The contour maps at 17 GHz on the 1992 October 27 solar burst are analysed.Using a nonthermal inhomogeneous model of the radio source,the variations of calculated source size with time are basically consistent with th...The contour maps at 17 GHz on the 1992 October 27 solar burst are analysed.Using a nonthermal inhomogeneous model of the radio source,the variations of calculated source size with time are basically consistent with the observation of maps.The variations of calculated brightness temperature with a distanceρdisplaced from the project center are in better agreement with the observation of map at 01:45:29:889 UT.The calculation shows that the characterizing magnetic field gradientαB at the peak of 17 GHz is about 2,magnetic strength B is about 737G with the magnetic field Bm of the core being 2000 G.However in order to measure the coronal magnetic field accurately,it is necessary to obtain radio-imaging data at more frequencies.展开更多
We discuss Whether the numbers of x-ray and radio-produced electrons in solar flares are the same.The number of the radio-produced electrons that is estimated with an inhomogeneous source increases by a factor of 10^(...We discuss Whether the numbers of x-ray and radio-produced electrons in solar flares are the same.The number of the radio-produced electrons that is estimated with an inhomogeneous source increases by a factor of 10^(3)-10^(4) because of the inhomogeneity and the decreased magnetic field(B=120 G)of the radio source.The number of the x-ray-produced electrons decreases by a factor of 10-30 due to the increase of the number density of ions(3 × 10^(10)cm^(-3)).These are the reasons why the number of radio-produced electrons is approximately equal to that of x-ray produced in the 1981 April 27 burst.展开更多
The solar radio inverted-U bursts are named after their shape of an inverted letter Uon the spectrograph records.They are important in the study of the corona mass ejectionand particle acceleration in solar flares.Up ...The solar radio inverted-U bursts are named after their shape of an inverted letter Uon the spectrograph records.They are important in the study of the corona mass ejectionand particle acceleration in solar flares.Up to now,most U bursts occur at frequenciesbelow 0.5 GHz;only one exception was reported in the 1.1—1.7 GHz frequency band.Inthis note,we investigate a U burst in the 1.0-2.8 GHz frequency band(figs.1,2),展开更多
The solar radio spectra of the gyro-synchrotron radiation without absorption from mildly relativistic non-thermal electron have been presented using the model with the spherical symmetric nonhomogeneity.These spectra ...The solar radio spectra of the gyro-synchrotron radiation without absorption from mildly relativistic non-thermal electron have been presented using the model with the spherical symmetric nonhomogeneity.These spectra have the following features: (i) Twists and turns of the spectra,which appear at the joint between the medium and high frequencies,(ii) Flux density drop at the lower frequencies.Even if there are no absorption in the radio sources,flux density drop at the lower frequencies is still present because of magnetic nonhomogeneity.(iii) These theoretical spectra belong to C type.This provides us a new interpretation for the observed solar burst C type spectra.展开更多
基金Supported by the National Natural Science Foundation of China under Grant No.19833050the Jiangsu Natural Science Foundation(BK97207)the 95 Major Project of Chinese Academy of Sciences.
文摘The contour maps at 17 GHz on the 1992 October 27 solar burst are analysed.Using a nonthermal inhomogeneous model of the radio source,the variations of calculated source size with time are basically consistent with the observation of maps.The variations of calculated brightness temperature with a distanceρdisplaced from the project center are in better agreement with the observation of map at 01:45:29:889 UT.The calculation shows that the characterizing magnetic field gradientαB at the peak of 17 GHz is about 2,magnetic strength B is about 737G with the magnetic field Bm of the core being 2000 G.However in order to measure the coronal magnetic field accurately,it is necessary to obtain radio-imaging data at more frequencies.
基金Supported by the National Natural Science Foundation of China under Grant No.19833050the Jiangsu Natural Science Foundation(BK97207)the 95 Major Project of Chinese Academy of Sciences.
文摘We discuss Whether the numbers of x-ray and radio-produced electrons in solar flares are the same.The number of the radio-produced electrons that is estimated with an inhomogeneous source increases by a factor of 10^(3)-10^(4) because of the inhomogeneity and the decreased magnetic field(B=120 G)of the radio source.The number of the x-ray-produced electrons decreases by a factor of 10-30 due to the increase of the number density of ions(3 × 10^(10)cm^(-3)).These are the reasons why the number of radio-produced electrons is approximately equal to that of x-ray produced in the 1981 April 27 burst.
基金Project supported by the National Natural Science Foundation of China.
文摘The solar radio inverted-U bursts are named after their shape of an inverted letter Uon the spectrograph records.They are important in the study of the corona mass ejectionand particle acceleration in solar flares.Up to now,most U bursts occur at frequenciesbelow 0.5 GHz;only one exception was reported in the 1.1—1.7 GHz frequency band.Inthis note,we investigate a U burst in the 1.0-2.8 GHz frequency band(figs.1,2),
基金Project supported by the National Natural Science Foundation of China.
文摘The solar radio spectra of the gyro-synchrotron radiation without absorption from mildly relativistic non-thermal electron have been presented using the model with the spherical symmetric nonhomogeneity.These spectra have the following features: (i) Twists and turns of the spectra,which appear at the joint between the medium and high frequencies,(ii) Flux density drop at the lower frequencies.Even if there are no absorption in the radio sources,flux density drop at the lower frequencies is still present because of magnetic nonhomogeneity.(iii) These theoretical spectra belong to C type.This provides us a new interpretation for the observed solar burst C type spectra.
