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排序方式: 共有371条查询结果,搜索用时 15 毫秒
81.
X射线脉冲星自主导航系统可以为深空探测器提供位置、速度、时间和姿态等丰富且自主的导航信息,以X射线脉冲星测得的信息作为量测量,结合轨道动力学方程,对航天器的轨道进行自主估计确定。论文阐述了该方案的导航原理,在借鉴现有航天器导航系统的基础上,提出了基于X射线脉冲星导航的方案,介绍了方案的硬件组成、系统结构,并针对方案中导航敏感器多冗余的特征,给出了基于多传感器组合导航技术的结构,最后用仿真资料对方案做了性能概算和精度估计。 相似文献
82.
The five main types of antisunward propagating energetic fluxes (particles and emission) may be thought of as well established to date, the effects of which lead to a particilar character of disturbance in the near-terrestrial environment (the Earth's magnetosphere, ionosphere and atmosphere). The strongest global restructuring of the magnetosphere and ionosphere is caused by fluxes of relatively dense n of 1-70 cm-3 at the Earth's orbit) Solar Wind (SW) quasi-neutral, low-energy (E < 10 keV) plasma which cause magnetospheric and ionospheric storms lasting 24 hours or longer. For that reason, main attention is given to their study at the initial stage of research. The physical essence of the method of predicting disturbances in the near-terrestrial space environment, the amplitude of which can be expressed in, for example, the Kp index units, involves:(1) identifying all the most geo-effective SW streams of type, (2) determing their sources on the solar disk,and (3) quantifying the correlations between the characteristics of their solar sources with a maximum value of the Kp-index that is caused by the concerned type of SW stream. Semi-phenomenological relations have been obtained, which relate parameters of type SW stream sources to characteristics of geomagnetic storms:storm commencement, the time at which the storm intensity reaches its maximum values, the storm duration,as well as to the storm amplitude expressed in terms of geomagnetic indeces. 相似文献
83.
84.
采用磁过滤直流真空阴极弧沉积技术在硅片、不锈钢片基体上制备了类金刚石(DLC)膜。检测结果表明,膜中存在着微米级的大颗粒分布,膜厚为290nm,sp3键的含量为62.23%。所制备的薄膜具有典型的DLC膜Raman光谱特征,耐磨性能优良,膜与基体的结合性能良好。 相似文献
85.
Eijiro Hiei 《Space Science Reviews》1994,70(1-2):189-192
X-ray emission from solar coronal loops changes on two different timescales: a) flare loops and transient active region brightenings show a rapid variability, b) quiet region loops are quasi-steady and change only slowly with time. This different time behavior has been analyzed on the basis of Yohkoh SXT observations and we report here on the results from our analysis, mainly focussing on quiet loop variability. 相似文献
86.
Eugene M. Trunkovsky 《Space Science Reviews》1995,74(3-4):485-488
Photoelectric WBVR observations of Be star HDE 245770=V 725 Tau, the optical counterpart of the transient X-ray pulsar A0535+26, having a pulse period of about 104 s, were conducted for more than 10 years. An irregular long-term optical variability of the star with amplitudes of the order of a few tenths of magnitude was found to be a usual phenomenon. In some cases rapid changes of the star's optical luminosity with a characteristic period of a few tens of minutes or a few hours, and an amplitude of several hundredths of magnitude in all the spectral bands used, which have practically coincided or correlated with the X-ray pulsar outbursts detected by X-ray satellites, were observed.Photoelectric recording of the optical flux from HDE 245770 were made in 1981–1982 with a time resolution of 1 second and 10 s, respectively, in theR spectral band (0 7000 Å) and in the narrowH
-emission-line band (1/2 75 Å) using a 48-cm reflector of High-Mountain Tien-Shan observatory of the Sternberg Astronomical Institute near Alma-Ata. An analysis of autocorrelation functions of the flux changes from object under study and a comparison with the star BD+26° 876 indicated the variability of luminosity of V 725 Tau in theR spectral band on a time scale of a few tens of second; this variability resembles shot noise with a characteristic time of stochastic bursts of about 15–20 s and their amplitudes of about a few tenths of a percent. InH
-emission-line radiation autocorrelation functions and power spectra show quasiperiodic variability of luminosity of HDE 245770 with a characteristic period of about 100–150 s and an amplitude in the neighbour-hood of 0.5%. The latter result is not quite reliable because of not quite fine weather conditions during the observations; independent observations and check-up are required. 相似文献
87.
介绍了一种新的宽带源DOA估计方法:TOFS。与TOPS(投影子空间正交性测试)方法类似,该方法通过同时测试频域各频段噪声子空间与阵列搜索流型之间的正交性来进行DOA估计。作为对比,根据非相关MUSIC方法,提出了一种新的适用于宽带的非相关MUSIC方法,称为I-MUSIC方法。与宽带相关方法不同,TOFS方法不需要任何初始值的预估。与宽带非相关方法也不相同,TOFS方法同时测试各频段噪声子空间与阵列搜索流型之间的正交性。仿真了TOFS与I-MUSIC、CSSM、TOPS的性能比较。仿真结果表明,CSSM方法在低信噪比时有较好的性能,TOFS方法在中等信噪比以上时,有较好的性能。同时,TOFS方法避免了TOPS方法中常常出现的伪峰。 相似文献
88.
89.
Yu.N. Gnedin G.V. Khozov V.M. Larionov 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1984,3(10-12)
Observations of the X-ray binaries 4U 0115+634 and A 0535+262 performed in 1981 – 1982 revealed significant IR variabilities of these sources. 4U 0115+634 was observed twice, in the state close to X-ray activity, and in the state of low activity, thus changing from K = 7m.75 to K > 9m. A 0535+262 shows the temporal variations ranged from tens minutes to some days. The regular variations of IR brightness are suspected with teh period close to 104 s that corresponds to the period of axial rotation of neutron star in A 0535+262. The results obtained present arguments in favour of hypothesis that IR radiation is generated near the accreting neutron star and is possibly of maser nature. 相似文献
90.
G.G. Pavlov 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1984,3(10-12)
A review is given of recent developments in the theory of emission from a magnetized plasma for accreting neutron star conditions. Some observational data on X-ray pulsars are discussed, and present problems are indicated. 相似文献