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Table of Content

    24 January 1985, Volume 5 Issue 1 Previous Issue    Next Issue
    论文
    Factors for Incompleteness of QSO's Sample and V/Vmax Analysis
    Liu Zu-wei;Zhang He-qi
    1985, 5 (1):  1-10.  doi: 10.11728/cjss1985.01.001
    Abstract ( 1378 )   PDF (684KB) ( 648 )   Save
    The V/Vmax analysis is a powerful method to study quasar density distribution and luminosity evlution, but the observed sample N(>lmin, <zn) can not be regarded as complete when used to investigate the density law in the range of z<zN and intrinsic luminosities of different sources in the sample are different, so that, to a certain extent, the results of usual procedure are not reliable enough. We present an idea that the quasar L-z curve, from which the deviation of actual sources obeys a certain probability distribution, can be obtained by statistics, and then, the incompleteness factor K(z|lmin)for each source can be given. In this paper we adopt the regression iteration procedure with censored data, assuming deviation of quasar sources from L-z curve follows normal distribution approximately, and analyze the SCRand 4Csamples. On 90% confidence level the space density distribution of quasars is relative to q0 For q0=0, quarsar are close to homogeneous distribution. For q0=1/2, the quasar number increases slightly with the increase of redshift. Only for q0=1, quasars have a strong cosmological evolution. The value of 2 to 6 of the parameter r of density law in the case q0=1 is smaller than that of 10 to 12 derived by previous V/Vmax test, so it is relatively more consistent with the theoretical model to explain quasar form and density evolution in virtue of low density of intergalactic medium. The 3CR sources detected in X-ray are also analyzed, which shows our revised method with incompleteness factors can characterize the sample in different wave band regions.
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    An Analysis for X-ray Flare on July 14, 1980 and Its Comparison with the Hα Flare
    Xu Ao-ao;Tang Yu-hua
    1985, 5 (1):  11-18.  doi: 10.11728/cjss1985.01.011
    Abstract ( 1367 )   PDF (524KB) ( 625 )   Save
    An investigation for the flare on July 14, 1980, is presented by using the Hα patrol observational data in A. R. obtained at Yunnan Observatory and X-ray data from SMM. Our comprehensive analyses for the flare contain the following items: determining its position at Ha; making a positional comparison at Hα and X-ray wavelengths; getting the energy spectra of X-ray bursts; determining the change of spectral index with time; calculating the total number of accelerating high energy electrons during its eruption and approaching the radiative mechanism of soft and hard X-ray bursts. The results show that: (17 the hard X-ray burst is produced by high energy non-thermal electrons accelerated in the current sheet; (2) the soft X-ray burst is produced by hot bremss-trahlung rediation of high-temperature plasma in the flare at first, then hot bremss-trahlung radiation is gradually replaced by bremsstrahlung one of non-thermal electrons; (3) when the comparison of positions between Hα and X-ray images is used to estimate the. altitude of the X-ray burst source, the flare model and the configuration of magnetic field must be considered. They all support Emerging Magnetic Flux mo-del[8] (EMFmodel) of flare process.
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    Distributions of the Magnetic Field Fluctuation Characteristics in the Earth's Magnetosheath
    Wei Feng-si
    1985, 5 (1):  19-26.  doi: 10.11728/cjss1985.01.019
    Abstract ( 1337 )   PDF (554KB) ( 960 )   Save
    The distributions of the magnetic field fluctuation characteristics near the ecliptic plane in the magnetosheath are discussed by using the MHDmodel for describing variations of the interplanetary magnetic field fluctuations across a shock wave. The main results are: (1) the fluctuation intensity and fluctuation anisotropy of the interplanetary magnetic field are amplified obviously in the magnetosheath region; (2) when the interplanetary magnetic field is in the ecliptic plane, the magnetic field fluctuation characteristics (intersity, relative fluctuation and anisotropy and so on) show a dawn-dusk asymmetry, namely, the dawn-side (quasi-parallel shock wave) is more remarkable than the dusk-side (quasi-perpendicular shock wave) obviously; (3) the distribution characteristics are controled strongly by the directions of the interplanetary magnetic field, the dawn-side more sensitive than the dusk-side, relatively speaking, the magnetic activity of the dusk-side is more stable than the dawn-side; (4) the turn-southward of the interplanetary magnetic field will results the maximum fluctuation region moving from the ecliptic plane to the north pole-high latitude region, so that the south-north anisotropy of the magnetic activity will increase, which will reach a maximum when the angle between the interplanetary magnetic field and the ecliptic plane equals about 45°; (5) the dawn-dusk anisotropy will decrease with the increase of the relative fluctuation of the magnetic field.The distribution characteristics of the magnetic field fluctuations in the magnetosheath, obtained from our model, are consistent with the satellites observations and are the possible cause of some of the dawn-dusk asymmetry of the magnetopause and the boundary.
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    Experimental Parameters for the Volland Convection Electric Field Model
    Wu Lei;Song Xiao-ting;B. L. Barouch
    1985, 5 (1):  27-33.  doi: 10.11728/cjss1985.01.027
    Abstract ( 1473 )   PDF (492KB) ( 740 )   Save
    The data obtained by some ground based and space-craft observations are gathered to give the experimental parameters for Vollaml's model of magnetospheric convection electric field. The results are well consistent with the plasmapause characteristics measured by the satellite GEOS-2 and with the Harang discontinuity dynamics measured by the STAREradars and with the magnetospheric-ionospheric electric fields measured in recent years. It is shown that the Volland's model with parameters represented by experimental results can be used to study the magnetosphere and ionosphere.
