Concerning spikes in emission and absorption in the microwave range  

作　　者：Gennady P.Chernov Robert A.Sych Guang-Li Huang Hai-Sheng Ji Yi-Hua Yan Cheng-Ming Tan 

机构地区：[1]Key Laboratory of Solar Activity,National Astronomical Observatory,Chinese Academy of Sciences [2]Pushkov Institute of Terrestrial Magnetism,Ionosphere and Radio Wave Propagation,Russian Academy of Sciences (IZMIRAN) [3]Institute of Solar-Terrestrial Physics [4]Purple Mountain Observatory,Chinese Academy of Sciences

出　　处：《Research in Astronomy and Astrophysics》2013年第1期115-128,共14页天文和天体物理学研究（英文版）

基　　金：supported by the Ministry of Education and Science of theRussian Federation;supported by the Chinese Academy of Sciences Visiting Professorship for Senior International Scientists (Grant Nos. 2011T1J20 and 2010T2J24);supported by the Russian Foundation of Basic Research (RFBR,GrantNos. 11-02-00757,11-02-91151,10-02-00153,12-02-91161-GFEN and FP7-PEOPLE-2011-IRSES);The National Basic Research Program of the Ministry of Science and Technology of China(Grant No. 2006CB806301);CAS-NSFC Key Project (Grant No. 10778605) support the Chinese

摘　　要：In some events, weak fast solar bursts （near the level of the quiet Sun） were observed in the background of numerous spikes in emission and absorption. In such a case, the background contains the noise signals of the receiver. In events on 2005 September 16 and 2002 April 14, the solar origin of fast bursts was confirmed by simultaneous recording of the bursts at several remote observatories. The noisy background pixels in emission and absorption can be excluded by subtracting a higher level of continuum when constructing the spectra. The wavelet spectrum, noisy pro- files in different polarization channels and a spectrum with continuum level greater than zero demonstrates the noisy character of pixels with the lowest levels of emission and absorption. Thus, in each case, in order to judge the solar origin of all spikes, it is necessary to determine the level of continuum against the background of which the solar bursts are observed. Several models of microwave spikes are discussed. The electron cyclotron maser emission mechanism runs into serious problems with the in- terpretation of microwave millisecond spikes： the main obstacles are too high values of the magnetic field strength in the source （Pe 〈 uB）. The probable mechanism is the interaction of plasma Langmuir waves with ion-sound waves （l ＋ s → t） in a source related to shock fronts in the reconnection region.In some events, weak fast solar bursts （near the level of the quiet Sun） were observed in the background of numerous spikes in emission and absorption. In such a case, the background contains the noise signals of the receiver. In events on 2005 September 16 and 2002 April 14, the solar origin of fast bursts was confirmed by simultaneous recording of the bursts at several remote observatories. The noisy background pixels in emission and absorption can be excluded by subtracting a higher level of continuum when constructing the spectra. The wavelet spectrum, noisy pro- files in different polarization channels and a spectrum with continuum level greater than zero demonstrates the noisy character of pixels with the lowest levels of emission and absorption. Thus, in each case, in order to judge the solar origin of all spikes, it is necessary to determine the level of continuum against the background of which the solar bursts are observed. Several models of microwave spikes are discussed. The electron cyclotron maser emission mechanism runs into serious problems with the in- terpretation of microwave millisecond spikes： the main obstacles are too high values of the magnetic field strength in the source （Pe 〈 uB）. The probable mechanism is the interaction of plasma Langmuir waves with ion-sound waves （l ＋ s → t） in a source related to shock fronts in the reconnection region.

关 键 词：solar flare -- radio emission -- spike-bursts 

分 类 号：P182[天文地球—天文学]