低温气体不透明度-- AESOPUS：一种通用的快速计算工具
Low-temperature gas opacity - AESOPUS: a versatile and quick computational tool
摘要：
我们介绍了一个新的工具- AESOPUS：精确的状态方程和不透明度实用软件-用于计算状态方程和Rosseland平均（RM）不透明度的物质在理想气体相。结果是作为一对状态变量的函数给出的（即温度T在3.2 <= log（T）<= 4.5的范围内，参数R= rho/（T/10^6 K）^3在-8 <= log（R）<= 1的范围内），以及任意的化学混合物。化学目前解决了约800种，包括近300种原子和500种分子。气体不透明度解释了许多连续和离散源，包括原子不透明度、分子吸收带和碰撞诱导吸收。在AESOPUS上进行的几次测试证明，新的不透明度工具在结果上是准确的，在输入处方的管理上是灵活的，并且在计算时间要求方面是敏捷的。我们建立了一个网络界面（http：//stev.oapd.inaf.it/aesopus），使用户能够根据他/她的具体需要计算和快速检索RM不透明度表，允许在指定气体的化学成分的完全自由度。有用的应用可能是考虑RM不透明度的气体混合物与i）缩放太阳的金属丰度，选择在各种太阳的混合物汇编在文献中; ii）不同的CNO丰度，适合于演化模型的红色和渐近巨星分支星和大质量恒星在沃尔夫-拉叶阶段; iii）α元素的不同程度的增强，以及C-N、Na-O和Mg-Al丰度的反相关，这是正确描述早型星系和银河系球状星团中恒星性质所必需的; iv）适合于研究原始条件下气体不透明度的零金属丰度。
英文摘要：
We introduce a new tool - AESOPUS: Accurate Equation of State and OPacity Utility Software - for computing the equation of state and the Rosseland mean (RM) opacities of matter in the ideal gas phase. Results are given as a function of one pair of state variables, (i.e. temperature T in the range 3.2 <= log(T) <= 4.5, and parameter R= rho/(T/10^6 K)^3 in the range -8 <= log(R) <= 1), and arbitrary chemical mixture. The chemistry is presently solved for about 800 species, consisting of almost 300 atomic and 500 molecular species. The gas opacities account for many continuum and discrete sources, including atomic opacities, molecular absorption bands, and collision-induced absorption. Several tests made on AESOPUS have proved that the new opacity tool is accurate in the results,flexible in the management of the input prescriptions, and agile in terms of computational time requirement. We set up a web-interface (http://stev.oapd.inaf.it/aesopus) which enables the user to compute and shortly retrieve RM opacity tables according to his/her specific needs, allowing a full degree of freedom in specifying the chemical composition of the gas. Useful applications may regard RM opacities of gas mixtures with i) scaled-solar abundances of metals, choosing among various solar mixture compilations available in the literature; ii) varying CNO abundances, suitable for evolutionary models of red and asymptotic giant branch stars and massive stars in the Wolf-Rayet stages; iii) various degrees of enhancement in alpha-elements, and C-N, Na-O and Mg-Al abundance anti-correlations, necessary to properly describe the properties of stars in early-type galaxies and Galactic globular clusters; iv) zero-metal abundances appropriate for studies of gas opacity in primordial conditions.
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