Thermodynamic data on the formation of solid carbon and organic compounds in primitive planetary atmospheres
Thermodynamic data on the formation of solid carbon and organic compounds in primitive planetary atmospheres
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原始行星大气中固体碳和有机化合物形成的热力学数据
DOI：
10.1029/jz067i005p02029
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发表时间：
1962
影响因子：
--
通讯作者：
H. Suess
中科院分区：
文献类型：
--
作者：
H. Suess
类地行星的大气层失去了原来存在的氢，这些氢是由CH4、CH3和H2O光解产生的。随着氧化条件的增加，气体可能会经过元素碳和各种有机化合物在热力学上保持稳定的阶段。H_2、CH_4、CO、CO和H_2O作为总H的函数的平衡浓度的数值计算是困难的，但Arnold Bainbridge已经在La Jolla CDC-1604计算机上对不同的温度、压力和碳氧比进行了计算。结果表明，在足够低的温度和足够高的碳氧比下，元素碳在热力学上是稳定的。金星表面的岩石似乎比地球上的岩石含有更多的碳。这可以解释为什么金星上存在大量二氧化碳，却没有氧气。
Atmospheres of terrestrial planets lose the hydrogen originally present and produced by photolysis of CH4, CH3, and H2O. With increasingly oxidizing conditions the gases may pass through a phase during which elementary carbon and various organic compounds are thermodynamically stable. Numerical calculation of the equilibrium concentrations of H2, CH4, CO, CO2, and H2O as a function of total H is difficult, but it has been carried out by Arnold Bainbridge on the La Jolla CDC-1604 computer for various temperatures, pressures, and carbon/oxygen ratios. The results show that at sufficiently low temperatures and sufficiently high carbon/oxygen ratios a range of total H will exist at which elementary carbon is thermodynamically stable. It seems possible that the surface rocks of Venus contain much more carbon than those of the earth. This would explain the presence of large amounts of CO2 and the absence of oxygen on Venus.