New emission branching fraction (BF) measurements for 183 lines of the second spectrum of chromium (Cr II) and new radiative lifetime measurements from laser-induced fluorescence for 8 levels of Cr+ are reported. The goals of this study are to improve transition probability measurements in Cr II and reconcile solar and stellar Cr abundance values based on Cr I and Cr II lines. Eighteen spectra from three Fourier Transform Spectrometers supplemented with ultraviolet spectra from a high-resolution echelle spectrometer are used in the BF measurements. Radiative lifetimes from this study and earlier publications are used to convert the BFs into absolute transition probabilities. These new laboratory data are applied to determine the Cr abundance log ε in the Sun and metal-poor star HD 84937. The mean result in the Sun is 〈logε (Cr II)〉 = 5.624±0.009 compared to 〈logε(Cr I)〉 = 5.644 ± 0.006 on a scale with the hydrogen abundance log ε(H) = 12 and with the uncertainty representing only line-to-line scatter. A Saha (ionization balance) test on the photosphere of HD 84937 is also performed, yielding 〈logε(Cr II)〉 = 3.417 ± 0.006 and 〈log ε(Cr I, lower level excitation potential E. P. >30 eV)〉 = 3.3743±30.011 for this dwarf star. We find a correlation of Cr with the iron-peak element Ti, suggesting an associated nucleosynthetic production. Four iron-peak elements (Cr along with Ti, V, and Sc) appear to have a similar (or correlated) production history-other iron-peak elements appear not to be associated with Cr.

中文翻译：

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太阳和贫金属星HD 84937的光球中改进的Cr II log（gf）值和丰度测定

报道了铬的第二光谱（Cr II）的183条谱线的新发射支化分数（BF）测量，以及8种Cr +水平的激光诱导荧光的新辐射寿命测量结果。这项研究的目标是改善Cr II中的跃迁概率测量，并根据Cr I和Cr II线调和太阳和恒星Cr的丰度值。高炉测量中使用了来自三个傅立叶变换光谱仪的18个光谱，再加上来自高分辨率echelle光谱仪的紫外线光谱。这项研究和较早发表的文献的辐射寿命用于将高炉转换为绝对跃迁概率。这些新的实验室数据被用于确定太阳和贫金属恒星HD 84937中的Cr丰度logε。太阳的平均结果为<logε（Cr II）> = 5.624±0。009与<logε（Cr I）> = 5.644±0.006相比，氢丰度logε（H）= 12且不确定度仅表示线对线散布。还对HD 84937的光球进行了Saha（电离平衡）测试，得出<logε（Cr II）> = 3.417±0.006和<logε（Cr I，较低水平的激发电势EP> 30 eV）> = 3.3743± 30.011这个矮星。我们发现Cr与铁峰元素Ti的相关性，表明相关的核合成产物。四个铁峰元素（Cr以及Ti，V和Sc）似乎具有相似（或相关）的生产历史-其他铁峰元素似乎与Cr不相关。还对HD 84937的光球进行了Saha（电离平衡）测试，得出<logε（Cr II）> = 3.417±0.006和<logε（Cr I，较低水平的激发电势EP> 30 eV）> = 3.3743± 30.011这个矮星。我们发现Cr与铁峰元素Ti的相关性，表明相关的核合成产物。四个铁峰元素（Cr以及Ti，V和Sc）似乎具有相似（或相关）的生产历史-其他铁峰元素似乎与Cr不相关。还对HD 84937的光球进行了Saha（电离平衡）测试，得出<logε（Cr II）> = 3.417±0.006和<logε（Cr I，较低水平的激发电势EP> 30 eV）> = 3.3743± 30.011这个矮星。我们发现Cr与铁峰元素Ti的相关性，表明相关的核合成产物。四个铁峰元素（Cr以及Ti，V和Sc）似乎具有相似（或相关）的生产历史-其他铁峰元素似乎与Cr不相关。