Loading...
中文核心期刊
CNKI期刊全文数据库
中国科学引文数据库(CSCD)源期刊
中国科技论文统计源期刊
万方数据知识服务平台
英国《科学文摘》(SA)
美国化学文摘(CA)
俄罗斯《文摘杂志》(AJ)
德国《天文学与天体物理学文摘》(AAA)
英国《中国天文学和天体物理学》(SCI收录)全文摘译期刊之一
《中国学术期刊文摘》
《中国物理文摘》
《中国天文学文摘》

Table of Content

    24 January 1982, Volume 2 Issue 1 Previous Issue    Next Issue
    论文
    A STATIC STRUCTURAL MODEL OF THE OUTER MAGNETOSPHERE OF JUPITER
    Liu Zhen-xing
    1982, 2 (1):  1-11.  doi: 10.11728/cjss1982.01.001
    Abstract ( 1325 )   PDF (756KB) ( 881 )   Save
    In this paper the ideal-state MHDequations are solved: the results show that there are two kinds of relationship between the variables and Z (the distame from equator) in the plasma sheet.One is a hyperbolic function,while the other is a trigonometric function.Observations would seem to agree with the hyperbolic function.Simple distribution formulas of pressure,density,temperature,magnetic field and current density in the plasma sheet are deduced.The relationship between the variables and radial distance r are: Po(r)~r-3.4,jo(r)~r-1.7. For an adiabatie proceess,po(r)~r-2.04,To(r)~r-1.36.For an isothermal process,po(r)~r-3.4,T=constant.Finally,the influences of the magnetic anomaly on the outer magnetosphere are dicussed.
    Related Articles | Metrics
    THE EQUILIBRIUM CONFIGURATION OF THR CORONA LOOP AND THE CORONA ARCHIDE
    Hu Wen-rui
    1982, 2 (1):  12-20.  doi: 10.11728/cjss1982.01.012
    Abstract ( 1510 )   PDF (810KB) ( 1006 )   Save
    Under the assumption of linear field,the equation of the two-dimensional configuration of corona loop or the corona archide may be given as Δψ+G(dG/dψ)=-4π(dp/dψ), which is solved by using the method of Foriour transformation.The analytical solution is applied to explain the observational results.The theoretical results show that the pressure should be uniform along the-loop,and the configuration of the loop is more stable than that of the force free field.The influence of the shear magnetic field and the pressure on the configuration are also discussed.More magnetic energy of shear or twisted magnetic field may be stored in the loop,the corona loop will be driven to produce the corona transient process or the plasma will be heated or accelerated to produce solar flares if part of the stored energy is released.
    Related Articles | Metrics
    PLASMA CURRENT SHEET STUDIED BY MEANS OF PARTICLE MOTION
    Xu Rong-lan
    1982, 2 (1):  21-30.  doi: 10.11728/cjss1982.01.021
    Abstract ( 1264 )   PDF (785KB) ( 1376 )   Save
    In this paper,we studied a one-dimensional plasma current sheet by means of the regular pattern of motion of charged particles moving in a neutral sheettmagnetic field.Aguiding centre theorem similar to that of Alfven's was used,the "8" shaped motion in non-perturbation region (where the magnetic field is small or equal to zero) is divided into two "circular" motions.Bach circular motion is equivalent to a magnet.So the "8" shaped motion is equivalent to two magnets in opposite directions.The electric current of plasma is derived from j=en+c(这里有图片19820103-21-1.GIF)×M where the distribution function of plasma is a function of constant motion.We found that the current sheet is mainly due to the "inverse drift" motion in the non-perturbation region.We have also studied the relation between charged particle motions and the magnetic field,and derived a self-consistent magnetic field.
    Related Articles | Metrics
    PERIODIC OSCILLATION IN SOLAR RADIO EMISSION PRECEDING MICROWAVE BURST
    Wu Hong-ao
    1982, 2 (1):  31-37.  doi: 10.11728/cjss1982.01.031
    Abstract ( 1321 )   PDF (720KB) ( 896 )   Save
    In this paper we have analysed the burst data at 3.2cm and 10cm during the period January to December,1979.The bursts that the peak flux density increase-ment (S/S)≥50% amount to 25 and we find that there are oscillations on the preburst recording curves of all the 25 bursts,the period of the oscillation is from a few seconds to ten seconds and the amplitude is about 1% of the solar undisturbed component.Such a oscillation usually precede burst for a few hours or a few days,but for outstanding burst it will be disappeared for tens minuts or a few hours before burst,and without this phenomenon in smaller,impulsive and shorter complex bursts.Thus the oscillating characteristics may be a process of energy accumulation in flare region.
    Related Articles | Metrics
    THE OBSERVED CHARACTERISTICS OF A RADIO OUTBURST ON THE SOLAR LIMB
    Zhou Ai-hua;Sun Jiu-zhen;Gu Zhong-yuan
    1982, 2 (1):  38-43.  doi: 10.11728/cjss1982.01.038
    Abstract ( 1328 )   PDF (536KB) ( 1038 )   Save
    The observed characteristics of the radio outburst occurred on the solar limb at 0808UT April 27,1981 have been gived in details.The morphology of the radio burst,the spectra of microwave burst and the energy spectra of non-thermal electrons have been analysed primarily.
