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Table of Content

    24 December 1981, Volume 1 Issue 2 Previous Issue    Next Issue
    论文
    A PRILIMINARY STUDY ON MECHANISM OF METAL-SILICATE SEPARATION OF THE TERRESTRIAL PLANETS
    Wang Dao-de;Xie Xian-de
    1981, 1 (2):  85-92.  doi: 10.11728/cjss1981.02.085
    Abstract ( 1410 )   PDF (626KB) ( 1010 )   Save
    It seems reasonable to assume the mechanism of metal-silicate separation between the initial cores and mantles of terrestrial planets during their thermal evolution process as thermal diffusion of Pe-Ni metals in solid state, partial melting of metals and metal-sulfides, and full melting and differentiation of metals, metal-sulfides and silicates. As a result of such metal-silicate redistribution, a small amount of silicate within the initial cores would move to the silicate mantles, and the metal-sulf ide components within the initial rock mantles would gradually sink to the cores, thus forming the final core-mantle struture patterns of terrestrial planets.
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    THE TRANSITIONAL CHARACTERISTICS OF MAGNETOHY-DRODYNAMIC ACCELERATION IN SOLAR WIND FLOW
    Hu Wen-rui
    1981, 1 (2):  93-101.  doi: 10.11728/cjss1981.02.093
    Abstract ( 1408 )   PDF (555KB) ( 936 )   Save
    In this paper, the accelerating feature of solar wind flow from subsonic and sub-Alfven velocity into supersonic and super-Alfven velocity is discussed in the axis-symmetric magnetic flux tube. In addition to the critical sonic line M2=1, there are critical Alfven line MA2=1 and line M2+MA2=1 if the two-dimensional effects of the flow and magnetic field are included. In this case, there is thrice transitions for the solar wind flow in the magnetic flux tube, and the type of the magnetohydrodynamic equations will change from elliptic ones into hyperbolic ones, then the elliptic, and at last, into the hyperbolic ones. The consistent solutions of the magnetohydrodynamic equations for the solar wind flow need to study, because the typical sonic velocity has the magnitude of order just the same as the typical Alfven velocity and the rapid expansion of the magnetic flux tube is interested. There may exist several transitions for solar wind flow in the local flow tube.
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    ON THE STABILITY OF CORONAL MAGNETIC LOOPS
    Chen Le-shan
    1981, 1 (2):  102-110.  doi: 10.11728/cjss1981.02.102
    Abstract ( 1364 )   PDF (539KB) ( 592 )   Save
    In this paper, it is pointed out that in most of the previous works about the stability of coronal magnetic loops, a rigid boundary condition is used (although sometimes without being mentioned) at the edge of a loop, which has a great influence on the result too large to be ignored, even if the pressure gradient is favourable. On the other hand, corona conditions are quite different from that in laboratories. Is it proper to use the rigid boundary condition at the edge of a loop? And what is the mechanism that makes the condition realized? They are still the questions open to further discussions.Besides, if m=1 is stable, according to Newcomb's theorem, it is unnecessary to consider the modes of m> 1; but if it is not stable, it will not be enough to examine m= 1 only. And this article shows that, sometimes, the modes of m > 1 may be more instable.Instead of using a marginal stability analysis such as many authors did, the MHD momentum equation of compressible fluid is used in this paper, so that both the instability region and the growth rate of instability can be obtained at the same time. In addition. the difficulties associated with the singularity in marginal stability analysis could then be avoided.
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    CHARACTERISTIC VELOCITY OF MHD SHOCK
    Zhang Gong-liang
    1981, 1 (2):  111-117.  doi: 10.11728/cjss1981.02.111
    Abstract ( 1806 )   PDF (452KB) ( 1292 )   Save
    According to the similarity between the boundary conditions on the MHD discontinuity and the equations of the MHD simple wave, a physical quantity U* called the characteristic velocity of MHD shock has been introduced. U* is defined by Eq. (4) as the ratio of the jump of total presure p* to that of density p, and equal to the geometric mean value of the shock velocities Wrelative to the up and down streams (Eq. (5)), approaching to the MHD wave velocity Uin the weak shock limit.The system of equations (7) express the shock relations with U* as the strengthparameter, where u, v =H/√4πρ and U± are respectively the velocity of fluid relativeto the shock front, and of the Alfven and the magnetosonic waves. These relations simplify the usual shock calculations and degenerate into the formulae for the MHD simple wave (Eq. (11)) in the infinitesimal jump limit.The fast, slow, and intermediate shock can be distinguished by Eq. (12-a, b, c) respectively. It is interesting to note that the jump formulae (7-a) and (13) show explicitly the transmission relations among the various modes of MHD shock and wave (Eq. (16-a, b, c) for the above three modes respectively), which are nothing but the immediate consequence of the compressive nature of shocks together with the conservation of mass (Eq. (14) and Eq. (15)). However, it needs a lengthy derivation to prove Eq. (16) without introducing U*.
