火星探测器转移轨道的自主导航方法

本文针对转移轨道火星探测器对自主导航的迫切需求,提出了一种基于小行星和X射线脉冲星交互观测的自主导航方法,并结合工程任务对上述量测信息的获取方式和获取条件进行了研究,仿真结果表明,与单独基于小行星或单独基于X射线脉冲星观测的自主导航系统相比,该方法不仅可获得更高的导航精度,为转移轨道中途修正提供准确的轨道信息,且工程实现简单,是一种可行的转移轨道火星探测器自主导航方案,可为我国火星探测器自主导航系统的设计提供参考.     

Parametric synthesis of pulsar time

A new method of generating pulsar time based on a coherent representation of a sequence of observed events is considered. The properties of pulsar time compared with the traditional approach are analyzed. __________ Translated from Izmeritel’naya Tekhnika, No. 6, pp. 39–44, June, 2006.     

Simulation of X-ray pulsar signals with multiphysical properties

In view of the few and discontinuous X-ray pulsar data, based on the physical properties of the X-ray pulsar real data from the Rossi X-ray Timing Explorer (RXTE) spacecraft, this paper adopts the fast iterative method and the 10 μs time transformation model, simulates the X-ray pulsar signals which have the periodic property, spectral property, and the background noise property as well as a variety of delay effects. We design and implement simulation software which can simulate the X-ray pulsar signals with multi-physical properties. The results of comparing the real data and simulation data in the same situation show that the simulation noises and the actual noises have the same distribution, that the period stability of the simulated X-ray pulsar data agrees with the real data, with the error of only 0.43％, in different energy levels, that the simulated data's integrated profile and the real data's standard profile are highly correlated with the Pearson correlation coefficient of 0.99, and that under the 10μs time transformation model, the time conversion accuracy of the simulation data can reach 10^-7s, the error between the simulation and the real data being just only 10^-7s, which meets the time transformation accuracy. Therefore, the proposed method can realize the high-fidelity simulations and generate the continuous pulsar signal with many physical properties.     

用脉冲星的脉冲序号复现坐标时方法

为实现包括地球和地球以外的时间统一, 需要运用相对时间观的两种时间来替代目前时间计量体系中的标准时间, 这两种时间分别是:原时和坐标时, 其中坐标时可溯源到脉冲星时间基准上。 为构建简单的本地轨道参数历表, 阐明分层嵌 套的空间包含关系, 形成时间相对统一的观点。 从计量角度, 提出了一种脉冲星复现坐标时的理论, 运用相对时间观中的时 间和空间不可分割观点, 归纳了统一时间的广域坐标系所必须具备的基本特征, 强调了原点观者的特殊性, 提出了基于原点 观者的脉冲星脉冲序号和初始历元的定义方法。 首先, 把一组脉冲星的脉冲序号约定为坐标时基准, 用来复现坐标时, 约定 一组脉冲星的脉冲周期为固定的常数数组, 约定后不再测定,常数的单位仍是国际单位制[秒], 常数可理解为脉冲序号的坐 标时间隔与[秒]之间换算的系数。 然后,基于平面电磁波模型, 把脉冲星的脉冲电磁波经过原点的时刻与脉冲序号一一对应, 于是原点观者的坐标时与连续的脉冲序号成为线性函数关系, 最后, 分析了脉冲星稳定特点, 给出了以一组序号为变量的脉 冲星集合稳定性判据。     

聚焦型X射线脉冲星望远镜Pareto多目标优化与多场耦合分析

为提高聚焦型X射线脉冲星望远镜的探测性能,提出一种聚焦型X射线脉冲星望远镜（Focusing X-ray pulsar telescope,FoXPT）多目标优化与多场耦合分析方法。基于X射线全反射理论构建以探测灵敏度和重量最小化为目标的多目标优化模型,采用改进的Pareto法获得产品的非劣解集。基于弹性力学、热传导和热辐射理论构建了结构-热耦合方程,以遴选的优化结果构建产品三维模型和有限元模型,获得产品应力与位移分布并提取X射线反射镜面形误差,基于高次多项式函数重构结构-热耦合形变后的X射线反射镜面形,并进行拟合和误差分析。采用Monte Carlo光学追踪法对产品的聚集性能进行仿真分析与评价,实现了FoXPT多目标优化与多场耦合分析的有效集成。结果表明：当嵌套层数为17层时,重量和探测灵敏度同时获得满意解,分别为3.112 kg和6.15×10^-4 phs/cm²/s/keV,光机热耦合分析最大应力为262.54 MPa,X射线聚焦效率提升至86.83%,满足实际工程设计要求。     

A new parametric equation of state and quark stars

It is still a matter of debate to understand the equation of state of cold matter with supra-nuclear density in compact stars because of unknown non-perturbative strong interaction between quarks. Nevertheless, it is speculated from an astrophysical view     

基于光量子探测的XPNAV半物理仿真及建模

基于X射线脉冲星导航(XPNAV)系统的工作原理,设计并实现了一种基于激光量子探测的XPNAV地面仿真系统.通过分析X射线脉冲星信号,建立了信号的调制模型,提出了脉冲星信号轮廓累积Renyi熵方法,模拟产生了X射线脉冲星信号.实验表明,构建的XPNAV半物理仿真系统简单实用,可以实现XPNAV的实验验证,其产生的模拟信...     

X射线脉冲星导航探测器的微通道板甄选

根据应用于X射线脉冲星导航系统的大面阵X射线探测器对微通道板(MCP)性能的要求,研究了甄选微通道板的方法。确定了甄选微通道板的4个关键参量,分别是增益的均匀性、阻抗匹配、暗计数率、增益系数。针对这4个参量设计了相应的测试实验,制定了甄选MCP的流程,并对采用该流程甄选出的MCP进行了幅值和计数率的测试。测试结果显示:采用单通道阳极接收信号时,每一个探测单元的幅值存在的相对误差各不相同,第i个探测单元输出的信号幅值的最大相对误差Δ1i和最小相对误差Δ2i的波动分别为7%~13.5%,3%~6.7%;而采用四通道共享阳极时输出信号的Δ1i为7.8%、Δ2i为3.1%;单通道阳极计数率之和(n=n1+n2+n3+n4)与四通道共享阳极计数率N的相对误差为4.38%,小于预估值10%。上述实验结果表明该甄选方法能够甄选出满足探测器要求的MCP。     

中子星磁场研究进展

射电脉冲星，包括单星和双星，其观测特征被评论．双星脉冲星和毫秒脉冲星的短周期和弱磁场相关性暗示这些脉冲星是存在双星吸积过程的反加速脉冲星．最近提出的中子星磁场起源与演化模型进行了分析．     

Synchronization on the basis of pulsar time

A new method of synchronization of atomic timekeepers on the basis of pulsar time that has been synthesized on the basis of observations of the rotation parameters of a pulsar is considered. An analysis of the attainable synchronization precision is presented. __________ Translated from Izmeritel’naya Tekhnika, No. 7, pp. 23–28, July, 2007.