Mechanism of magnetic energy dissipation in weakly ionized solar atmospphere

通过对日月号航天器上太阳光学望远镜观测到的太阳色球喷流的数值模拟和分析，研究了太阳低层大气中完全碰撞弱电离等离子体的磁能量耗散机制。我们发现，与完全电离的日冕中的情况类似，与等离子体抛射相关的间歇性和快速的磁重联也发生在太阳色球中。这种间歇性和快速的磁重联的原因是双极扩散的不均匀。

We studied the magnetic energy dissipation mechanism of the fully collisional and weakly ionized plasma in the solar lower atomosphere by numerical simulation and analysis of the solar chromospheric jets observed by Solar Optical Telescope on Board Hinode space craft. We found that, similarly to the case in the fully ionized solar corona, intermittent and fast magnetic reconnection associated with plasmoids ejection is occurring also in the solar chromosphere. The cause of such intermittent and fast magnetic reconnection is the inhomogeneity of the ambipolar diffusion.