标题： 硫的禁线1082 nm：太阳的光球硫丰度和三维效应 显示英文标题

标题： The forbidden 1082 nm line of sulphur: the photospheric abundance of sulphur in the Sun and 3D effects

摘要： 硫是一种在α过程中形成的元素，在外部星系的气相中很容易被测量。 由于它不形成尘埃，因此是α元素的首选指标，而不是需要尘埃修正的硅或镁。 测量恒星中的硫丰度并不是一项简单的任务，主要依赖于激发程度较高的谱线，这些谱线在非局部热平衡（non-LTE）条件下有不可忽略的偏差。 1082纳米硫的禁戒跃迁对偏离LTE的敏感性较低，并且比其他通常用作丰度指示剂的硫线对温度不确定性的依赖性更低。 因此，它应该提供更可靠的丰度诊断。 目标：从1082纳米[S I]线推导太阳光球层中硫的丰度，并研究G型和F型大气在太阳金属丰度及更低金属丰度下的三维效应。 方法：使用高分辨率、高信噪比的太阳强度和通量光谱来测量[S I] 1082纳米线的硫丰度。 使用co5bold流体力学模型大气来预测[S I]线的三维丰度修正。 结果：太阳的硫丰度被确定为7.15±(0.01)统计±(0.05)系统，其中统计不确定性表示使用四种不同的太阳光谱进行测定的散射情况，系统不确定性是由于混合线建模引起的。 从这条线得到的硫丰度不受微湍流的影响。 通过一维与三维模型之间的严格差分比较得出的三维丰度修正在太阳中可以忽略不计，但对于金属丰度较低的矮星则变得显著。 显示英文摘要

摘要： Sulphur is an element which is formed in the alpha-process and is easily measured in the gaseous phase in external galaxies. Since it does not form dust, it is the preferred indicator for alpha-elements, rather than Si or Mg, for which dust corrections are necessary. The measurement of the sulphur abundance in stars is not an easy task, relying mainly on high excitation lines with non-negligible deviations from LTE. The 1082 nm sulphur forbidden transition is less sensitive to departures from LTE and is less dependent on temperature uncertainties than other sulphur lines usually employed as abundance indicators. Therefore it should provide a more robust abundance diagnostics. aims: To derive the solar photospheric abundance of sulphur from the 1082 nm [SI] line and to investigate 3D effects present in G- and F-type atmospheres at solar and lower metallicity. method: High-resolution, high signal-to-noise solar intensity and flux spectra were used to measure the sulphur abundance from the [SI] 1082 nm line. co5bold hydrodynamical model atmospheres were applied to predict 3D abundance corrections for the [SI] line. results: The solar sulphur abundance is derived to be 7.15+- (0.01)stat +- (0.05)sys, where the statistical uncertainty represents the scatter in the determination using four different solar spectra and the systematic uncertainty is due to the modelling of the blending lines. Sulphur abundances obtained from this line are insensitive to the micro-turbulence. 3D abundance corrections, found from strictly differential comparisons between 1D and 3D models, are negligible in the Sun, but become sizable for more metal-poor dwarfs.