first time, by performing N-body simulations. These simulations considered distinct timescales of MMR crossing and planet migration. In total, 68 high-resolution simulation runs using 2000 disk planetesimals were performed, which was a significant improvement on previously published results. Even when the effects of the 1:2 MMR crossing and planet migration were included in the system, Venus and Earth analogs (considering both orbits and masses) successfully formed in several runs. In addition, we found that the orbits of planetesimals beyond a ∼ 1.5–2 AU were dynamically depleted by the strengthened sweeping secular resonances associated with Jupiter's and Saturn's more eccentric orbits (relative to the present day) during planet migration. However, this depletion did not prevent the formation of massive Mars analogs (planets with more than 1.5 times Mars's mass). Although late MMR crossings (at t > 30 Myr) could remove such planets, Mars-like small mass planets survived on overly excited orbits (high e and/or i), or were completely lost in these systems. We conclude that the orbital migration and crossing of the mutual 1:2 MMR of Jupiter and Saturn are unlikely to provide suitable orbital conditions for the formation of solar system terrestrial planets. This suggests that to explain Mars's small mass and the absence of other planets between Mars and Jupiter, the outer asteroid belt must have suffered a severe depletion due to interactions with Jupiter/Saturn, or by an alternative mechanism (e.g., rogue super-Earths).