伴随CME的微波爆发的特征

The features of CME-associated microwave bursts

分析了与日冕物质抛射(CME)有关的太阳微波爆发(SMB)的特征,包括持 续时间、峰值流量、爆发类型、谱指数等．选取了从1999年11月至2003年9月的136 个事件,包括60个部分晕状CME(120°<宽度<360°)／晕状CME(宽度=360°)和 76个正常CME(20°<宽度<120°)／窄CME(0°<宽度<20°)． 研究发现: (1)与正常CME／窄CME有关的微波爆发持续时间较短,与部分晕状 ／晕状CME有关的微波爆发持续时间有长有短; (2)与慢CME有关的微波爆发持续时 间较短,与快CME有关的微波爆发持续时间可长可短;(3)与正常／窄CME有关的微 波爆发峰值辐射流量比较小,与部分晕状／晕状CME有关的微波爆发峰值辐射流量有大 有小;(4)与慢CME有关的微波爆发峰值辐射流量较小,与快CME有关的微波爆发峰 值辐射流量可长可短; (5)与正常／窄CME有关的微波爆发绝大多数为简单(simple) 型,与晕状CME有关的微波爆发绝大多数为复杂(C)／大爆发(GB)型; (6)与CME 有关的事件在频率,f<fmax(fmax是峰值频率)的高频部分都比较平坦．统计结果表明, 当CME／耀斑发生时,太阳微波波段会有明显的信号,太阳微波爆发可以为CME／耀 斑的研究提供信息． CME／耀斑和太阳微波爆发之间具有内在的物理联系．

The relationship of solar microwave bursts （SMBs） associated with CMEs is analysed. The features of SMBs are regarded including, we included lasting time, maximum flux, burst type, and spectral index. We choose 136 events, which are from November 1999 to September 2003 and include 60 partial halo/full halo CMEs and 76 narrow/normal CMEs. We find that： 1） The lasting times of SMBs associated with normal/narrow CMEs are usually short, but they cover a larger range when associated with partial halo/full halo CMEs. 2） The lasting times of SMBs associated with slow CMEs are usually short, but they cover a lager range when associated with fast CMEs. 3） The maximum fluxes of SMBs associated with normal/narrow CMEs or slow CMEs are small, but they cover a lager range when associated with partial halo/full halo CMEs or fast CMEs. 4） Most of SMBs associated with normal/narrow CMEs are S type, while most of them are C/GB type when associated with full halo CMEs. 5） The spectra of most of the CME-associated events are flat at higher frequencies. The statistical results show that an intrinsically physical relationship exists between CME/flare and SMB. SMB may provide some information on early life of CME/flare.