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Chun-Sheng Li and Shu-Ying Jiang · about 5 minutes
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N87-21793 STATISTICAL ANALYSIS OF FAST HARD X-RAY BURSTS BY SMM OBSERVATIONS AND MICROWAVE BURSTS BY GROUND-BASED OBSERVATIONS Li Chun-sheng and Jiang Shu-ying Astronomy Department Nanjing University Nanjing, China I. Data and Method of Analysis In order to understand the relationship between fast hard X-ray bursts (fIXRB) and microwave bursts (NWB), we have used the data published in the following publications. Io NASA Technical Memorandum 84998. The Hard X-Ray Burst Spectrometer 2. Solar Geophysical Data (1980-i983). Event Listing 1980, 1981 and 1982. Academia Sinica 3. Monthly report of Solar Radio Emission. Toyokawa Observatory, Nagoya University (1980-1983). 4. NASA and NSF: Solar Geophysical Data (1980-1983). We get the data of fast HXRB detected with time resolutions of I0 ms, 5 ms, and I ms and corresponding data of MWB observed (with a time constant of 1 s) at frequencies of 17GHz, 9.4 GHz, 2.75 GHz, and 2.8 GHz during the same flare-burst event. For analyzing individual events, the criterion of the same event for HXRB and MWB is determined by the peak time difference. T = ITmw - Thx I < 20 seconds The regression relation between the physical parameters of MWB and HXRB may be written as: Y=A+BX 85
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where X indicates the logarithm of the following parameters: peak flux density Sp, total flux density St, and duration T'mw of MWB. Y indicates the logarithm of the corresponding parameters: peak rate Cp, total counts Ct, and duration T'hx of HXRB. B is the regression coefficient A is the regression constant Sp is in s.f.u. St = S.T'mw, S = the mean flux T'mw in seconds Cp in counts per second Ct in counts Thx in seconds 2. Results and Conclusions density With the method of data analysis mentioned above, we obtain the results presented in Table 1 and Figures I to 4. In Table i, the parameters have the following meanings: R is the correlation coefficient between X and Y for the energy range of channels I to 15 (i.e. 25-500 keV) R1 is the correlation coefficient for the energy range of channels 1 to 5 (i.e. 25-140 keV) R2 is the correlation coefficient for the energy range of channels 6 to 15 (i.e. 145-500 keV). The statistical analysis run so far and the comparisons of correlation parameters with one another clusions: I. There is a good linear correlation MWB and fast HXRB. allow us to draw the following conbetween the physical parameters of 2. Comparison of R, RI and R2 at different frequencies for MWB show the best correlation coefficients occur at 9.4 GHz. . R2 is larger than R1 at any frequency. This means that the correlation between X and Y is closer in the higher energy range of 145-550 keV than that in the energy range of 25-140 keV at the same frequency. 4. Correlation coefficients between others, but they increase as the T'mw and T'hx are not as good as the frequency decreases. 86
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0 0 0 O000 ,--_ 0 o 000 bO J-J 0 0 ..a 00 o4 0 -,--I .t-4 4J I,-a 0 4.1 .Z: 0 ¢%1 t'_ (DO e_ u,-i 0 o u u_o 0 0 0 0 0 4-1 c_ ,-4 ,"=4 ,0 i ¢_ ) m oO ,-_ C. oO O0 0 0 0 1" 00 000 dg_; u'_ 00 cO u'_ c',4 p-., P,., 00 o ;o u' u_O Of'. O0 ;o o ,. ¢1 00 ,-. c_ 0 .--_ ,--I ,.O ,-..# *'.-I u_ 0 0 ~1__ _ N ,,1_ ._ 0 em ¢xl 87 000 .) .' r,3 r,,.) ._ II
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8: - , LARGE RADIO BURSTS -- M '''" 2.84 GHz II . 6-- m _ 0800 Figure I: Time profiles of radio 0900 1000 U.T. bursts at 2.84 GHz and hard X-ray bursts during the large solar flare of May 16, 198l. 3 2 LOG Sp 1 I ! I I • 0 1 2 3 4 Figure 2: Correlation diagram between peak flux Sp at 9.4 GHz and hard X-ray intensity Cp (in 25-500 keY. 88 counts/s) in the energy range of
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LOGC. 6.(_ 5.0 4.0 . • o oe _ • • o0 • • ° °, • t • • • _ • ° po wt • • • . 4 ° • • • • °s | • ° ° • • 3.0 • " • // 2.0 I, I 2.0 3.0 Figure 3: Correlation diagram between LOG Sp I I 4.0 5.0 peak flux Sp at 3.7 GHz and hard X-ray intensity Cp (in counts/s) in the energy _ of 25-500 keV. 89
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LOG Cp 5.0 4.0 i 0o o • • • • e ° • e ° e 3.0 • • • °" D • • • e" e_oe ° • • • • oe . 0 • .o ° • e. _ 2.0 • e jl ° I I 1.0 2.0 "_ • I I 3.0 4.0 LOG Sp Figure 4 : Correlation diagram between peak flux Sp at 17 GHz and hard X-ray intensity Cp 25-500 keV. (in counts/s) in the energy of 90
