标题： 冰-rich行星内部的新视角：冰-岩混合物而非分层结构 显示英文标题

标题： A new perspective on interiors of ice-rich planets: Ice-rock mixture rather than a layered structure

摘要： 富含冰的行星形成于冰线之外，因此预计会含有大量的冰（挥发物）。 高含量的冰会导致内部出现独特的条件，在这种条件下，行星的结构可能受到冰与其他金属相互作用的影响。 我们使用高压下冰-岩相互作用的实验数据，并计算了富含冰行星可能内部结构的详细热演化过程。 我们通过包括恒星辐射通量和包层质量损失的影响，模拟了向内迁移对富含冰内部的影响。 我们发现，由于高压下的互溶性，岩石和冰在大多数行星内部（质量超过99%）预计将保持混合状态，适用于广泛的行星质量。 我们还发现，如果未发生质量损失，迁移至不同距离恒星的行星双星的深部内部通常相似。 显著的质量损失会导致由混合冰和岩石球体组成的内部结构，周围是质量小于行星1%的挥发性大气层。 在这种情况下，水/蒸汽大气的质量受到冰-岩相互作用的限制。 我们得出结论，当行星内部冰丰富时，冰和岩石在十亿年内倾向于保持混合，其内部结构不同于通常假设的简单分层结构。 这一发现可能对行星的观测特性产生重大影响，应在系外行星特征分析中加以考虑。 显示英文摘要

摘要： Ice-rich planets formed exterior to the iceline and thus are expected to contain substantial amount of ice (volatiles). The high ice content leads to unique conditions in the interior, under which the structure of a planet may be affected by ice interaction with other metals. We use experimental data of ice-rock interaction at high pressure, and calculate detailed thermal evolution for possible interior configurations of ice-rich planets. 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 rock and ice are expected to remain mixed, due to miscibility at high pressure, in most of the planet interior (>99% in mass) for a wide range of planetary masses. 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 an interior structure of a mixed ice and rock ball, surrounded by a volatile atmosphere of less than 1% of the planet's mass. In this case, 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 ice and rock tend to stay mixed for giga-years, and the interior structure differs from the simple layered structure that is usually assumed. This finding could have significant consequences on planets' observed properties, and it should be considered in exoplanets characterisation.