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3-D Magnetohydrodynamics Simulation of the Solar Emerging Flux

机译：3-D磁力流体动力学模拟太阳能出现助焊剂

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This three-dimensional magnetohydrodynamics simulation is used to study the nonlinear evolution of the magnetic buoyancy instability of a magnetic flux sheet with magnetic shear. A horizontal flux sheet that is initially placed below the solar photosphere is susceptible to both the interchange insta. bility and the Parker instability (the undular mode of the magnetic buoyancy instability). In the nonlinear stage, the development depends on the initial perturbation as well as the initial magnetic field configuration (i.e., the presence of magnetic shear). When an initial non-periodic perturbation or random perturbations is assumed, the magnetic flux expands horizontally when the magnetic field emerges a little into the photosphere. The distribution of the magnetic field and gas tends to be in a new state of magnetohydrostatic equilibrium. When magnetic shear is present in the initial magnetic flux sheets, the interchange mode is stabilized so that the emerging loop is higher than in the no magnetic shear case. We discuss how the presented results are related to the emerging flux observed on the Sun.
机译：这种三维磁力流体动力学模拟用于研究磁性剪切磁通片的磁性浮力不稳定性的非线性演变。最初放置在太阳照片低下的水平磁通片易于交换Insta。 Bility和Parker不稳定性（磁力浮力不稳定的非模式）。在非线性阶段，显影取决于初始扰动以及初始磁场配置（即，磁剪切的存在）。当假设初始非周期性扰动或随机扰动时，当磁场出现一点进入Photosphere时，磁通量水平膨胀。磁场和气体的分布趋于处于磁性水氢化性平衡的新状态。当磁剪切存在于初始磁通量表中时，稳定互换模式，使得新出现的环路高于No磁剪切壳体。我们讨论所提出的结果与在太阳上观察到的新兴助焊剂有关。

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