First measurements of periodicities and anisotropies of cosmic ray flux observed with a water-Cherenkov detector at the Marambio Antarctic base

A new water-Cherenkov radiation detector, located at the Argentine Marambio Antarctic Base (64.24S-56.62 W), has been monitoring the variability of galactic cosmic ray (GCR) flux since 2019. One of the main aims is to provide experimental data necessary to study interplanetary transport of GCRs during transient events at different space/time scales. In this paper we present the detector and analyze observations made during one full year. After the analysis and correction of the GCR flux variability due to the atmospheric conditions (pressure and temperature), a study of the periodicities is performed in order to analyze modulations due to heliospheric phenomena. We can observe two periods: (a) 1 day, associated with the Earth’s rotation combined with the spatial anisotropy of the GCR flux; and (b) $～$ 30 days due to solar impact of stable solar structures combined with the rotation of the Sun. From a superposed epoch analysis, and considering the geomagnetic effects, the mean diurnal amplitude is $～$ 0.08% and the maximum flux is observed in $～$ 15 h local time (LT) direction in the interplanetary space. In such a way, we determine the capability of Neurus to observe anisotropies and other interplanetary modulations on the GCR flux arriving at the Earth.     

基于多目标决策的 对岸火力支援火力分配模型

在建立对岸火力支援作战中火力分配思维机制的基础上,根据最优火力分配的基本要素,构建了基于多目标决策分析的火力分配模型。通过改进后遗传算法对模型进行仿真求解,结果验证了多目标决策分析方法在对岸火力分配问题中的适用性,运用改进后的遗传算法对火力分配模型求解具有明显的优势。     

红外探测设备抗烟幕干扰试验及评估方法

红外探测设备抗烟幕干扰能力是其抗干扰能力的重要部分。常规方法对场地和实施要求很高,试验次数安排有限。文章对该试验设计的关键问题开展分析和研究,根据红外探测设备作用距离与目标能量的关系,采用"等效试验"构建外场静态试验干扰环境,并合理选择试验因素采用均匀设计方法进行试验设计,确定抗干扰试验方案和评估方法。该方案可指导试验获得科学合理有效的数据,从而实现烟幕干扰环境下红外探测设备的抗干扰能力的准确评估。     

基于单光子探测器恢复时间的误码率分析

在深空激光通信中，为满足通信距离远、传输速率高的要求，常采用脉冲位置调制（Pulse Position Modula-tion， PPM）与单光子探测器（Single-Photon Detector， SPD）相结合的探测体制。本文从单光子探测器的恢复时间特性出发，推导了探测器单元探测概率和虚警概率模型，建立了基于信号或硬判决和最大计数硬判决的多元单光子探测器阵列误码率模型。仿真分析结果表明：在16-PPM调制和RS（15，8）编码（Reed-Solomon Codes，里德-所罗门编码）体制下，为实现1.22 Gbps的通信速率、误码率优于10^-7，当探测器单元数为4时，探测器恢复时间应≤3.2 ns；当探测器单元数为25时，探测器恢复时间应≤10 ns。     

A new approach for pulse amplitude measurement using Lagrange’s interpolation for radiation or particle detectors

In radiation detector signal processing, usually, the charge-sensitive preamplifier converts the small charge signal coming from the semiconductor-based detector into voltage form and then the signal is further amplified to measure the energy of the incoming radiation. The voltage pulse from a charge-sensitive preamplifier (CSPA) is amplified using a shaping amplifier which reduces the signal bandwidth. To achieve better energy resolution, precise measurement of the peak amplitude of shaping amplifier output is required. The signal processing methods are available in which the signal from the charge-sensitive preamplifier can be directly digitized using high-speed Analog to Digital Converters (ADC), and then further signal processing such as gain and shaping is carried out inside the Field Programmable Gate Arrays (FPGA). For multiple detector systems, digital signal processing methods are quite difficult to implement in Field Programmable Gate Arrays (FPGA). In this context, The development of an alternative technique is initiated that uses a charge-sensitive preamplifier, shaping amplifier, low sampling analog-to-digital converter, and FPGA, where LaGrange’s interpolation technique is implemented in FPGA to precisely measure the peak of the analog pulse. In this paper, the comparison of the proposed method with other pulse amplitude measurement techniques is discussed. Results show that the implemented technique gives similar energy resolution compared to digital pulse processing and standard peak detector-based techniques.