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    The Ratio of OI5577Åto N2+ 3914Åunder Diffuse Auroral Condition
    Tad Hong-sheng
    1985, 5 (1):  34-39.  doi: 10.11728/cjss1985.01.034
    Abstract ( 1394 )   PDF (410KB) ( 629 )   Save
    Alinear relationship between the ratio of 015577Å to N2+3914Å and the corresponding altitudes are found in this paper. With this dependence the quenching factor of O(1S) in lower thermosphere is obtained, this quenching factor is not very large.
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    The Lacuna Phenomenon of Ionogram over Wuchang, China
    Tan Zi-xun;Huang Xin-yu
    1985, 5 (1):  40-44.  doi: 10.11728/cjss1985.01.040
    Abstract ( 1444 )   PDF (905KB) ( 942 )   Save
    In this paper, a Lacuna phenomenon over Wuchang, China is revealed and studied. The obvious difference between this Lacuna phenomenon and the common one is that it occurs on a geomagnetieally quiet day.Some other very rare phenomena occurring in that day are also studied. It may by a coincidence that several rare phenomena come together on the same day. But at least it enlightens us on that the special events are liable to recognization on geomagnetieally quiet days.
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    The Selection of Optimum Spectral Channels for Multispectral Remote Sensing
    Wang Chuan-shan
    1985, 5 (1):  45-52.  doi: 10.11728/cjss1985.01.045
    Abstract ( 1950 )   PDF (536KB) ( 1087 )   Save
    So far there is no theoretically effective method for the selection of optimum spectral channels for multispectral remote sensing. In this paper a new method is proposed which is based on the criteria of maximum information. As strong correlation exists among signals in different spectral channels, this factor must ibe seriously considered during the computation of amount of information. Prom the measured spectral characteristics of main ground objects, mutual correlation factors of all spectral channels are computed. If signals are supposed to be normally distributed, then by computing determinants of correlation matrices, conditional information of each channel signal can be obtained. By comparing the total amount of information of every possible combination of channels, the optimum combination can be found. When the number of possible channels is too large, the computation process may be very complex and time comsuming. Asimple method is also recommended which can give "quasi-optimum" selection of spectral channels. An example is shown for illustration, and the result is compared with the experimental result in foreign literature. Some comments are made by the author for the design of future remote sensing satellite mutisipectral systems.
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    Studies of Infra-thermogram of the Head and Neck
    Pang Cheng;Sun Hong-yuan;Chang Shao-yong
    1985, 5 (1):  53-58.  doi: 10.11728/cjss1985.01.053
    Abstract ( 1473 )   PDF (961KB) ( 956 )   Save
    The characteristics of the skin temperature distribution in the head and neck regions under two different air temperatures are researched. According to the degree of the effects of air temperature on them, the. distribution in the head and neek regions can be divided into thermostable and thermolabile areas. By computer processing, the result of digital image displays of temperature show that skin temperature presented in irregular and large lumped or small scattered distribution. The latter condition more often occurred under the air temperature of 20℃. By statistical measures, mean skin temperature under higher air temperature has the following features: the temperature of the frontal part is higher, that of the lateral part is moderate, while that of the back part is lower. When the air temperature lowered down, the differences among these parts do not remain, but the surface temperature of each corresponding part still show the ability in changing skin temperature under the influence of air temperature. The characteristics of skin temperature distribution in the head and neek regions has a practical significance for the design of personal protective equipments such as liquid-cooled cap etc.
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    Statistical Analysis of Chemical Components of Moon and Terrestrial Planets
    Xu Dao-yi
    1985, 5 (1):  59-64.  doi: 10.11728/cjss1985.01.059
    Abstract ( 1389 )   PDF (399KB) ( 1173 )   Save
    Materials of model chemical analysis of Moon and terrestrial planets are examined by some multivariate statistical analyses (cluster analysis and discriminant analysis). The results show that the Moon's constituents are more closely related to those of the Mars and asteroids than other terrestrial planets including the Earth. Therefore, it is suggested that the Moon possibly came from the region located at the outer side of Earth's formation region.
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    Self-focusing of Whistler Waves in the Magnetosphere(II)——A Discussion on the Case of Wave Amplification Taking Place
    Wang Yuan-dian
    1985, 5 (1):  65-68.  doi: 10.11728/cjss1985.01.065
    Abstract ( 1369 )   PDF (276KB) ( 873 )   Save
    Self-focusing of whistler waves in the magnetosphere are analysed. The results show that it is possible for moderate and strong whistlers to be focused during their propagation in the magnetosphere. The self-focusing may be a nonlinear mechanism for the guided propagation of the whistlers. Furthermore, it is pointed in this paper that, if there is wave amplification in the magnetosphere, it is easier for the waves to be focused ; oppositely, if there is wave absorption, it is not easier for the waves to be focused.
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    Relations Between Transmission Distance and Phase/Group Path for Oblique Propagation
    Liu Xuan-mou;Gu Tao;Cui Eong;Bao Li
    1985, 5 (1):  69-74.  doi: 10.11728/cjss1985.01.069
    Abstract ( 1510 )   PDF (433KB) ( 936 )   Save
    In this paper, a set of differential equations is obtained which relates phase path P, group path P' and transmission distance Dfor oblique propagation under the assumption that the ionosphere is spherically stratified. The expressions with regard to the P-Dand P'-Dcurve slopes are also derived, and a possible application of these curves is briefly discussed.
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