Recent planetary data and geophysical modeling suggest that hydrothermal activity is ongoing under the ice crust of Enceladus, one of Saturn's moons. According to these models, hydrothermal flow in the porous, rocky core of the satellite is driven by tidal deformation that induces dissipation and volumetric internal heating. Despite the effort in the modeling of Enceladus' interior, systematic understanding—and even basic scaling laws—of internally heated porous convection and hydrothermal activity are still lacking. In this article, using an idealized model of an internally heated porous medium, we explore numerically and theoretically the flows that develop close to and far from the onset of convection. In particular, we quantify heat‐transport efficiency by convective flows as well as the typical extent and intensity of heat flux anomalies created at the top of the porous layer. With our idealized model, we derive simple and general laws governing the temperature and hydrothermal velocity that can be driven in the oceans of icy moons. In the future, these laws could help better constraining models of the interior of Enceladus and other icy satellites.

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内热多孔对流：土卫二水热活动的理想模型

最近的行星数据和地球物理模拟表明，土星卫星之一的土卫二的冰壳下正在进行热液活动。根据这些模型，卫星多孔岩心中的热液流是由潮汐变形驱动的，潮汐变形引起耗散和内部体积加热。尽管对土卫二内部进行了建模工作，但仍然缺乏对内部加热的多孔对流和热液活动的系统理解，甚至是基本的比例定律。在本文中，我们使用内部加热的多孔介质的理想化模型，在数值和理论上探索了对流发生时接近和远离对流的流量。尤其是，我们通过对流以及在多孔层顶部产生的热通量异常的典型程度和强度来量化传热效率。利用我们的理想模型，我们得出了可控制冰月卫星海洋中温度和热液速度的简单且通用的定律。将来，这些法律将有助于更好地约束土卫二和其他冰冷卫星的内部模型。