THE EVOLUTION AND INTERNAL STRUCTURE OF JUPITER AND SATURN WITH COMPOSITIONAL GRADIENTS
THE EVOLUTION AND INTERNAL STRUCTURE OF JUPITER AND SATURN WITH COMPOSITIONAL GRADIENTS
复制标题
具有成分梯度的木星和土星的演化和内部结构
DOI：
10.3847/0004-637x/829/2/118
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
A. Kovetz
中科院分区：
文献类型：
--
作者：
A. Vazan;R. Helled;M. Podolak;A. Kovetz
气态巨行星的内部结构可能比通常假设的具有绝热温度分布的核心-包层结构更复杂。不同的原始内部结构和不同的物理过程会导致成分分布不均匀。非均匀的内部结构对行星的热演化和最终结构有重要的影响。在本文中，我们提出了木星和土星的替代结构和演化模型，允许非绝热原始结构和重元素在这些行星演化过程中的对流混合。我们介绍了行星的演化，说明了不同的初始成分梯度，在土星的情况下，包括氦雨导致的富氦区域的形成。我们研究了对流组成梯度区域的稳定性，发现土星的氦壳保持稳定，不与包膜的其余部分混合。在其他情况下，对流混合了行星内部，尽管存在成分梯度，导致包膜中重元素的富集。我们证明了木星和土星的非绝热结构（和冷却历史）是可行的。在这种情况下，内部温度比标准绝热模型要高得多。我们的结论是，内部结构与行星的形成和演化历史直接相关。在解释即将到来的朱诺号和卡西尼号数据时，应该考虑木星和土星的这些不同的内部结构。
The internal structure of gas giant planets may be more complex than the commonly assumed core-envelope structure with an adiabatic temperature profile. Different primordial internal structures as well as various physical processes can lead to non-homogenous compositional distributions. A non-homogenous internal structure has a significant impact on the thermal evolution and final structure of the planets. In this paper, we present alternative structure and evolution models for Jupiter and Saturn allowing for non-adiabatic primordial structures and the mixing of heavy elements by convection as these planets evolve. We present the evolution of the planets accounting for various initial composition gradients, and in the case of Saturn, include the formation of a helium-rich region as a result of helium rain. We investigate the stability of regions with composition gradients against convection, and find that the helium shell in Saturn remains stable and does not mix with the rest of the envelope. In other cases, convection mixes the planetary interior despite the existence of compositional gradients, leading to the enrichment of the envelope with heavy elements. We show that non-adiabatic structures (and cooling histories) for both Jupiter and Saturn are feasible. The interior temperatures in that case are much higher than those for standard adiabatic models. We conclude that the internal structure is directly linked to the formation and evolution history of the planet. These alternative internal structures of Jupiter and Saturn should be considered when interpreting the upcoming Juno and Cassini data.
影响因子：
4.9
作者：
Nettelmann, N.;Becker, A.;Redmer, R.
通讯作者：
Redmer, R.
H/He 分层和土星的冷却行为
影响因子：
3.2
作者：
Püstow R;Nettelmann N;Lorenzen W;Redmer R.
通讯作者：
Redmer R.