1983 Vol. 3, No. 1

Display Method:
THE SPIRAL SECTOR TRANSITION REGIONS IN THE INTERPLANETARY MAGNETIC FIELDS
Zhao Xue-pu, J. M. Wilcox, P
1983, 3(1): 1-9. doi: 10.11728/cjss1983.01.001
Abstract(1564) PDF 742KB(1086)
Abstract:
Based on the large-scale configuration of the magnetic fields in the interplanetary space and the possible association of the solar wind flow near the sector boundary crossing with the coronal streamer,it is suggested that in the interplanetary space there might be some spiral sector transition regions which are thicker than the sector boundaries.In situ observations of interplanetary magnetic field and solar wind plasma do show the existence of the spiral sector transition regions.The magnetic strength in the regions does not go to zero for all the 45 cases studied in this work,most of them have the magnetic strength either much higher or much lower than the average of 5γ in the adjecent magnetic sectors.The physical properties in the magnetic depressing (MD) and magnetic enhancement (MB) regions and the possible rauses have also been analyzed and discussed.
THE CHARGED PARTICLE DISTRIBUTION AND THE FORMATION OF ELECTRIC FIELD IN ACCRETION COLUMN OF NEUTRON STAR
Zhang He-qi
1983, 3(1): 10-15. doi: 10.11728/cjss1983.01.010
Abstract(1489) PDF 535KB(1104)
Abstract:
In this paper we establish a set of kinetic equations from Liouville's theorem which can be used to describe the charged particle distribution in the accretion column of a neutron star.Abrief description of the general behavior of the plasma on a accretion column of a neutron star having a very strong magnetic field with a weak inhomoge-neity and with cylindrical symmetry is given.It is pointed out that the inhomogeneous magnetic field seems to have major effect on the plasma and the charged particle distribution in the accretion column greatly depend both on the magnetic field structure and on gravitational field of the neutron star.From the analysis we lead to the following conclusions.(1)The charged particle distribution in the accretion column with a very strong magnetic field is quite different from the one only controled by gravitational field of the neutron star as most of the high energy astrophysicists have done.Sometimes one would expect that the charged particles can be pushed outward along the direction of magnetic field and the matter density will increase with height.(2)Due to the difference in mass between the electron and the proton the distribution of protons with height is different from that of the electrons.So a strong electric field can take place near the surface of a neutron star.The type of electric field depends on the charged particle distribution.(3)For very young neutron stars,the role of the magnetic field may exceed that of the gravitational field.In this case there will be no possibility to form the accretion column and the pulse radiation therefore can not be produced.
THE CHANGE RATE OF ENERGY OF THE TEST ELECTRON CAUSED BY PLASMA TURBULENCE
Liu Zhen-xing
1983, 3(1): 16-22. doi: 10.11728/cjss1983.01.016
Abstract(1396) PDF 558KB(865)
Abstract:
The distribution function of the electron beam moving in the turbulent plasma is given for a definite diffusion coefficient.Using this distribution function and the kinetic equation,we have developed two formulas of change rate of the electron energy.One is the change rate of energy of the electrons with definite velocity de/dt,and the other is the change rate of mean electron energy de/dt.These formulas are more general than the previous formulas used in this field.
SCATTERING AND PRECIPITATING OF PARTICLES OF THE MAGNETOTAIL UNDER THE ACTION OF THE DAWN-DUSK ELECTRIC FIELD
Xu Rong-lan, Gu Shi-fen
1983, 3(1): 23-28. doi: 10.11728/cjss1983.01.023
Abstract(1559) PDF 579KB(835)
Abstract:
We think that scattering of particles of the magnetotail in forming of precipitating particles is very importment.In this paper,the pitch angle changing of charged particles of the magnetotail under the action of the dawn-dusk electric field is studied by evaluating about 900 trajectories by computer.The results show clearly that the charg-ed particles of the magnetotail under the action of the dawn-dusk electric field undergo evident scattering process.The particles of the magnetotail which move through the nonperturbation region are reflected many times inside the nonperturbation region,the magnetic moment is no longer invariant,and when they leave the nonperturbation region,their pitch angles are changeable.This change makes isotropic initial pitch angles distribution change into a Maxwellian state,when the particles are away from the neutral line and enter into the region of near earth.The space career of these particles are also studied,and it is found that they undergo space separation (dawn-dusk separation,latitude separation and a relative separation between the protons and electrons) when they leave the magnetotail and enter into near earth with the clear precipiting pattern of the particles.
