论文标题
陆地行星形成的原始摩尔泥和原始拟南芥之间的极端紧密相遇
Extreme close encounters between proto-Mercury and proto-Venus in terrestrial planet formation
论文作者
论文摘要
陆地行星形成的现代模型需要固体在行星盘中耗尽内部至0.5-0.7 au，以解释少量汞。大约100个MYR碰撞生长后出现地球和金星类似物，而汞形成在地球磁盘的扩散尾部。我们进行了250张N体磁盘的N体模拟，其中质量局限于0.7-1.0 au，以研究近期提议的近距离相遇的统计数据，这些统计是邓（Deng）（2020年）的高铁质量分数的解释。我们在总计中形成了39个汞类似物，所有原始类似物均通过原始拟南芥向内散射。原始 - 库里通常会经历6种极端近距离遇到（最接近6个金星半径的方法），在原弱拟南芥获得了0.7金星质量后，原始拟南芥在这种紧密的分离下获得了0.7金星，潮汐相互作用已经可以显着影响轨道运动，因此N体治疗本身无效。如果轨道角动量的潮汐消散，预计会有更多和紧密的相遇。理想的杂交N体流体动力模拟自我一致地处理轨道和遭遇动力学，以评估原始碳酸盐的潮汐地幔剥离程度。
Modern models of terrestrial planet formation require solids depletion interior to 0.5-0.7 au in the planetesimal disk to explain the small mass of Mercury. Earth and Venus analogues emerge after ~100 Myr collisional growth while Mercury form in the diffusive tails of the planetesimal disk. We carried out 250 N-body simulations of planetesimal disks with mass confined to 0.7-1.0 au to study the statistics of close encounters which were recently proposed as an explanation for the high iron mass fraction in Mercury by Deng (2020). We formed 39 Mercury analogues in total and all proto-Mercury analogues were scattered inward by proto-Venus. Proto-Mercury typically experiences 6 extreme close encounters (closest approach smaller than 6 Venus radii) with Proto-Venus after Proto-Venus acquires 0.7 Venus Mass. At such close separation, the tidal interaction can already affect the orbital motion significantly such that the N-body treatment itself is invalid. More and closer encounters are expected should tidal dissipation of orbital angular momentum accounted. Hybrid N-body hydrodynamic simulations, treating orbital and encounter dynamics self-consistently, are desirable to evaluate the degree of tidal mantle stripping of proto-Mercury.
