在太阳风中团块的形成和加速：会聚流和粘性的作用
Blob formation and acceleration in the solar wind: role of converging flows and viscosity
摘要：
本文用电阻MHD模拟方法分析了粘性和会聚流对慢太阳风中斑点形成的影响。形成斑点的日冕流光上方的区域（Sheeley等人，1997）使用先前由Einaudi等人（1999）提出的模型进行模拟。我们的调查结果是双重的。首先，我们证明了一种新的机制，增强形成的斑点和周围的快速太阳风之间的动量传递。这种效果是由形成斑点的撕裂不稳定性引起的更长范围的电场引起的。电场进入快速的太阳风并与之相互作用，造成一种粘性阻力，这种阻力本质上是全局性的，而不是像正常的不带电流体（如水）那样局部地穿过流体层。第二，在冕盔流光尖端的磁尖点的存在导致流光两侧的流的会聚和快速的太阳风对正在形成的岛的直接推动，从而导致更有效的动量交换。
英文摘要：
The effect of viscosity and of converging flows on the formation of blobs in the slow solar wind is analysed by means of resistive MHD simulations. The regions above coronal streamers where blobs are formed (Sheeley et al., 1997) are simulated using a model previously proposed by Einaudi et al. (1999). The result of our investigation is twofold. First, we demonstrate a new mechanism for enhanced momentum transfer between a forming blob and the fast solar wind surrounding it. The effect is caused by the longer range of the electric field caused by the tearing instability forming the blob. The electric field reaches into the fast solar wind and interacts with it, causing a viscous drag that is global in nature rather than local across fluid layers as it is the case in normal uncharged fluids (like water). Second, the presence of a magnetic cusp at the tip of a coronal helmet streamer causes a converging of the flows on the two sides of the streamer and a direct push of the forming island by the fast solar wind, resulting in a more efficient momentum exchange.
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