Transition probabilities of trans-iron elements

对于热致密恒星的定量光谱分析，考虑偏离局部热力学平衡(LTE)的模型大气是必需的。与通过Saha和Boltzmann方程计算原子能级占据数的LTE不同，在所谓的非LTE中，它们必须被详细计算。其先决条件是所有辐射和碰撞跃迁的准确数据。这包括线跃迁，即原子能级之间的辐射束缚-束缚跃迁。精确的振子强度对于在模型大气计算中代表一个元素的模型原子中的所有谱线跃迁都是必要的。数据质量对丰度测定的精确度至关重要。最近发现的白矮星中比铁更重的元素，首次使人们能够确定演化恒星中所谓的反铁元素的丰度。这只有在计算振子强度之后才有可能。在这个项目中，我们建议将振子强度的计算扩展到很大一部分反铁元素(铜到钡)，并计算电离阶段III到VII的均匀数据，即2到6。新计算的振子强度首次允许在恒星演化的最后阶段对这些元素的丰度进行分析。这使我们能够建立S过程核合成的边界条件，即通过中子俘获产生反铁元素。

For the quantitative spectral analysis of hot, compact stars, model atmospheres that consider deviations from the local thermodynamical equilibrium (LTE) are mandatory. In contrast to LTE where the occupations numbers of atomic levels are calculated via Saha and Boltzmann equations, in the so-called non-LTE, they have to be calculated in detail. A pre-requisite therefor is accurate data for all radiative and collisional transitions. This includes line transitions, i.e. radiative bound-bound transitions between the atomic levels. Precise oscillator strengths are necessary for all line transitions in the model atom that represents an element in the model-atmosphere calculation. The data quality is crucial for the precision of abundance determinations.The recent discovery of elements that are heavier that iron in a white dwarf allowed for the first time to determine the abundance of so-called trans-iron elements in evolved stars. This was only possible after the calculation of oscillator strengths. We propose in this project to extend the calculation of oscillator strengths to a large part of the trans-iron elements (copper to barium) and to calculate homogeneous data for the ionization stages III to VII, i.e. 2+ to 6+.The newly calculated oscillator strengths allow for the first time the abundance analysis of these elements in stars in the final phase of their evolution. This enables us to establish boundary conditions for the s-process nucleosynthesis, i.e. the creation of trans-iron elements by neutron captures.