Evolvement of microwave spike bursts in a solar flare on 2006 December 13  

作　　者：Jian-Fei Tang De-Jin Wu Jun-Lin Wan Ling Chen Cheng-Ming Tan 

机构地区：[1]Xinjiang Astronomical Observatory,Chinese Academy of Sciences,Urumqi 830011,China [2]Key Laboratory of Planetary Sciences,Purple Mountain Observatory,Nanjing 210023,China [3]CAS Key Laboratory of Solar Activity,National Astronomical Observatories,CAS,Beijing 100101,China [4]School of Astronomy and Space Science,University of Chinese Academy of Sciences,Beijing 100049,China

出　　处：《Research in Astronomy and Astrophysics》2021年第6期359-368,共10页天文和天体物理学研究（英文版）

基　　金：supported by 2018-XBQNXZ-A-009 and 2017-XBQNXZ-A-007;by the National Natural Science Foundation of China(Grant Nos.11673055,41531071,11873018,11773061,11790301 and 11973057);the Tianshan Youth funding(Grant 2017Q401);by Key Laboratory of Solar Activity at National Astronomical Observatories,CAS。

摘　　要：Solar radio spikes are one of the most intriguing spectral types of radio bursts.Their very short lifetimes,small source size and super-high brightness temperature indicate that they should be involved in some strong energy release,particle acceleration and coherent emission processes closely related to solar flares.In particular,for the microwave spike bursts,their source regions are much close to the related flaring source region which may provide the fundamental information of the flaring process.In this work,we identify more than 600 millisecond microwave spikes which recorded by the Solar Broadband Radio Spectrometer in Huairou(SBRS/Huairou)during an X3.4 solar flare on 2006 December 13 and present a statistical analysis about their parametric evolution characteristic.We find that the spikes have nearly the same probability of positive and negative frequency drifting rates not only in the flare rising phase,but also in the peak and decay phases.So we suppose that the microwave spike bursts should be generated by shockaccelerated energetic electrons,just like the terminational shock(TS)wave produced by the reconnection outflows near the loop top.The spike bursts occurred around the peak phase have the highest central frequency and obviously weak emission intensity,which imply that their source region should have the lowest position with higher plasma density due to the weakened magnetic reconnection and the relaxation of TS during the peak phase.The right-handed polarization of the most spike bursts may be due to the TS lying on the top region of some very asymmetrical flare loops.

关 键 词：Sun:activity Sun:flares Sun:radio radiation 

分 类 号：P182.52[天文地球—天文学]