We carry out a study of the global three-dimensional (3D) structure of the electron density and temperature of the quiescent inner solar corona ( r < 1.25 R ⊙ $r<1.25\,\mathrm{R_{\odot }}$ ) by means of tomographic reconstructions and magnetohydrodynamic simulations. We use differential emission measure tomography (DEMT) and the Alfvén Wave Solar Model (AWSoM), in their latest versions. Two target rotations were selected from the solar minimum between Solar Cycles (SCs) 23 and 24 and the declining phase of SC 24. We report in quantitative detail on the 3D thermodynamic structure of the core and outer layers of the streamer belt, and of the high latitude coronal holes (CH), as revealed by the DEMT analysis. We report on the presence of two types of structures within the streamer belt, loops with temperature decreasing/increasing with height (dubbed down/up loops), as reported first in previous DEMT studies. We also estimate the heating energy flux required at the coronal base to keep these structures stable, found to be of order 10 5 erg cm − 2 s − 1 $10^{5}~\text{erg}\,\text{cm}^{-2}\,\text{s}^{-1}$ , consistently with previous DEMT and spectroscopic studies. We discuss how these findings are consistent with coronal dissipation of Alfvén waves. We compare the 3D results of DEMT and AWSoM in distinct magnetic structures. We show that the agreement between the products of both techniques is the best so far, with an overall agreement ≲ 20 % $\lesssim 20\%$ , depending on the target rotation and the specific coronal region. In its current implementation the ASWsoM model cannot reproduce down loops though. Also, in the source region of the fast and slow components of the solar wind, the electron density of the AWSoM model increases with latitude, opposite to the trend observed in DEMT reconstructions.

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日冕的热力学结构：断层扫描重建和 MHD 建模

我们对静止内日冕的电子密度和温度的全局三维（3D）结构进行了研究（ r < 1.25 R ⊙ $r<1.25\,\mathrm{R_{\odot }}$ ）通过断层扫描重建和磁流体动力学模拟。我们在最新版本中使用差分发射测量断层扫描 (DEMT) 和阿尔文波太阳模型 (AWSoM)。从太阳活动周期 (SC) 23 和 24 之间的太阳极小期以及 SC 24 的下降阶段中选择了两个目标旋转。我们定量详细报告了拖缆带核心和外层的 3D 热力学结构，以及DEMT 分析揭示的高纬度日冕洞 (CH)。我们报告了在拖缆带中存在两种类型的结构，温度随高度降低/增加的循环（称为向下/向上循环），如先前 DEMT 研究中首次报道的那样。我们还估计了日冕底部保持这些结构稳定所需的热能通量，发现其数量级为 10 5 erg cm − 2 s − 1 $10^{5}~\text{erg}\,\text{cm} ^{-2}\,\text{s}^{-1}$ ，与之前的 DEMT 和光谱研究一致。我们讨论这些发现如何与阿尔文波的日冕耗散一致。我们比较了 DEMT 和 AWSoM 在不同磁结构中的 3D 结果。我们表明，两种技术的产品之间的一致性是迄今为止最好的，总体一致性 ≲ 20 % $\lesssim 20\%$ ，取决于目标旋转和特定的冠状区域。但是，在其当前实现中，ASWsoM 模型无法重现向下循环。还，