Aspects related to variability of radiative cooling by NO in lower thermosphere,TEC and O/N2 correlation,and diffusion of NO into mesosphere during the Halloween storms

Nitric Oxide is a very important trace species which plays a significant role acting as a natural thermostat in Earth’s thermosphere during strong geomagnetic activity. In this paper, we present various aspects related to the variation in the NO Infrared radiative flux (IRF) exiting the thermosphere by utilizing the TIMED/SABER (Thermosphere Ionosphere Mesosphere Energetics and Dynamics/ Sounding of the Atmosphere using Broadband Emission Radiometry) observational data during the Halloween storm which occurred in late October 2003. The Halloween storm comprised of three intense-geomagnetic storms. The variability of NO infrared flux during these storm events and its connection to the strength of the geomagnetic storms were found to be different in contrast to similar super storms. The connection between the quantum of energy outflux from the upper atmosphere into space in terms of NO IRF and the duration of storms is established. The NO radiative cooling, and the closely correlated depletion in O/N₂ ratio are controlled by the Joule heating intensity (proxied by AE-index). The collisional excitation rate of NO, calculated using the modelled datasets of WACCM-X (Whole Atmosphere Community Climate Model with thermosphere and ionosphere extension), correlates well with the observed pattern of radiative emission by NO. Observational datasets from TIMED/GUVI (Global Ultra-Violet Imager) and MIT Haystack observatory madrigal GNSS (Global navigation satellite system) total electron content (TEC) database shows that the TEC and O/N₂ enhancement in low-mid northern hemispheric latitudes are mainly controlled by the z-component of Interplanetary magnetic field (IMF-B_z). The penetration of eastward electric field during the storm events is found to be responsible for the overall enhancement of TEC. The contribution of enhanced day-side TEC in observed variation of O/N₂ ratio by GUVI is also reported. It is also seen that during substorms related events the night-time polar region experiences more cooling due to NO than the daytime polar region. The connections between the mid- and low-latitude enhancement in NO IRF with the propagation of LSTIDs (Large-scale traveling ionospheric disturbances) in combination with the O/N₂ variability, and the altitudinal variation in NO flux with the progression of the storm is also investigated. This study presents the evidence on the role of diffusion processes in the large scale enhancement of NO in the mesospheric altitudes.     

基于电加热膜防冰设计方案的分流环表面换热特性试验研究

分流环表面换热特性对提升防冰设计效能至关重要。针对传统热气防冰方案中试验件与试验方案系统复杂、成本高昂等问题，本文提出了一种新型电加热膜防冰设计方案的分流环表面换热系数的试验方法。根据能量守恒定律，推导出分流环表面换热系数理论公式。试验研究了不同俯仰角、速度、液态水含量（Liqid water content,LWC）以及水滴中位体积直径（Median volumetric diameter, MVD）等对分流环表面换热特性的影响。试验结果表明：前缘区域换热系数随俯仰角先增大后降低，25°俯仰角是明显的转折点；相同喷雾条件下的前缘区域、下表面区域的平均换热系数约是干空气条件下的3倍；分流环前缘的换热系数明显大于上、下表面的换热系数。     

Distributed satellite autonomous navigation using X-ray pulsars

Distributed X-ray pulsar-based navigation (DXNAV) is an effective method to realize earth-orbit satellite positioning under weak pulsar signal conditions. In this paper, we propose a new DXNAV method based on multiple information fusion. The DXNAV system principle and the pulse phase estimate Cramér-Rao lower bound are deduced. To suppress the calculation complexity and the error source, the X-ray pulsar photon time-of-arrival detected by each satellite is equivalently converted to the leading satellite directly using the inter-satellite link ranging and starlight angular distance measurement. A high precision estimate model of the pulse phase is built using pulsar standard profile, observed profile, and star-geocentric angular distance from distributed satellites. The estimated pulse phase is real-time supplied to the navigation system, which is established in the form of a deviation equation. The two-stage Kalman filter is designed to estimate the pulse phase in profile histogram bin step and the leader position in real-time step. Compared separately with the maximum likelihood phase estimate method and the celestial navigation method using only the star-geocentric angular distance, the simulation analysis shows that the estimation precisions of position and velocity are improved by 29% and 25%.     

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.     

中远红外高功率量子级联激光技术研究进展

量子级联激光器具有体积小，重量轻，波长可调谐，以及光源能够覆盖中远红外和太赫兹波段等特点，使其在痕量气体检测、定向红外对抗、自由空间光通讯以及红外成像和光谱等领域有着广泛的应用。自从1994年第一个量子级联激光器问世以来，大功率、高电光效率以及室温下连续工作的量子级联激光器一直是人们追求的目标。首先介绍了量子级联激光器的有源层设计、波导设计和器件散热设计方面的研究进展；其次重点讨论了4 μm~5 μm 中波红外和 8 μm~12 μm长波红外高功率室温下连续量子级联激光器的发展和演变、以及大功率脉冲量子级联激光器研究情况；最后简要介绍了大功率量子级联激光器芯片的外延制备技术。     

标定脉宽对冲击传感器标定结果的影响

不同冲击脉宽在标定压电式冲击传感器过程产生不同的结果，主要原因是脉宽冲击频率处于传感器安 装频响的放大区，不同的脉宽作用于传感器后放大效应不同，导致标定结果差异。冲击传感器使用空气炮和霍普金 生杆进行单独标定，对标定结果进行了差异分析。对传感器安装频响曲线进行了定性分析，符合冲击脉宽差导致不 同标定结果的事实。对标定过程中标定脉宽控制提出了具体的措施，对于正确标定冲击传感器具有指导意义。     

脉冲爆震发动机中温度和组分浓度测量技术的发展

脉冲爆震发动机内部工作条件极其恶劣,测量爆震波温度和某组分浓度十分困难。本文回顾了近几年国内外在爆震温度场测量方面的技术发展,特别是应用激光诊断技术测量爆震波的温度和某些组分浓度。总结了国内外应用光学诊断技术测得的爆震波火焰温度,结果发现:对气体燃料/氧气而言,在化学恰当比下一般其爆震波温度大约为3900K,与CJ理论值非常接近;然而对液态燃料JP-10而言,当氧化剂为氧气时,爆震波温度为2500K;当氧化剂为空气时,爆震波温度仅仅约为1500K。