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首页> 外文期刊>Icarus: International Journal of Solar System Studies >The role of atmospheric pressure on Mars surface properties and early Mars climate modeling
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The role of atmospheric pressure on Mars surface properties and early Mars climate modeling

机译：大气压对火星表面性能的作用和早期火星气候建模

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The thermal inertia of a planetary surface is a compound function of the regolith thermal conductivity, density and specific heat. On planetary bodies with atmospheres, the conductivity of the surface must account for the contributions of both the solid component of the surface as well as that of atmospheric gas found in the interstitial pore spaces. Today, variations in thermal inertia and thermal conductivity on Mars affect the size and timing of areas for which surface temperatures exceed the melting point temperature of water, which is a necessary-but-not-sufficient prerequisite for surface liquid water. Models of past Mars climate, when the atmosphere may have been significantly thicker than at present, have largely neglected the potential role of interstitial atmospheric gas as a thermally conducting element of the 'surface,' though we show here that such underestimation of surface conductivity and thermal inertia has no appreciable effect on models of past Mars climate. In more recent Mars history, changes in obliquity have a similar effect of inflating or collapsing the Mars atmosphere, though to a lesser extent. Orbital changes will also modify surface thermal properties, leading to variations in surface conductivity (and thermal inertia) on 10(5)-10(7) year cycles. We show that these variations, in fact, should not be neglected. We propose an obliquity-driven cycle of surface evolution that drives variability in surface thermal inertia, and suggest that the potential for liquid water at the surface should increase with time following large, positive excursions in Mars' obliquity.
机译：行星表面的热惯性是石油热导率，密度和特定热的复合功能。在具有大气的行星体上，表面的电导率必须考虑表面固体组分的贡献以及间质孔隙空间中发现的大气气体。如今，火星上热惯性和导热率的变化会影响表面温度超过水熔点温度的区域的尺寸和定时，这是表面液体水的必要但不足的先决条件。过去的模型气候，当大气可能比目前显着厚，大大忽略了间质大气气体作为“表面的导热元件”的潜在作用，尽管我们在这里显示了这种低估了表面电导率和热惯性对过去火星气候的模型没有明显的影响。在最近的MARS历史中，倾斜的变化具有相似的效果膨胀或坍塌的火星氛围，但在较小程度上。轨道变化也将改变表面热性质，导致表面电导率（和热惯性）的变化在10（5）-10（7）年周期上。我们表明这些变化实际上不应该被忽视。我们提出了一种表面演变的倾斜驱动循环，驱动表面热惯性的可变性，并表明表面在火星倾斜度的大而正偏移之后的时间随时间增加。

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