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Table of Content

    24 June 1981, Volume 1 Issue 1    Next Issue
    论文
    THE ANALYTICAL TRAJECTORY OF THE CHARGED PARTICLE MOVING IN A NEUTRAL MAGNETIC FIELD
    Xu Hong-lan
    1981, 1 (1):  2-14.  doi: 10.11728/cjss1981.01.002
    Abstract ( 1410 )   PDF (982KB) ( 1471 )   Save
    Neutral magnetic field was found wide important applications in space physics and satrophysics[1-4].In a rectangular coordinate system x y and z, the neutral magnetic field is, given by Eq.(2-1), where h is a small northward magnetic field[5], a and e are the parameters of the field.When ε=0 the field is a neutral sheet.An analytical trajectory of the charged particle moving in this field has been calculated The results are:(1)By means of a perturbation method[5], we found that the motion of the charged particle in a neutral sheet field can be defined by the first approximation of motions either in a neutral magnetic field or in a neutral sheet field with a small northward component.The first, second and third approximation of the motion in a neutral magnetic field satify respectively the Eqs.(2-7);(2-8)and(2-9), and in neutral sheet with northward component they satify Eqs.(2-12), (2-13)and(2-14).(2) In the neutral sheet field, the whole region can be devided into a perturba-tion region and non-perturbation region(|x|≤L).Innon-perturbation region, the Alfven’s perturbation method can not be used, the analytical solution of the motion equation(2-7)is given by Eqs.(3-7)and(3-16), where z’ and the drift velocity Vz are given by Eqs.(3-17)and(3-15).In the perturbation region, the anlytical solution of Eq.(2-7)is given by Eqs.(4-8)and(4-22), where z’ and Vz are given by(4-23)and(4-18).The thrid approximation of the analytical trajectory and the trajectory evaluation by computer agree quite well, except for a slight deviation around the boundary of the perturbation region and the non-perturbation region.(3)The trajectory of the particle moving in a neutral sheet field can be devided into two motions, one is along a closed oscillation trajectory in the plane perpendicular with the magnetic field while its center drifts in a direction parallel to the neutral line, and the other along the magnetic line with an uniform velocity.In the non-perturbation region, the closed oscillation trajectory of particles with diference initial conditions are shown in Fig.2 by lines(1), (2), (3), (4)and(5)They are derived from Eqs.(3-7)and(3-17), and take a "8" shape motion.Lines(5), (6), (7)and(8)are derived from Eq.(4-8)and(4-23)in the perturbation region, and take a circular motion.There is a slight deviation between(5)and(5)The drift velocity in non-perturbation region determined by Eq.(3-15)has an opposite direction and a much higher value than that in the perturbation region.The projection of the trajectories on x-y plane corresponds to the particles with different initial conditions are shown in Pigs.1 and 3 by full lines, and the dashed lines denote the founda-mental and higer harmonic of the corresponding trajectories.Acomplete analytical form has been obtained from the above results.
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    THE PROPAGATION OF EXTRA-RELATIVISTIC COSMIC RAY ELECTRON IN THE INTERSTELLAR MEDIUM
    Zhang He-qi;Qu Qin-yue;Wang Zhen-ru
    1981, 1 (1):  15-20.  doi: 10.11728/cjss1981.01.015
    Abstract ( 1372 )   PDF (510KB) ( 1046 )   Save
    In this paper the propagation of cosmic ray e ectrons with energy larger than 1012eV is investigated.Our theoretical calculations show shat the effects of resonant scattering caused by the interstellar hydromagntic waves on the propagation of cosmic ray electrons are very important.On the basis of it the solution of the kinetic equation of cosmic ray electrons leads to the following conclusions:1)Due to the interstellar scattering, the maximum flux of cosmic ray electrons coming from the supernova surces which are in a distance less than 1 kpc from us has not arrived in the earth yet.So the flux of cosmic ray electrons in the neighbourhood of the earth is still in the ascending stage.2)In TeVenergy region, a "dropping phenomena" of the electron energy spectrum is expected.3)The high energy y-ray source observed by SAS-2 may be produced by inverse compton effect through the interaction of cosmic ray electrons with the interatellar radiation fields.Asupport to this suggestion comes from the fact that the dimension of the y-ray source is in agreement with that of cosmic ray electron cloud characterized by the gaussian half width WGi≌(4ξti)1/2ln2 drived in this paper.
