The aim of this paper is to determine the kinetic temperature of solar prominences from widths of emission lines with a careful evaluation of its validity, and to investigate the spatial distribution of the non-thermal velocity and the kinetic temperature in prominences. Spectroscopic observations of prominences were carried out using the Domeless Solar Telescope at the Hida observatory in four emission lines, i.e., H|$\alpha$||$656.3\:$|nm, H|$\beta$||$486.1\:$|nm, Ca|$^{+}$|IR |$854.2\:$|nm, and Ca|$^{+}$|K |$393.4\:$|nm. We found systematic differences in temperature and its spatial distributions in prominences obtained from different pairs of spectral lines. The reason for the difference is that the intrinsic widths of emission lines determined by a single-slab model are different for optically thick and thin lines, and can be attributed to the assumption of a Gaussian profile of the non-thermal broadening in the single-slab model. With numerical experiments, we found that the observed differences among line pairs can be reproduced by a multi-slab model, in which each slab has different non-thermal broadening and line-of-sight velocity. The most accurate evaluation of the temperature is obtained with the pair of H|$\beta$| and Ca|$^{+}$|IR in our selection. Based on these results, we found the typical kinetic temperature of prominences to be 8000–|$12000\:$|K, which is significantly higher than the temperature determined by radiative balance and suggests the presence of mechanical heating in prominences. Also suggested is the presence of positive spatial correlation between non-thermal velocity and temperature. We revisit past observational results on the prominence temperature and discuss the reason for discrepancies among them.

中文翻译：

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通过多波长观测对太阳突出的温度进行分析

本文的目的是通过仔细评估其有效性从发射线的宽度确定太阳突出的动温度，并研究非热速度和突出的动温度的空间分布。在飞Do天文台使用无圆顶太阳望远镜在四个发射线（即H | $ \ alpha $ |）上进行了突出的光谱观察。| $ 656.3 \：$$ nm，H | $ \ beta $ | | $ 486.1 \：$$ nm，Ca | $ ^ {+} $ | IR | $ 854.2 \：$ | nm和Ca | $ ^ {+} $ | K | $ 393.4 \ :: $ |纳米 我们发现了温度及其空间分布的系统差异，这些差异是从不同对光谱线获得的。造成这种差异的原因是，由单板模型确定的发射线的本征宽度对于光学上的粗线和细线而言是不同的，并且可以归因于以下假设：平板模型。通过数值实验，我们发现线对之间观察到的差异可以通过多板模型来再现，其中每个板具有不同的非热展宽和视线速度。通过| H | $ \ beta $ |对可获得最准确的温度评估。和Ca | $ ^ {+} $ |IR在我们的选择中。根据这些结果，我们发现突起的典型动力学温度为8000– | $ 12000 \：$ |。K，其显着高于通过辐射平衡确定的温度，并表明突出存在机械加热。还建议在非热速度和温度之间存在正空间相关性。我们回顾了以往关于突出温度的观测结果，并讨论了其中差异的原因。