Although 98% of the solar material consists of hydrogen and helium, the remaining chemical elements contribute in a discernible way to the thermodynamic quantities. An adequate treatment of the heavy elements and their excited states is important for solar models that are subject to the stringent requirements of helioseismology. The contribution of various heavy elements in a set of thermodynamic quantities has been examined. Characteristic features that can trace individual heavy elements in the adiabatic exponent γ1 = (? ln p/? ln )s (s being specific entropy), and hence in the adiabatic sound speed, were searched. It has emerged that prominent signatures of individual elements exist and that these effects are greatest in the ionization zones, typically located near the bottom of the convection zone. The main result is that part of the features found here depend strongly on both the given species (atom or ion) and its detailed internal partition function, whereas other features only depend on the presence of the species itself, not on details such as the internal partition function. The latter features are obviously well suited for a helioseismic abundance determination, while the former features present a unique opportunity to use the Sun as a laboratory to test the validity of physical theories of partial ionization in a relatively dense and hot plasma. This domain of plasma physics has so far no competition from terrestrial laboratories. Another, quite general, finding of this work is that the inclusion of a relatively large number of heavy elements has a tendency to smear out individual features. This affects both the features that determine the abundance of elements and the ones that identify physical effects. This property alleviates the task of solar modelers because it helps to construct a good working equation of state that is relatively free of the uncertainties from basic physics. By the same token, it makes more difficult the reverse task, which is constraining physical theories with the help of solar data.
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机译：尽管98％的太阳能材料由氢和氦组成，但其余化学元素以可辨别的方式对热力学量有所贡献。对重元素及其激发态的适当处理对于受到日震学严格要求的太阳模型很重要。已经检查了各种重元素在一组热力学量中的贡献。搜索可以追踪绝热指数γ1=（Δln p /Δln）s（s为比熵），从而绝热声速的单个重元素的特征。已经显示出存在单个元素的显着特征，并且这些效应在通常位于对流区底部附近的电离区中最大。主要结果是，此处找到的部分特征在很大程度上取决于给定的物种（原子或离子）及其详细的内部分配功能，而其他特征仅取决于物种本身的存在，而不取决于诸如内部的细节分区功能。后者的特征显然非常适合于流变丰度的测定，而前者的特征提供了一个独特的机会，可以使用太阳作为实验室来测试相对密集和热等离子体中部分电离的物理理论的有效性。迄今为止，等离子体物理学的这一领域还没有与地面实验室竞争。这项工作的另一个相当普遍的发现是，包含相对大量的重元素往往会弄脏各个特征。这会影响确定元素丰度的功能以及确定物理效果的功能。该特性减轻了太阳建模者的工作，因为它有助于构建一个良好的状态方程，而该方程基本没有基本物理学的不确定性。同样地，逆向任务也变得更加困难，逆向任务借助太阳数据限制了物理理论。
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