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  pulsar
ART-P/Granat observations of the X-ray pulsar 4U0115+634 during the outburst in February 1990
      
Observations of the transient X-ray pulsar 4U0115+634 with the ART-P telescope aboard the Granat Observatory during the outburst in February 1990 are presented.
      
Spectral variability of the X-ray pulsar Hercules X-1
      
We present the results of our comparative timing and spectral analysis of the high and low (off) states in the X-ray pulsar Her X-1 based on data from the ART-P telescope onboard the Granat observatory.
      
X-ray variability of the pulsar Vela X-1 as observed with ART-P/Granat
      
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A synchronised accumulation technique is used to achieve a resolution of up to 10-13 cm for the oscillating amplitude of a laser interferometer. Such a technique is applied to observe the 60.4 Hz gravitational radiation which is possibly emitted from the pulsar NP 0532 of the Crab Nebula. Present experiments show that no such signal is received.

本文采用同步积累技术,使激光干涉仪对于微小振动振幅的检测能力达到10~(-13)厘米的水平;运用这一技术对蟹状星云中的NP0532脉冲星可能存在的60.4赫芝引力辐射进行了观测。实验表明:未收到这一信息。

The results of statistical analyses of radio luminosity of 81 pulsars obtained in this paper are likely in favor of the version that the radio radiation is emitted from the region near the light cylinder. The various statistical relations given in Table 1-2would provide some clues for exploring the mechanism of radio radiation of pulsars.

本文对81颗脉冲星作了统计分析,所得结果似支持射电辐射产生于光速圆柱附近的看法。文中给出射电辐射(或其与能损率之比)与一系列物理量的关系,为探讨射电辐射机制提供了一些线索。

83 pulsars are statistically studied in this paper. The main results are as follows: (1)Taking the ratio λ of the loss rate of rotational energy to the radio luminosity of pulsars as a parameter of classification, we divide the 83 pulsars into 3 categories. This is not only necessary to the study of the statistical relationship between the luminosity and the magnetic energy in various regions, but it may also be a better method of classification. It may be seen from the plots of P-P, L_(radlo)-P...

83 pulsars are statistically studied in this paper. The main results are as follows: (1)Taking the ratio λ of the loss rate of rotational energy to the radio luminosity of pulsars as a parameter of classification, we divide the 83 pulsars into 3 categories. This is not only necessary to the study of the statistical relationship between the luminosity and the magnetic energy in various regions, but it may also be a better method of classification. It may be seen from the plots of P-P, L_(radlo)-P and L_(radlo)-t that different categories of pulsars have different evolutionary tracks and physical properties. The evolutionary tracks of the 3 categories of pulsars by the λ classification are something similar to those of the model proposed by Lyne et al.(1975) which involves a secular decay of magnetic dipole moment. Therefore the various categories of pulsars may reflect the fact that the different categories of pulsars have different time constants of decay, or the initial values of the magnetic moments were different at birth. There are no apparent properties on the above mentioned plots for the morphological classification by the integrated pulse profiles(S,D and C)(Taylor and Huguenin, 1971). (2)The radio luminosities of pulsars of various categories are all closely correlated to the magnetic energies and“twining”magnetic energies at the light cylinder, and not correlated to the magnetic energies at the surface of the neutron star. This shows that the local radiation regions are in the vicinity of the light cylinder. These magnetic energies may be the energy sources of pulsar radiation. (3)Some pulsars in the right region of the plot of P against P constitute a cut-off line of radio radiation, whose slope is just—4.So that it is a line for which the“twining”magnetic energy PP~(-4)is constunt, It is closer to the observational results than the cut-off line, proposed by Lyne et al.(1975), for which PP~(-5)is constant. This result gives support to the accumulatimi and release of energy in the vicinity of the light cylinder.

本文对83颗脉冲星进行了分类统计研究。主要结果如下: 1.采用转动能损失率与射电光度的比值作为分类参数可以较好地反映不同类型脉冲星的物理特性和演化方式。 2.由于各类脉冲星的射电光度和光速圆柱附近的磁能之间都有着相关系数较高的回归关系,而射电光度和表面磁能之间却不相关,由此推论脉冲星辐射部位很可能在光速圆柱附近。 3.在周期变率户和周期P的关系图上,光速圆柱附近的“缠绕”磁能PP-4的某一临界值可作为射电辐射的截止线,它比Lyne等提出的光速圆柱处的磁能户PP~(-5)作为射电辐射截止线更接近观测事实。

 
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