摘要
本文分析了Sag。Hill天文台观测到的1989年3月6日在1353 UT左右发生的一个罕见的大C型爆,即延伸型耀斑大爆发。假设射电辐射来自处于磁环顶部的均匀源,采用合适的日冕磁场值(100高斯),可推算出射电源中的非热电子总数N_R(5.6×10^(37)),这与一个标准硬X射线发射(I_p=10~6ε^(-3.5))的薄靶模型所预计的非热电子总数N_X(2.8×10^(37))相近。由此表明这两类辐射可能有共同的或紧密相关的非热电子分布起源。文中还用统计规律估算该事件的硬X射线大于30keV以上各通道的总记数率,即HXRBS峰率F_X为1.1×10~5s^(-1)。 文中还分析了长期存有争论的N_R与N_X相差10~3—10~5的原因,可能主要是N_R估计不准。这种估计不准,除理论原因外,还有流量测量精度不够的原因。如流量测量误差在±30％时,就可使N_R的估计值相差10~2—10~3。
A type C microwave burst observed at Sag. Hill observatory is analysed. It occoured at 1353UT on 6 March 1989 in active region 5395. The number of electrons Nr in the radio emission source is calculated using a proper value of magnetic field (100G), assuming the source to be homogeneous and to be located on the coronal part of magnetic loops. We have also calculated the number of electrons, NX, which is required for interpreting the hard X-ray flare emission (Ip = 106ε-3.5) in the standard thin-target model. We find that Nr(5.6×1087) is similar to Nx (2.8×1037). So it is reasonable to conclude that both emissions may be produced by the same population of electrons. The HXRBS peak rate Fx, the sum of the counting rate in all channels ≥30KeV, is estimated to be 1.1×105/s based on a statistical result. It is point out that the long-standing controversy concerning the Nx and Nx may be caused in great part by the measurement error of radio flux S. For example, an ±30% error of S could cause a 102-103 times difference in estimating the number Nr.
