Title: Magnetic flux emergence and solar eruptions in partially ionized plasmas Show Chinese title

Title: 部分电离等离子体中的磁场通量浮现与太阳爆发活动

Abstract: We have performed 3D MHD simulations to study the effect of partial ionization in the process of magnetic flux emergence in the Sun. In fact, we continue previous work and we now focus: 1) on the emergence of the magnetic fields above the solar photosphere and 2) on the eruptive activity, which follows the emergence into the corona. We find that in the simulations with partial ionization (PI), the structure of the emerging field consists of arch-like fieldlines with very little twist since the axis of the initial rising field remains below the photosphere. The plasma inside the emerging volume is less dense and it is moving faster compared to the fully ionized (FI) simulation. In both cases, new flux ropes (FR) are formed due to reconnection between emerging fieldlines, and they eventually erupt in an ejective manner towards the outer solar atmosphere. We are witnessing three major eruptions in both simulations. At least for the first eruption, the formation of the eruptive FR occurs in the low atmosphere in the FI case and at coronal heights in the PI case. Also, in the first PI eruption, part of the eruptive FR carries neutrals in the high atmosphere, for a short period of time. Overall, the eruptions are relatively faster in the PI case, while a considerable amount of axial flux is found above the photosphere during the eruptions in both simulations. Show Chinese abstract

Abstract: 我们进行了三维磁流体力学（MHD）模拟，以研究部分电离效应对太阳磁场浮现过程的影响。 实际上，我们延续了之前的工作，并且现在关注两个方面：1）太阳光球层上方磁场的浮现；2）随后进入日冕的爆发活动。 我们发现，在部分电离（PI）的模拟中，浮现磁场的结构由类似拱桥的磁力线组成，且扭曲程度很小，因为初始上升磁场的轴线仍位于光球层以下。 与完全电离（FI）的模拟相比，浮现体积内的等离子体密度较低，运动速度更快。 在这两种情况下，由于浮现磁力线之间的重新连接，都会形成新的磁绳（FR），最终以喷发的方式向太阳外部大气层爆发。 我们观察到两种模拟中都发生了三次主要的爆发。 至少对于第一次爆发，在完全电离的情况下，爆发性磁绳的形成发生在低层大气中，而在部分电离的情况下则发生在日冕高度。 此外，在第一次部分电离的爆发中，有一部分爆发性磁绳在高大气层中短暂地携带中性粒子。 总体而言，部分电离情况下的爆发相对更快，而在两次模拟的爆发过程中，都在光球层以上发现了相当数量的轴向通量。