日冕物质抛射及其伴生的射电辐射观测特征  

Observational Characteristics of CME Events and Associated Radio Emission

作　　者：谢瑞祥[1] 汪敏[1] 颜毅华[2] 谭程明[2] 

机构地区：[1]中国科学院国家天文台云南天文台,云南昆明650011 [2]中国科学院国家天文台,北京100012

出　　处：《天文研究与技术》2011年第2期95-99,F0002,F0003,共7页Astronomical Research & Technology

基　　金：国家自然科学基金(10978006)资助

摘　　要：统计分析了太阳活动周下降段(2003～2005年)发生的76个共生CME的射电爆发事件。射电爆发资料来自国家天文台和Culgoora的微波和米波频谱仪。在76个事件中有50个快速CME和26个慢速CME。从中发现,快速CME和慢速CME的产率分别随着太阳活动周的降低而下降和上升,这可能说明CME的产率与太阳活动周中日冕磁结构的位形和位置变化有关。同时也发现,射电爆发的类型和寿命有一个变化规律,即随着频率的降低射电爆发的寿命变长,此特征支持了伴生CME的II型爆发统一模型的思想。另外还发现在厘米—分米波范围,CME开始前后,容易发生射电III型爆发或快速精细结构。这说明射电辐射的精细结构可能是CME的前兆现象或CME早期发展阶段由于磁重联引发的低日冕小尺度磁扰动的结果。We statistically analyze 76 radio-burst events associated with CME events during the period of 2003 - 2005, which is in the descending phase of solar activity cycle. The radio data are within the frequency range of 18 MHz to 7 200 MHz and are obtained from the LACSO/SOHO or the spectrometers of Culgoora and NAOC （National Astronomical Observatories of China）. Out of the 76 events 50 and 26 are fast and slow, respectively. We find that the fractions of fast and slow CME events decrease and increase in the descending phase of solar activity cycle, respectively. This is possibly because of the correlation of the frequencies of CME events with the variations of structures and positions of solar magnetic fields during the solar activity cycle. Furthermore, we find a trend for types and durations of radio bursts. The durations decrease with the radio frequencies. The trend supports the idea of a unified model about type-Ⅱ radio bursts associated with CMEs. In addition, we find that type-Ⅲ bursts or fast fine structures （FS） frequently occur in the wavelength range of centimeters to meters just before or after the CMEs start. The radio FS could be interpreted as precursor phenomena of the CMEs or as the results of small-scale magnetic disturbances in the lower corona caused by magnetic reeonnections during the early phases of the CMEs.

关 键 词：太阳 CME 射电爆发 

分 类 号：P182.24[天文地球—天文学]