A ‘proof of principle’ is presented, whereby the Ohmic and viscous heating determined by a three-dimensional (3D) MHD model of a coronal avalanche are used as the coronal heating input for a series of field-aligned, one-dimensional (1D) hydrodynamic models. Three-dimensional coronal MHD models require large computational resources. For current numerical parameters, it is difficult to model both the magnetic field evolution and the energy transport along field lines for coronal temperatures much hotter than $1\, \mathrm{MK}$, because of severe constraints on the time step from parallel thermal conduction. Using the 3D MHD heating derived from a simulation and evaluated on a single field line, the 1D models give coronal temperatures of $1\, \mathrm{MK}$ and densities $10^{14}\textrm {--}10^{15}\, \mathrm{m}^{-3}$ for a coronal loop length of $80\, \mathrm{Mm}$. While the temperatures and densities vary smoothly along the field lines, the heating function leads to strong asymmetries in the plasma flows. The magnitudes of the velocities in the 1D model are comparable with those seen in 3D reconnection jets in our earlier work. Advantages and drawbacks of this approach for coronal modelling are discussed.

中文翻译：

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连接计算模型以跟踪加热日冕等离子体的演变

提出了“原理证明”，其中由日冕雪崩的三维 (3D) MHD 模型确定的欧姆和粘性加热被用作一系列场对齐的一维 (1D) 的日冕加热输入) 水动力模型。三维日冕 MHD 模型需要大量的计算资源。对于当前的数值参数，由于平行热传导对时间步长的严格限制，很难对日冕温度远高于 $1\, \mathrm{MK}$ 的磁场演化和沿磁力线的能量传输进行建模. 使用来自模拟的 3D MHD 加热并在单个场线上进行评估，1D 模型给出的日冕温度为 $1\, \mathrm{MK}$ 和密度 $10^{14}\textrm {--}10^{15 }\, \mathrm{m}^{-3}$，冠状环长度为 $80\，\mathrm{嗯}$。虽然温度和密度沿场线平稳变化，但加热功能会导致等离子体流中的强烈不对称性。1D 模型中的速度大小与我们早期工作中的 3D 重新连接喷流中的速度大小相当。讨论了这种冠状建模方法的优点和缺点。