太阳米粒中的氧气线。I.针对具有高空间和光谱分辨率的新观测结果测试3D模型
Oxygen lines in solar granulation. I. Testing 3D models against new observations with high spatial and spectral resolution
摘要：
目的：我们寻求提供额外的测试线形成的理论三维太阳光球模型。特别是，我们开始测试的空间分辨线形成在几个视角，从太阳盘中心的肢体和原子氧线的重点。这些测试的目的是提供关于3D模型是否适合导出太阳氧丰度的额外信息。我们的目标还在于经验约束中性氢碰撞的NLTE配方，使用OI 777 nm线的空间分辨观测。研究方法：利用瑞典1米太阳望远镜，我们获得了高空间分辨率的观测结果，在太阳盘面的五个位置上观测到五条氧原子谱线（以及其他种类的谱线）。这些观测具有高的空间和光谱分辨率，以及在615 nm处高达9%的连续强度对比度。使用3D模型计算理论谱线轮廓，其中氧气采用全3D NLTE处理，其他谱线采用LTE处理。结果：在磁盘中心，我们发现一个很好的协议之间的预测和观察到的线位移，强度，半高宽和不对称性。在其他视角下，一致性也很好，但较小的连续强度对比度使定量比较变得困难。我们利用盘心观测值来约束与中性氢碰撞效率的标度因子S_H。我们发现，S_H=1提供了最好的匹配的观察。结论：总的来说，预测和观测到的太阳颗粒线特性之间有很好的一致性。这进一步强化了3D模型是现实的，是导出太阳氧丰度的可靠工具的观点。
英文摘要：
Aims: we seek to provide additional tests of the line formation of theoretical 3D solar photosphere models. In particular, we set out to test the spatially-resolved line formation at several viewing angles, from the solar disk-centre to the limb and focusing on atomic oxygen lines. The purpose of these tests is to provide additional information on whether the 3D model is suitable to derive the solar oxygen abundance. We also aim to empirically constrain the NLTE recipes for neutral hydrogen collisions, using the spatially-resolved observations of the OI 777 nm lines. Methods: using the Swedish 1-m Solar Telescope we obtained high-spatial-resolution observations of five atomic oxygen lines (along with lines for other species) for five positions on the solar disk. These observations have a high spatial and spectral resolution, and a continuum intensity contrast up to 9% at 615 nm. The theoretical line profiles were computed using the 3D model, with a full 3D NLTE treatment for oxygen and LTE for the other lines. Results: at disk-centre we find an excellent agreement between predicted and observed line shifts, strengths, FWHM and asymmetries. At other viewing angles the agreement is also good, but the smaller continuum intensity contrast makes a quantitative comparison harder. We use the disk-centre observations we constrain S_H, the scaling factor for the efficiency of collisions with neutral hydrogen. We find that S_H=1 provides the best match to the observations. Conclusions: overall there is a very good agreement between predicted and observed line properties over the solar granulation. This further reinforces the view that the 3D model is realistic and a reliable tool to derive the solar oxygen abundance.
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