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    REFRACTIVE EFFECTS ON VERY HIGH FREQUENCY RADIO WAVES THROUGH A THREE-DIMENSIONAL INHOMOGENEOUS IONOSPHERE
    Sun Chuan-li
    1981, 1 (2):  118-127.  doi: 10.11728/cjss1981.02.118
    Abstract ( 1352 )   PDF (558KB) ( 863 )   Save
    Ionospheric refraction effects on VHPradio waves play an important role in space technique, such as tracking, navigation, telemetry etc. In theorical range, it has always been supposed that the ionospheric parameters are spherically symmetric except Alpert did in 1963. But Alpert's formulas only contain ionospherically first-order contribution, (ionospherical refraction effects can be expanded as power series in terms of 1/f)In this paper, based on Alpert's work (1963), a new ray diffrencial equations are given aswhere k1=R0 sin ds and ds. From this, it is easy to give expressions of ionospherical refraction effects including higher order ionospheric contribution. In consideration of the complexity of those expressions, only first three order contribution are provided.
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    A METHOD FOR THE DETERMINATION OF THE INTEGRATING CONSTANT OF TOTAL ELECTRON CONTENT
    Jiang He-rong;Song Li
    1981, 1 (2):  128-134.  doi: 10.11728/cjss1981.02.128
    Abstract ( 1359 )   PDF (433KB) ( 726 )   Save
    Amethod is described in this paper for the determination of the integrating constant of T. E. C.. It is based on the variation of the reletive Faraday ratation angle (ΩR) of geostationary satellite signals with the diurnal value f02F2. The regression line of ΩRon f02F2 was calculated by using the least mean squares method. The slope of the regression line is proportinal to ι, the equivalent thickness of the ionosphere, and its interception with the ordinate axis (ΩR) gives Ω0.
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    THE NO+O CONTINUUM AND EXCITATION MECHANISM OF THE OXYGEN GREEN LINE IN THE LOWER THERMOSPHERE
    Tai Hong-sheng
    1981, 1 (2):  135-142.  doi: 10.11728/cjss1981.02.135
    Abstract ( 1394 )   PDF (522KB) ( 583 )   Save
    Acomparison has been made of the discrepancies between the observed NO+O continuum intensities from the horizontal scanning photometer aboard the OGrO-6 and the calculated intensities with Ovalue based on the Chapman excitation mechanism and NOdata from Meira's measurement.These results seem to show an indication that the excitation mechanism of airglow green line could be in accordance with the relation of J∝[O]2 but not J∝[O]3 as in Chapman's mechanism.
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    AN ANALYSIS OF WHISTLER SOURCES
    He You-wen
    1981, 1 (2):  143-152.  doi: 10.11728/cjss1981.02.143
    Abstract ( 1474 )   PDF (583KB) ( 993 )   Save
    By analizing the macrostrueture and electric properties of thunderclouds and lightnings a theoretical study of main observed results of whistler sources, has been made and it has come to a conclusion that lightning producing whistlers are from only certain kinds of different cloud-to-ground lightnings.
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    BIOMEDICAL PROBLEMS OF MANNED SPACE FLIGHT
    Wang Jin-hua
    1981, 1 (2):  153-160.  doi: 10.11728/cjss1981.02.153
    Abstract ( 1426 )   PDF (676KB) ( 640 )   Save
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    WHISTLERS DISPLAY CIRCUIT
    Wang you-shan
    1981, 1 (2):  161-164.  doi: 10.11728/cjss1981.02.161
    Abstract ( 1358 )   PDF (246KB) ( 927 )   Save
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