THE SPACECRAFT OBSERVATIONS OF THE POSITION OF MAGNETOPAUSE
Zhuang Hong-chun, G. T. Eussell
1983, 3(1): 29-35. doi: 10.11728/cjss1983.01.029
Abstract(1439) PDF 751KB(673)
Abstract:
1024 magnetopause crossing data from 1963 to 1979 are used to calculate the ellipsoid of the dayside magnetopause surface.An attempt is made to search for the effects of the interplanetary magnetic field and solar wind thermal pressure on the position and shape of the dayside magnetopause.The uncertainties in the determination of the parameters of the ellipsoid from various sources are analyzed.Both numerical results and theoretical analyses show that the accuracy of the data available is not adequate enough to see the effects.Some suggestions are proposed for further work.Observations of the average values of the size,shape and orientation of the dayside magnetopause agree quite well with the theoretical prediction.
THE RELATION BETWEEN THE ONSET TIMES OF THE NEGATIVE PHASE OF IONOSPHERIC STORMS AND THE MAIN PHASE OF MAGNETIC STORMS AND A THEORETICAL MODEL
Tu Chuan-yi
1983, 3(1): 36-43. doi: 10.11728/cjss1983.01.036
Abstract(1395) PDF 712KB(1056)
Abstract:
In this paper,major negative phase ionospheric storms occurred from 1969 to 1973 at Manchouli (49.5°N,117.5°E),Billerica (43°N,71.5°W) and Freiburg (48°N,07°E) are analyzed.It is found that if the associated magnetic storm main phase being around noon,the ionospheric storm negative phase begins in the afternoon at Billerica station and at Freiburg station,but the negative phase begins around midnight at Manchouli station.Athearetical model is presented to calculate the negative phase onset time.The model is based on two extended heat sources,one is on the day side of the auroral oval and the other on the night side.When the magnetic storm main phase begins,the molecule enriched air appears at the heat sources.The air is brought to the middle latitudes by the thermospheric winds and the electron loss rate there increases.This gives rise to the occurrence of the negative phase ionospheric storms.The onset times of negative phase is calculated,and the results agree rather well with those of statistics.
THE MORPHOLOGY AND OCCURRENCE OF Es-s OVER WUCHANG,CHINA
Wang Shen, Huang Xin-yu, Tan Zi-xun
1983, 3(1): 44-50. doi: 10.11728/cjss1983.01.044
Abstract:
The occurrence and morphology of ionospheric Es-s over Wuchang,China,are examined and statistically analysed.The Es-s over this area is possessed of high occurrence and clear trace.We consider that Es-s is neither an intrinsic companion of magnetic disturbances,nor a phenomenon existing exclusively in the auroral zones and in the geomagnetic equatorial region. Over this area,Es-s occurred mostly in magnetic quiet days,and the maximum of occurrence rate is arround 09h or 10h LMT diurnally and in summer months seasonally.No effect on this feature due to variations of geomagnetic field or solar activity has so far been detected.
STATISTICAL ANALYSIS OF THE PLASMA COMETS
Li Zhong-yuan, Gu Shun-yong
1983, 3(1): 51-57. doi: 10.11728/cjss1983.01.051
Abstract(1372) PDF 631KB(1150)
Abstract:
In this paper,a statistical analysis by which the comets are classified is presented.The relationship between the solar activity and the occurrence frequencies of the plasma comets is discussed.The analysis shows that the correlation of cometary events with the solar activity is weak,but obviously,the cometary events correlate to the velocity of the solar wind.Finally,the aberration angle and its kinked effect are discussed,it is quite clear and definite that they both correlate with the solar wind.
