【摘要】 观测研究表明有利于磁重联的新浮磁流与日冕物质抛射(CME)有密切关系．利用数值模拟的方法,新浮磁流触发CME的物理模型对观测结果进行了物理解释．基于这种模型,不考虑重力和热传导, 2．5维的数值模拟的理论结果显示:是否能够触发暗条爆发及CME,取决于新浮磁流磁通量的大小、浮现的位置以及其磁极走向,并给出了能够触发暗条爆发与不能触发爆发的参数空间．利用2002年和2003年的15个暗条爆发事例以及2002年的44个非爆发事例,对新浮磁流磁通量的大小、浮现的位置以及磁极走向进行了统计研究．结果表明并非所有的新浮磁流都能够使暗条失去平衡,形成CME．统计结果基本上支持了数值模拟的理论结果．这个结果可为空间天气预报研究提供有用的参考信息．更多还原

【Abstract】 Observations indicated that solar coronal mass ejections (CMEs) are strongly associated with reconnection-favored flux emergence. As suggested by observations, two types of emerging flux with reconnection-favored direction can trigger filament eruptions (and then CMEs): one is within the filament channel, and the other is on the outer edge of the channel. Based on numerical simulations, a physical model of the emerging flux trigger mechanism for CMEs is proposed, which explained well the observational phenomena. Using 2.5 dimensional numerical simulations with the gravity and heat conduction being omitted, the eruption and non-eruption regimes are presented in parameter space, which indicate that whether a CME can be triggered depends on both the amount and the location of an emerging flux, besides its polarity orientation. Furthermore, by analyzing 15 eruption events in 2002 and 2003 and 44 non-eruption events in 2002, the relation between filament eruptions (and CMEs) and the properties of emerging flux including its polarity orientation, its location, and the amount of the unsigned flux is studied statistically. The results show that not all the emerging flux can make a filament lose equilibrium and then trigger the onset of a CME. The statistic results basically support the theoretical numerical simulations, in which the 2.5 dimensional time dependent compressible resistive MHD equations are numerically solved with a multi-step implicit scheme. This research provides useful information for the space weather forecast.更多还原