太阳射电毫秒Spike辐射窄带宽的理论探讨  

A THEORETICAL STUDY ON THE NARROW BANDWIDTH OF THE SOLAR RADIO MILLISECOND SPIKE RADIATION

作　　者：史建魁[1] 赵仁扬[1] 

机构地区：[1]中国科学院北京天文台

出　　处：《天体物理学报》1990年第1期75-81,共7页

摘　　要：在磁拱底部非线性等离子体密度波传播期间,损失锥分布的反射电子驱动着电子迴旋maser不稳定性的增长,激励出二次谐频波模,支配着太阳射电毫秒Spike辐射。根据这个理论模型,本文着重研究了太阳射电毫秒Spike辐射的频带宽度问题。对于典型参数,计算结果发现:辐射带宽一般为几MHz到几十MHz,最高为100MHz。而且通常折射出的二次谐频z模辐射带宽较窄,而二次谐频o模辐射带宽较宽。The reflected electrons of a loss-cone distribution can drive the electron cyclotron maser instability when a nonlinear density wave travells through the bottom part of the magnetic loop. The maser instability will excite the second harmonic O-mode and X-mode to dominate the solar radio millisecond spike radiation. On the basis of the above model, we have emphatically studied the bandwidth of the solar radio millisecond spike radiation. It can be found from the calculations that the bandwidths of the millisecond spike radiation are generally from a few MHz to scores of MHz, i.e. not more than 100 MHz. The bandwidths of the second harmonic refracted Z-model are generally narrower than those of the second harmonic O-mode.

关 键 词：太阳 射电 SPIKE辐射 频带宽度 

分 类 号：P182.24[天文地球—天文学]