A STATISTICAL STUDY OF THE RELATION BETWEEN SOLAR FLARE AND GEOMAGNETIC DISTURBANCE FOR 1966-1978
Zhang Gong-Hang, Lu Chen
1983, 3(1): 58-66. doi: 10.11728/cjss1983.01.058
Abstract(1440) PDF 824KB(1041)
Abstract:
This paper provides a set of curves for the variation of various geomagnetic indices,Ap,AE,Dst and Kp initiated by solar flares grouped by their optical importance,duration,and the distance from the central meridian.Fig.1 and 2 show that both the duration and optical importance are good criteria for the geomagnetically-effective flares.Statistically,only the major flares of importance 3 or that of importance 2 but with duration ≥1.5 hours can significantly disturb the geomagnetic field onto the levels of Kp≥4.For these major flares,brightness plays an important role in determing both the intensity and the character of the resulted disturbance.In general,the bright major flares affect the Ap,AE,and Dst indices,onto Kp≥4,while the normal or faint ones result in significant disturbance of the AEindex limited to Kp-4 or 5 only.It can be shown from Fig.3 that there are two kinds of the east-west asymmetry in the distribution of flare's position in response to the geomagnetic disturbance.Statistically,the disturbance in Ap and Dst indices intensified onto Kp≥6 are related mainly to the flares situated between30°Eand 60°W,whereas the occurrence frequency of the disturbance with intermediate intensity of Kp=4 or 5 increases when the flare goes from the east to the west of the central meridian,peaking at 60°-90°W.The disturbance of AE index has bath the above asymmetries.Also,there are some indications of the dependence of the intensity of geomagnetic disturbance upon the sun-earth propagation velocity of the flare ejecta,which may be sped up when the flare goes from the east to the west of the central meridian.These results reflect the complex nature of the interplanetary disturbance produced by solar flares,which are under study and will be published elsewhere.
THE REFLECTION AND TRANSMISSION OF ELECTROMEGNETIC WAVES FROM THE LOSSY PLASMA MOVING PARALLEL TO THE INTERFACE
Liu Tieh-chiin
1983, 3(1): 67-71. doi: 10.11728/cjss1983.01.067
Abstract(1476) PDF 344KB(860)
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In this paper,by using the method of the relativistic theory,the expressions of the reflection and transmission coefficients of electromagnetic waves for a lossy plasma moving parallel to the interface are derived.It is shown that the reflected and transmitted fields are dependent on the velocity of the moving plasma if the collision are taken into account.If the collision is negligible,the result is identical with one derived by Yeh,C..In normal incident case,contrary to oblique incidence the reflected and transmitted fields are independent on the velocity of the moving plasma.
THE APPLICATION OF THE PHYSICAL PARAMETER METHOD IN THE SOLAR X-RAY TELESCOPE——THE EXACT MEASUREMENT OF THE CORONAL PLASMA PARAMETERS
Han Zheng-zhong, Pan Da-xion, Lin Chun-mei
1983, 3(1): 72-77. doi: 10.11728/cjss1983.01.072
Abstract(1475) PDF 448KB(816)
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The application of the physical parameter method in the solar X-ray telescope is discussed in this paper.The method is described principally,and the calculation results are given.Analysis and calculations show that the energy densities of different structure in the solar corona can be measured quantitatively and directly by the method,and the results are more accurate than the filter ratio method.
MEASUREMENT OF CHARGE COMPOSITION OF PRIMARY COSMIC RAY USING CR-39 PLASTIC TRACK DETECTOR
Ren Guo-xiao, Zhou Yin-zao, Huang Rong-qing
1983, 3(1): 78-81. doi: 10.11728/cjss1983.01.078
Abstract(1350) PDF 280KB(884)
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