The structure and evolution of Jupiter - The fluid contraction stage
The structure and evolution of Jupiter - The fluid contraction stage
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DOI：
10.1086/153689
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发表时间：
1975-07
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影响因子：
--
通讯作者：
H. Graboske;J. Pollack;A. Grossman;R. Olness
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文献类型：
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作者：
H. Graboske;J. Pollack;A. Grossman;R. Olness
用恒星结构方法对一个0.00095 M/太阳质量/星星，由对流、绝热、均匀流体组成的恒星进行了演化研究。一种新的数值技术被用来计算模式大气的时间平均垂直温度结构的形式，包括所有相关的不透明度源和太阳能沉积组件。利用最近的高压实验结果和新的理论方法，研究了纯氢和太阳混合物（X = 0.74，Y = 0.24，Z = 0.02）在-7 ≤ logrho（g cm$sup-3 $）≤ 1和1.78 ≤ logT（K）≤ 4.78时的热力学性质。由此产生的引力收缩演化模型表现出两个阶段。早期的恒星阶段，表现得像一个典型的低质量前主序星，具有高光度，在伽利略卫星的结构中留下了记录。这个阶段也有很高的内部温度，（T/sub c/）/sub max/达到51，400，这确保了作为一个完全混合的对流结构的长期后续演变。第二阶段是一个方法，以简并矮冷却曲线，这给出了很好的协议与观测到的半径和光度的木星。标准绝热流体模型（2.6 x 10$sup 9$年）的shortmore »时间尺度被影响行星演化的几个因素的组合所扩展。演化对化学成分、太阳能沉积、状态方程、模型大气和超绝热性的敏感性分析表明，状态方程和超绝热性对行星时间尺度的影响最大。（auth）«少
An evolutionary study of a 0.00095 M/solar mass/ star, composed of a convective, adiabatic, homogeneous fluid, has been performed using stellar structure methods. A new numerical technique is used to calculate model atmospheres in the form of time-average vertical temperature structures, including all relevant opacity sources and a solar energy deposition component. Thermodynamic properties for pure hydrogen and a solar mixture (X = 0.74, Y = 0.24, Z = 0.02) are developed for -7 less than or equal to log rho (g cm$sup -3$) less than or equal to 1 and 1.78 less than or equal to log T(K) less than or equal to 4.78, utilizing recent high-pressure experimental results and new theoretical methods. The resultant gravitationally contracting evolutionary models exhibit two phases. An early stellar phase, behaving like a typical low- mass pre-main-sequence object, has high luminosities which have left a record in the structure of the Galilean satellites. This phase also has high internal temperatures, (T/sub c/)/sub max/ reaching 51,400, which ensures a long subsequent evolution as a fully mixed, convective structure. The second phase is an approach to a degenerate dwarf cooling curve, which gives excellent agreement with the observed radius and luminosity of Jupiter. A shortmore » time scale for the standard adiabatic fluid models (2.6 x 10$sup 9$ years) is extended by combinations of several factors influencing the planetary evolution. An analysis of the sensitivity of evolution to chemical composition, solar energy deposition, equation of state, model atmospheres, and superadiabaticity demonstrates that equation of state and superadiabaticity have the strongest influence over planetary time scales. (auth)« less