标题： 冰质行星内部的新视角：冰-岩混合物而非冰在岩石之上 显示英文标题

标题： A new perspective on interiors of ice-rich planets: Ice-rock mixture instead of ice on top of rock

摘要： 富含冰的行星形成于水冰线之外，因此预计会含有大量的冰。 高冰含量导致内部环境具有独特条件，在这种条件下，行星结构受冰与其他金属相互作用的影响。 我们应用了高压下冰与岩石相互作用的实验数据，并计算了质量范围从超级地球到海王星（5到15个地球质量）的富含冰的行星可能的内部结构热演化。 我们通过包括恒星辐射通量和包层质量损失的影响来模拟向内迁移对富含冰的行星内部的影响。 我们发现由于高压下的混溶性，在行星内部的大部分区域，冰和岩石预计会在数十亿年内保持混合状态。 我们还发现，如果未发生质量损失，迁移到不同距离的行星双胞胎的深层内部通常相似。 显著的质量损失会导致水从岩石表面分离，并出现少于行星质量百分之一的挥发性大气。 水/蒸汽大气的质量由冰与岩石的相互作用所限制。 我们得出结论，当行星内部存在大量冰时，行星结构可能与标准的岩石核心上覆盖一层水壳的分层结构有很大不同。 这种结构预计在靠近恒星和远离恒星的行星中都存在。 显示英文摘要

摘要： Ice-rich planets are formed exterior to the water ice-line and thus are expected to contain a substantial amount of ices. The high ice content leads to unique conditions in the interior, under which the structure of a planet is affected by ice interaction with other metals. We apply experimental data of ice-rock interaction at high pressure, and calculate detailed thermal evolution for possible interior configurations of ice-rich planets, in the mass range of super-Earth to Neptunes (5-15 Earth masses). We model the effect of migration inward on the ice-rich interior by including the influences of stellar flux and envelope mass loss. We find that ice and rock are expected to remain mixed, due to miscibility at high pressure, in substantial parts of the planetary interior for billions of years. We also find that the deep interior of planetary twins that have migrated to different distances from the star are usually similar, if no mass loss occurs. Significant mass loss results in separation of the water from the rock on the surface and emergence of a volatile atmosphere of less than 1 percent of the planet's mass. The mass of the atmosphere of water/steam is limited by the ice-rock interaction. We conclude that when ice is abundant in planetary interiors the planet structure may differ significantly from the standard layered structure of a water shell on top of a rocky core. Similar structure is expected in both close-in and further-out planets.