THE QUIET SOLAR ATMOSPHERE OBSERVED AND SIMULATED IN Na i D1
THE QUIET SOLAR ATMOSPHERE OBSERVED AND SIMULATED IN Na i D1
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Na i D1 中安静的太阳大气观测和模拟
DOI：
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发表时间：
2009
期刊：
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通讯作者：
V. Hansteen
中科院分区：
文献类型：
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作者：
J. Leenaarts;R. Rutten;K. Reardon;M. Carlsson;V. Hansteen
太阳光谱中的Na I D1线有时被归因于太阳色球。我们研究了它在静太阳网络和网际网络中的形成。我们首先展示了用邓恩太阳望远镜的成像光谱仪干涉二维光谱仪在这条线上拍摄的高分辨率轮廓分辨率图像，并将这些图像与在CA II8542ä和Hα上同时拍摄的色球图像进行了比较。然后，我们通过对来自三维辐射-磁流体模拟的快照进行三维(3D)非局域热力学平衡剖面合成来模拟Na I D1形成。我们发现，大多数Na I d1亮度不是色球的，而是采样了光球中组成太阳安静网络的磁场浓度，远低于它们合并到色球冠层的高度，来自3D共振散射的光晕。线路核心对磁力集中区及其附近的磁声激波非常敏感，这些磁声激波发生在比其他地方更深的地方，并可能提供磁力集中区深处加热的证据。
The Na i D1 line in the solar spectrum is sometimes attributed to the solar chromosphere. We study its formation in quiet-Sun network and internetwork. We first present high-resolution profile-resolved images taken in this line with the imaging spectrometer Interferometric Bidimensional Spectrometer at the Dunn Solar Telescope and compare these to simultaneous chromospheric images taken in Ca ii 8542 Å and Hα. We then model Na i D1 formation by performing three-dimensional (3D) non-local thermodynamic equilibrium profile synthesis for a snapshot from a 3D radiation-magnetohydrodynamics simulation. We find that most Na i D1 brightness is not chromospheric but samples the magnetic concentrations that make up the quiet-Sun network in the photosphere, well below the height where they merge into chromospheric canopies, with aureoles from 3D resonance scattering. The line core is sensitive to magneto-acoustic shocks in and near magnetic concentrations, where shocks occur deeper than elsewhere, and may provide evidence of heating deep within magnetic concentrations.