    Related Articles | Metrics
    KELVIN-HELMHOLTZ INSTABILITY IN BOUNDARY LAYER REGIONS OF THE PLASMA SHEET DURING MAGNETOSPHERIC SUBSTORM RECOVERY
    Zhou Guo-cheng;Wu Hong-zhong
    1982, 2 (1):  44-51.  doi: 10.11728/cjss1982.01.044
    Abstract ( 1469 )   PDF (665KB) ( 665 )   Save
    The Kelvin-Helmholtz instability in boundary layer regions of the plasma sheet during magnetospheric substorm recovery is studied based on two idealized MHDmodels.One model consists of three uniform plasma regions-the tail lobe,the plasma sheet,and the south tail lobe.In this model the unstable mode is excited at the boundary surface between the north (or south) tail lobe and the plasma sheet.The other model consists of five uniform plasma regions-the north tail lobe,the north boundary layer of the plasma sheet,the middle layer of the plasma sheet,the south boundary layer of the plasma sheet,and the sorth tail lobe.There are two unstable modes in boundary layer regions of the plasma sheet:one is excited at the boundary surface between the north (or south) boundary layer and the middle layer of the plasma sheet (Mode-I) and the other is excited at the boundary surface between the north (or south) boundary layer of the plasma sheet and the north (or south) tail lobe (Mode-II).Mode-Iis unstable most of the time.These unstable modes may cause some features of boundary layer regions of the plasma sheet observed oil satelittes.
    Related Articles | Metrics
    PROPAGATION EFFECT ON INTERFEROMETER
    Han Wen-jun
    1982, 2 (1):  52-62.  doi: 10.11728/cjss1982.01.052
    Abstract ( 1388 )   PDF (891KB) ( 603 )   Save
    From three aspects——atmospheric refraction,effect of secondary waves andscreen effect between antennas located at each terminal of the base line,we discussed the propagation effect on interferometers with various lengthes of base line.According to the result calculated with some typical parameters,we obtained the following conclusions:1.Horizontal inhomogenity of the troposphere and that of the ionosphere are the main causes to produce the maximum relative excess path difference for shorter and longer (especially for VLBI) base line respectively,but it is mainly due to the maximum initial elevation angle difference between two terminals of the base line,for longer base line at low elevation angle.Prom the point of view that phase errores were not larger than 20°,the characteristics of the synthesized beam would not be influenced,the atmospheric refraction effect on interferometer with base line shorter than 1 km can be neglected.2.According to the accuracy of atmosphere measurement and the statistical distribution of maximum horizontal gradient of atmospheric inhomogenity,we know that the minimum spatial coherent scales are about 10 km and 400 km for troposphere and ionosphere respectively,the minimum temporal coherent scale is about 1/2 Hr.for both.So that,it is unreasonable to correct the atmospheric refraction by utilizing atmospheric model with poor accuracy,for interferometer with base line shorter than 10 km.3.In the presence of ground reflected wave,there will be introduced an phase difference error,Δφ.For VLBI the maximum of which is determined by the reflection coefficients,Ar at each terminal of the base line,that is,(Δφ)max=sin-1 Ar1+sin-1Ar2 For shorter base line,because of unequal heights of the antennas relative to each reflecting plane,Δφmay be large at low elevation angle,but it is reduced at high elevation angle by the reduction of the equivalent reflection coefficient from the secondary beam effect of the antenna.4.The larger the ratio of the diameter of the parabolic antenna,da to the base line's length,D,and that of the wave length,λ,to D are,the larger the diffraction loss due to defect of the Fresnel's clearance is.But from the example calculated with (da:D)max=(9:12),and λ=1.293m,onr result is that the diffraction loss is less than 1 db.
    Related Articles | Metrics
    THE BLAST WAVE PROPAGATING IN A MOVING MEDIUM WITH VARIABLE DENSITY
    Wei Feng-si
    1982, 2 (1):  63-72.  doi: 10.11728/cjss1982.01.063
    Abstract ( 1469 )   PDF (786KB) ( 1189 )   Save
    The blast wave propagating from a point source in a moving medium with variable density has been treated.On the basis of the analytical solutions obtained by the paper some important characteristics of the flare-generated shock waves propagating in the Solar wind are discussed.It is found that the 1AUregion is just a transitional region of various important effects of the flare-generated shock waves; the equivalent power of the deceleration of Shock wave (D=K(uo,Es)R-t(uo,Es,R) is the function of Selar wind velocity uo,Shock wave energy Es and Shock's propagation distance R,usually i<1/2 and the convection effect of Solar wind is very important when R>1AU,due to this effect a stronger Shock wave could propagate to the 10-20 AU beyond,it consists with the recent observations of the space-crafts Pioneer 10 and 11.
    Related Articles | Metrics