论文标题
B-Star在太阳能街区的霓虹灯丰度
Neon Abundances of B-stars in the Solar Neighborhood
论文作者
论文摘要
我们使用可用的最新原子数据为NEI-NEII构建了一个综合模型原子，并评估了代表B型星的大气的NEI和NEII的非本地热力学平衡（NLTE）线形成。我们发现，与2P $^5 $ 3P $ - $ 2P $^5 $ 3S过渡阵列相对应的NEI线的大型NLTE加强阵列发生，这是由于2p $^5 $ 3S水平的极小光电离截面导致这些水平相对于其LTE群体的强大人口过多。对于最多的NEII线，与LTE的偏差很小，绝对值中不超过0.11〜DEX。我们在10 \，400 $ \ le $ \ teff \ $ \ $ 33 \，400〜k的温度范围内分析了20行NEI和13行NEII的NEII和13行NEII。对于五颗恒星，NLTE导致NEI和NEII的一致性，而LTE丰度的差异最高可达0.50〜DEX。 Piracha等人最近测量的实验振荡器强度的使用。 （2015年）导致对最受调查的恒星的逐线散射较小。在太阳能社区二十四个B型星中的平均霓虹灯丰度为8.02 $ \ pm $ 0.05。该值可能会在太阳光球霓虹灯丰度上提供间接限制。
We constructed a comprehensive model atom for NeI -- NeII using the most up-to-date atomic data available and evaluated the non-local thermodynamic equilibrium (NLTE) line formation for NeI and NeII in classical 1D models representing the atmospheres of B-type stars. We find that the large NLTE strengthening of the NeI lines corresponding to the 2p$^5$3p $-$ 2p$^5$3s transitions array occurs due to extremely small photoionization cross-sections of 2p$^5$3s levels that leads to strong overpopulation of these levels relative to their LTE populations. The deviations from LTE for the most NeII lines are small and do not exceed 0.11~dex in the absolute value. We analysed 20 lines of NeI and 13 lines of NeII for twenty-four B-type stars in the temperature range of 10\,400 $\le$ \Teff\ $\le$ 33\,400~K. For five stars, the NLTE leads to consistent abundances of NeI and NeII, while the difference in LTE abundance can reach up to 0.50~dex. The using of the experimental oscillator strengths recently measured by Piracha et al. (2015) leads to smaller line-by-line scatter for the most investigated stars. The averaged neon abundance in twenty-four B-type stars in solar neighborhood is 8.02$\pm$0.05. This value may provide indirect constraints on solar photospheric neon abundance.
