中性铬的实验室跃迁几率的改进及太阳和三星铬吸收度的重新测定
Improved Laboratory Transition Probabilities for Neutral Chromium and Re-determination of the Chromium Abundance for the Sun and Three Stars
摘要：
从傅里叶变换光谱与公布的辐射寿命的分支分数测量被用来确定263线的中性铬的跃迁几率。利用这些实验室数值推导出一个新的太阳光球丰度：log $ε$（Cr I）$_{\odot}$ = 5.64 $\pm$ 0.01（$σ= 0.07$）。这些Cr I太阳丰度没有表现出任何趋势线强度，也没有与激发能，也没有明显的迹象偏离LTE。此外，FERRUM项目最近报告的单离子化铬的振子强度用于确定：log $ε$（Cr II）$_{\odot}$ = 5.77 $\pm$ 0.03（$σ= 0.13$）。跃迁概率数据也被应用于三颗恒星的光谱：HD 75732（富金属矮星）、HD 140283（贫金属亚巨星）和CS 22892-052（贫金属巨星）。在所有选定的恒星，铬I被发现是相对于铬II不足。这种丰度差异和明显的电离不平衡的可能原因进行了讨论。
英文摘要：
Branching fraction measurements from Fourier transform spectra in conjunction with published radiative lifetimes are used to determine transition probabilities for 263 lines of neutral chromium. These laboratory values are employed to derive a new photospheric abundance for the Sun: log $ε$(Cr I)$_{\odot}$ = 5.64$\pm$0.01 ($σ= 0.07$). These Cr I solar abundances do not exhibit any trends with line strength nor with excitation energy and there were no obvious indications of departures from LTE. In addition, oscillator strengths for singly-ionized chromium recently reported by the FERRUM Project are used to determine: log $ε$(Cr II)$_{\odot}$ = 5.77$\pm$0.03 ($σ= 0.13$). Transition probability data are also applied to the spectra of three stars: HD 75732 (metal-rich dwarf), HD 140283 (metal-poor subgiant), and CS 22892-052 (metal-poor giant). In all of the selected stars, Cr I is found to be underabundant with respect to Cr II. The possible causes for this abundance discrepancy and apparent ionization imbalance are discussed.
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