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    TEMPERATURE PROFILE AND ALEVEN FLUCTUATION ENERGY FLUX IN CORONAL HOLE
    Zhao Xue-pu
    1981, 1 (1):  21-30.  doi: 10.11728/cjss1981.01.021
    Abstract ( 1379 )   PDF (757KB) ( 889 )   Save
    Based on the assumptions that the propagation of the Alfven fluctuations in coronal holes is undamped and the reasonable coronal temperatures lie in the range 9×105K and 2.5×106K, the propagation characteristics of the Alfven fluctuations in a rapidly diverging flow tube is derived, the acceptable temperature profiles, in a coronal hole are determined and the relerant Alfven fluctuation energy flux density at coronal base obtained as being 5×105 ergs cm-2 sec-1≤FA≤1×106 ergs cm-2 sec-1 are obtained as being it seems reasonable that the acceleration by such Alfven fluctuations as discribed above is effective and sufficient for the coronal plasma to become the high speed wind streams.
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    PROPAGATION EFFECTS OF SOLAR COSMIC RAYS (II)——PROPAGATION CORRECTION OF PEAK SPECTRUM
    Zhang Gong-liang
    1981, 1 (1):  31-40.  doi: 10.11728/cjss1981.01.031
    Abstract ( 1479 )   PDF (912KB) ( 871 )   Save
    The influence of interplaneatry propagation upon the peak spectrum of the solar cosmic say events are discussed in terms of the dimensional solution for the propagation equation with emphasis on the importance of the propagation correction of spectrum.Solar wind convection is one of the probable causes of flattening in low energy spectrum.Under certain conditions, an injected power-law spectrum may change into an observed exponential one, and a kinetic energy spectrum into a rigidity one.The power index of spectrum increases with the magnetic azimuth of source flares, the distribution of which shows a marked east-west asymmetry.Furthermore, the injection spectrum of the relativistic events observed during the 20th solar cycle are evaluated through a correction for the propagation effect, some of the deduced injection spectra may be expressed as a power law with a unitary index, while others are still flattened in the low energy range.
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    IDENTIFICATION OF THE DISCONTINUITIES AT THE MAGNETOPAUSE
    Zhou Guo-cheng(Chow Gou-chon)
    1981, 1 (1):  41-46.  doi: 10.11728/cjss1981.01.041
    Abstract ( 1734 )   PDF (499KB) ( 11841 )   Save
    In this paper we have studied the possibility to identify different types of the magnetopause discontinuities by means of the characteristics of the discontinuities of the magnetic fields, teh bulk flow velocities and the thermaldynamic parameters.This method itself is independent of the normal directions on the magnetopause.The analysis shows that this method may be used to identify several types of the discontinuities which may occur at the magnetopause.
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    AN ANALYSIS OF THE U. S. STANDARD ATMOSPHERE, 1976
    Sun Chao
    1981, 1 (1):  47-51.  doi: 10.11728/cjss1981.01.047
    Abstract ( 2019 )   PDF (371KB) ( 1415 )   Save
    In this note an analysis of USSA 1976 has been made about its physical assumptions and atmospheric tables.The main results are:1.Temperature profile T(Z) may be defined with absolute temperature in full height range without using molecular-scale temperature TM. 2.The elliptical segment of T(Z) will give a sudden heat sink of the order of 10-7J/m3.s at 110 km which is too large.3.It seems the only systematic mistake in atmospheric tables is the coefficient of thermal conductivity.4.Adetailed discussion is given about the possible choices to connect the computations of the homosphere and the upper heterosphere.5.We suggert to introduce CO2 as a component in the upper atmosphere model and lower the computing interface down to 80 km.
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    A STATISTICAL STUDY ON THE RISE TIME AND THE PEAK INTENSITY OF SOLAR PROTON EVENT
    Cheng Dong-yuan;Wu Ji-ping
    1981, 1 (1):  52-56.  doi: 10.11728/cjss1981.01.052
    Abstract ( 1391 )   PDF (406KB) ( 856 )   Save
    This paper intends to put forward a semi-quantitative method of prediction of solar proton events, i.e., to estimate the peak intensity of solar protons and the rise time in which solar protons expense to reaching it’s peak intensity from the onset of the optical flare presumed to have been identified as a proton flare.We had collected and studied statistically the systematic data of solar proton events and associated solar flare and radio burst data published abroad.The statistical results show that the correlation coefficient between the rise time t of solar proton event and the flare heliographic longitude 0 is about 0.87 and the fitting equation is t=18.1-0.39θ+0.0033θ2.Furthmore, the solar radio data of six frequencies(9400, 8800, 4995, 2800, 1415, and 606 MHz)were analysed and fitted to the equation lgP=AlgK+B.Among them, the correlation between the 8800MHz radio parameters and the solar proton intensity is the best.The correlation coefficients between the averge flux, the peak flux and the integrating flux of the 8800-MHz radio-burst events and the peak intensity of solar proton events are 0.70, 0.68 and 0.69 respectively.The coefficients can be raised to 0.77, 0.77 and 0.75 respectively if two large proton events occured in August, 1972 are also considered.Thus, using the corresponding empirical equation, We cam forecast the rise time and the peak intensity of solar proton events from the observed data of the solar flare longitude and the fluxes of the 8800MHz radio burst.
