Statistical study of the detection of solar protons of highest energies at 20 January 2005

On January 20, 2005, 7:02–7:04 UT the Aragats Multichannel Muon Monitor (AMMM) registered enhancement of the high energy secondary muon flux (energy threshold ∼5 GeV). The enhancement, lasting 3 min, has statistical significance of ∼4σ and is related to the X7.1 flare seen by the GOES satellite and the ground level enhancement detected by the world-wide network of neutron monitors and by muon detectors. The most probable proton energy corresponding to the measured 5 GeV muon flux is within 23–30 GeV. Due to upmost importance of the detection of solar particles of highest energies in presented paper we perform detailed statistical analysis of the detected peak. The statistical technique introduced in the paper is also appropriate for the searches of sources of ultra-high energy cosmic rays.     

An improved neutron transport algorithm for HZETRN

Long-term human presence in space requires the inclusion of radiation constraints in mission planning and the design of shielding materials, structures and vehicles. It is necessary to expose the numerical tools commonly used in radiation analyses to extensive verification, validation and uncertainty quantification. In this paper, the numerical error associated with energy discretization in HZETRN is addressed. An inadequate numerical integration scheme in the transport algorithm is shown to produce large errors in the low energy portion of the neutron and light ion fluence spectra. It is further shown that the errors result from the narrow energy domain of the neutron elastic cross section spectral distributions and that an extremely fine energy grid is required to resolve the problem under the current formulation. Since adding a sufficient number of energy points will render the code computationally inefficient, we revisit the light ion and neutron transport theory developed for HZETRN and focus on neutron elastic interactions. Two numerical methods (average value and collocation) are developed to provide adequate resolution in the energy domain and more accurately resolve the neutron elastic interactions. An energy grid convergence study is conducted to demonstrate the improved stability of the new methods. Based on the results of the convergence study and the ease of implementation, the average value method with a 100 point energy grid is found to be suitable for future use in HZETRN.     

Neutrino pair emission from the inner crust of a neutron star

It is shown that spin-orbital interaction of neutrons with clusters (nuclei or bubbles) immersed in the neutron sea of the inner crust of a neutron star can intensify substantially the neutrino pair emission (with respect to the neutrino emission in the uniform nuclear matter) at temperatures typical for the neutrino cooling epoch of the star. The neutrino pair emissivity of sub-nuclear matter is calculated both for the case when clusters are at random positions and for the case when clusters are ordered in a lattice.     

复杂星孔球形药柱燃面近似解析计算方法

球形星孔药柱是固体火箭发动机广泛采用的一种药型,多呈现复杂的三维特性。为进行设计参数的快速选择与优化,以一种具有复杂星孔的球形药柱为基础,给出了药柱燃面变化规律的近似解析计算方法,依据该方法能够在设计初期快速计算药柱燃面的变化规律,并能依此进行发动机工作性能预估,进而对设计参数进行调整和初步优化;近似解析方法与三维CAD方法所得到的燃面变化规律基本吻合,燃烧面积最大偏差小于4%。     

伽利略光学实验分析

对伽利略光学实验进行了全面的分析,其中包括实验装置和元器件的分析,并重点分析了实验发射系统的工作原理和工作过程,对准、跟踪系统的工作原理和工作方式.并对实验的结果进行了详细分析,针对实验中出现的因大气影响而导致接收失败,讨论了采用自适应光学对大气影响进行补偿的方案的可行性,对于因背景光过强而导致的链路性能劣化,分析了采用干涉滤光片对背景光进行抑制的可行性,为我国将来开展深空光通信的研究提供参考.     

Neutron star masses derived from relativistic measurements of radio pulsars

Radio telescope observations of relativistic phenomena in binary pulsar systems yield straightforward and robust determinations of the masses of pulsars and their companion stars. This paper summarizes masses measured by this means.     

The structure of the solar cycle maximum phase in the galactic cosmic ray 11-year variation

Two phenomena connected with the maximum phase of the 11-year solar cycle in the galactic cosmic ray intensity – the change in the energy dependence of the intensity variations and the double-peak structure in the intensity modulation time profile – are considered for the last five solar cycles (Nos. 19–23). The distinct 22-year cycle in the magnitude of the so called energy hysteresis is observed.The periods of the solar cycle maximum phase in the galactic cosmic ray intensity, characterized by the specific energy dependence of the intensity, are estimated. It is found that the double-peak structures belonging to the solar cycle maximum phase and those around it are very similar both in the amplitude and in its energy dependence.     

基于微小卫星的空间目标光学探测定位方法

为实现空间目标的天基光学观测,利用双星定位原理,采用仅测角的观测方式,结合最小二乘法建立了双星几何定位模型。考虑到星点提取作为光学定位算法中的重要一环将直接影响最终的定位精度,因而针对就星图处理部分,分析了星图的灰度特点,采用阈值分割法进行了去噪处理,选取了几种质心法对星点进行提取,利用真实星图对提取结果进行比较,选出了形心法和阈值质心法 2种较为可行的星点提取算法。通过仿真计算和蒙特卡洛误差分析结果可知,不考虑误差时,定位误差小于 10-5 m;考虑主要误差源时,定位误差小于 100 m;且姿态误差对定位方法的精度影响最大,数值上可以达到总误差的 0.9倍以上,速度误差的影响最小,只有总误差的 1/30,可以忽略;定位误差近似呈高斯分布且误差的大小与误差源近似呈线性关系。由此可见,文章所建立的定位算法可以对空间目标实现较为精确的定位。     

星光导航技术现状与发展综述

对国内外星光导航技术的研究现状和发展过程进行综述和总结,汇总介绍国外几种典型应用平台星敏感器的发展现状.最后阐述星光导航技术面临的问题和未来的发展趋势.     

应用于天文导航的白昼恒星探测技术

对白昼恒星探测技术的方案进行研究,通过分析大气透过率以及散射光和恒星的光谱分布,选定900～1 700 nm探测波段.根据星表及探测器噪声的实测结果,计算得出基于光轴固定的单一视场与探测灵敏度、捕获概率的关系,并提出适应白昼观星的探测器选型、积分时间、星表设计以及多帧算法策略.观星试验结果与理论计算一致.