子载波相位与BOC信号功率谱密度的关系研究

首先介绍了导航信号功率谱密度求解的一种通用方法,基于该方法,经过建模和推导,得到任意相位子载波BOC(二进制偏移载波)信号的功率谱密度显式表达式。通过仿真及分析表明,不同的子载波相位对应的BOC信号功率谱密度存在差别,正是这些差别影响了导航系统的性能,同时也为导航系统的信号体制设计带来了灵活性。文中得到的一些结论,可以给未来的导航信号体制设计中BOC信号子载波相位的选择提供一些借鉴。     

BPSK调制信号中的幅度调制现象分析

在许多场合 ,需要找出BPSK(BinaryPhaseShiftKey ,即二进制相移键控 )调制信号的调制时刻。但实际上并不能直接发现BPSK调制信号的调制时刻 ,只能看到有明显的幅度调制现象。对这种现象产生的原因和用途作了分析 ,并通过仿真实验对这种现象进行了验证。     

基于CAPS系统的信号调制方式的比较研究

概述了二元相移键控(BPSK)调制以及二进制偏移载波(Binary Offset Carrier,BOC)的调制原理,并基于由中国科学院主导研发的中国区域定位系统(Chinese Area Positioning System,CAPS)的实际情况,对其调制信号的测距精度、跟踪性能、多径误差的影响做了分析。分析结果对于中国区域定位系统信号体制设计、调制方式的选取具有一定的借鉴意义。     

2009年7月22日日食期间VLF信号相位和场强的观测和分析

2009年7月22日日食期间,分别在重庆、桂林和青岛利用阿尔法场强与相位监测仪观测了来自俄罗斯阿尔法导航系统位于Novosibirsk、Krasnodar和Khabarovsk的3个发射台3个频率的甚低频信号,并对实验数据进行了分析。通过建立日食期间的电离层模型,结合实际传播路径地面电磁参数,推测全食区低电离层的等效高度;给出经不同路径传播的VLF(甚低频)信号相位突变与日食发生时刻的关系及原因;分析了日食期间经不同路径传播的VLF信号的场强起伏变化,发现场强变化滞后于相位变化这一现象。     

Morphology and kinematics of the gas envelope of the Mira binary W Aquilae

We analyse ALMA observations of the12CO(3-2) emission of the circumstellar envelope(CSE)of the Mira variable binary star W Aql. These provide, for the first time, spatially resolved Doppler velocity spectra of the CSE up to angular distances to the central star ofy nature of the observations(only five minutes in each of～5′′(meaning some 2000 AU). The explorator two different configurations) does not allow for a detailed modelling of the properties of the CSE but provides important qualitative information on its morphology and kinematics. Emission is found to be enhanced along an axis moving from east/west to north-east/south-west when the angular distance from the central star projected on the plane of the sky increases from zero to four arcseconds. In parallel, the Doppler velocity distribution displays asymmetry along an axis moving from east/west to north-west/south-east. The results are discussed in the context of earlier observations, in particular of the dust morphology.     

Internal stellar rotation and orbital period modulation in close binary systems

The orbital period modulation, observed in close binary systems with late-type secondary stars, is considered in the framework of a general model that allows us to test the hypothesis proposed by Applegate. It relates the orbital period variation to the modulation of the gravitational quadrupole moment of their magnetically active secondary stars produced by angular momentum exchanges within their convective envelopes. By considering the case of RS CVn binary systems, it is found that the surface angular velocity variation of the secondary component required by Applegate's hypothesis is between 4 and 12 per cent, i.e. too large to be compatible with the observations and that the kinetic energy dissipated in its convection zone ranges from 4 to 43 times that supplied by the stellar luminosity along one cycle of the orbital period modulation. Similar results are obtained for other classes of close binary systems by applying a scaling relationship based on a simplified internal structure model. The effect of rapid rotation is briefly discussed finding that it is unlikely that the rotational quenching of the turbulent viscosity may solve the discrepancy. Therefore, the hypothesis proposed by Applegate is not adequate to explain the orbital period modulation of close binary systems with a late-type secondary.     

Biperiodic orbital period modulation of the W UMa binary system CK Bootis

A study of the orbital period variation of the W UMa system CK Bootis is made using an extended observational time base. The biperiodicity of the orbital period modulation is emphasized. Both detected periodicities (24.14 yr and 10.62 yr) cannot be explained through the light-time effect unless the companion would be a white dwarf as suggested by other authors, too. Moreover, we also argue that, nowadays at least, it seems that there is no causal relation between the orbital period variation and the recently discovered visual companion. Consequently, we infer that at least one of the two periodicities may be related to the magnetic activity cycles in the component stars of CK Boo, while the other periodicity could be related to the presence of a fourth companion in the system.     

The interaction between the secondary and the common convective envelope in a contact binary

It has been suggested that a contact system almost certainly cannot exist in static equilibrium undergoing periodic thermal relaxation oscillation. The energy transfer in a common convective envelope (CCE) makes the secondary have a complex structure, so the interaction between the secondary and CCE may play an important role in the structure and evolution of the contact system. The present paper tests the TRO theory and investigates this interaction with polytropic stellar model from the observational datum of 22 contact systems directly. It shows that the A-type systems are expanding with a velocity of 25.04 m yr^–1, and the W-type systems are contracting at velocity of 3.10 m yr^–1 by the calculations about these contact systems. Also, we calculate the ratio of energy transfer and the interaction coefficient for them. The HS (hot secondary) model is supported by our calculations. These results may help to understand the TRO theory and the W-phenomenon.