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    THE RELATIONSHIP BETWEEN INDICES AE AND Dst
    Tu Heng;Xie Liu-xiang
    1981, 1 (1):  57-59.  doi: 10.11728/cjss1981.01.057
    Abstract ( 1564 )   PDF (260KB) ( 946 )   Save
    In this paper Data of AEand Dst indices from July 1972 to December 1974 have been analyzed for the correlation between these two indices the correlation coefficient of the data for every half year are between 0.5 and 0.6. As the geomagnetic disturbance level increases, that means when the values of the Dst index decreases the correlation coefficient decreases.Since the Dst index mainly reflect the intensity of the equatorial ring current whereas the AEindex mainly reflect the intensity of the auroral electrojet, the correlation between these two indices may reflect the relationship between these two current systems.The results of the correlative analyses also show that the south-north component of the interplanetary magnetic field have no obvious influence on this relationship.
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    ON THE ENERGY STORAGE IN THE SOLAR ATMOSPHERE BY TWISTING MAGNETIC FIELD
    Liu Xin-ping;Ao Chao
    1981, 1 (1):  60-67.  doi: 10.11728/cjss1981.01.060
    Abstract ( 1439 )   PDF (676KB) ( 893 )   Save
    In this paper a complete set of MHDequations was used to study the energy storage in the solar atmosphere by twisting the tube of magnetic lines of force at the base.By means of numerical method, dynamic evolution of nonlinear, force-free magnetic fields of the solar surface, including the transition region, was investigated.It was assumed that the initial magnetic fields configuration is a potential field;the plasma motions at the feet of lines make magnetic fields in the active regions twisting.Magnetic energy is rearranged in this way much of magnetic energy can be stored in the local regions.Computed results give a quantitative expression for nonlinear force-free fields..These results could explain the energy-storing process of solar flares.
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    METHODS OF COMPUTATION OF GEOMAGNETIC FIELD AT GREATER ALTITUDE IN A LOCAL REGION
    An Chen-chang;Xu Yuan-fang
    1981, 1 (1):  68-73.  doi: 10.11728/cjss1981.01.068
    Abstract ( 1306 )   PDF (464KB) ( 728 )   Save
    In this paper two methods have been given to calculate the geomagnetic fields at great altitudes in a local region.In the first method surface spline is used to express the distribution of the geomagnetic fields and its horizontal gradient on the ground surface, the formulas areThe surface spline can express both normal distribution and anomalous distribution of the geomagnetic fields, and also geomagnetic horizontal gradient, so the use of surface spline makes Zmuda’s method simpler.The other method is with the aid of spherical harmonic analysis of the geomagnetic fields in a local region, the procedure is(1)to compute a set of spherical harmonic coefficients based on the geomagnetic data on the ground surface in a local region, (2)to compute the geomagnetic fields at great altitudes by using these coefficients.
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    A STUDY OF COSMOGENIC NUCLIDES ON METEORITES
    Zhou Xiao-xia;Sung Shao-yi;Li Jui-xiang
    1981, 1 (1):  74-76.  doi: 10.11728/cjss1981.01.074
    Abstract ( 1369 )   PDF (321KB) ( 1033 )   Save
    Astudy of Cosmogenic nuclides in the Kirin meteorite is presented in brief here.The depth distribution of Co60 in four specimens taken at different depths inside the Kirin meteorite No.1 is described in some detail.Finally multiple exposure history of the Kirin meteorite is also discussed.
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    THE ESTIMATE OF PROBABILITY DISTRIBUTION OF THE DOMINANT FREQUENCIES FOR THE LIGHTNING DURING AN ECLIPSE OF THE SUN
    Ling Fu-gen
    1981, 1 (1):  77-81.  doi: 10.11728/cjss1981.01.077
    Abstract ( 1309 )   PDF (413KB) ( 866 )   Save
    In this paper we estimated the probability distribution of the dominant frequencies for the lightning during a total eclipse of the Sun, using the spectral data from 1 It was pointed out that the dominant frequencies may follow a Gaussian(or normal)distribution, and the reliable region of mean and rms for dominant frequencies are 8845 Hz, 10381 Hz and 2485 Hz, 3203 Hz respectively.
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