High-resolution, coupled thermosphere–ionosphere models for space weather applications

Current first-principles global models of the coupled thermosphere–ionosphere (T–I) system use grids that are too coarse to simulate the mesoscale and small-scale structures that occur in this complex system. These small-scale and mesoscale structures have a great effect on global-scale neutral and plasma distributions and have important consequences for daily space weather. In this paper, we present a new first-principles, high-resolution, T–I nested grid (TING) polar cap model that incorporates multiple nesting levels and two-way interaction. The TING model simulation of the electron densities and temperatures demonstrates the importance of high spatial resolution. It is found that both the mid-latitude electron density trough and its associated dawn electron temperature peak are more pronounced and structured in the nested grid than in the coarse grid. Using the TING model to simulate ionospheric F₂ region electron density variations with geomagnetic activity and universal time (UT) is also discussed.     

Space weather service activities and initiatives at LAMP (Argentinean Space Weather Laboratory group)

Since more than one decade ago, several institutions started to offer a large variety of Operative Space Weather (SWx) products. This is of major importance because Space Weather events can affect aviation communications, global positioning systems, grid electric power, satellite technologies, and human health in space. The scientific potential on solar-terrestrial physics in Argentina motivated the creation of an interdisciplinary Laboratory of Space Weather in Argentina. The Argentinean Space Weather Laboratory (in Spanish ‘Laboratorio Argentino de Meteorología del esPacio’, LAMP) was initiated in 2016, and it carries out daily monitoring of real-time information (space and ground-based instruments) on Space Weather. The information is synthesized on a weekly bulletin as a summary of the Space Weather conditions, and it is posted on a website (spaceweather.at.fcen.uba.ar). The analyzed information includes own data and of other centers that offer them publicly, and it is also analyzed and discussed later on, during monthly briefings. In particular, one of the regional products that is included in the briefing discussions and it was developed by LAMP in collaboration with INPE-EMBRACE, involves Vertical Total Electron Content (VTEC) maps in the Argentinean region. LAMP set up a Space Weather Laboratory in the Antarctic peninsula, in the Argentine Marambio base, where a Water Cherenkov radiation Detector (WCD) was installed during the Argentinean Antarctic campaign (January-March of 2019). This detector is the southern node of a Latin American Collaboration (LAGO, Latin American Giant Observatory), which is a network of WCDs installed throughout more than 10 Latin American countries.     

The lower ionosphere response to its disturbances by powerful radio waves

The paper presents data from some campaigns at Sura heating facility in 2011–1016. The experiments on probing of the artificial disturbed region of the lower ionosphere were carried out at two observation sites. One of them was located near Vasil’sursk 1 km from Sura facility (56.1°N; 46.1°E) and the other site was located at the Observatory (55.85°N; 48.8°E) of Kazan State University, 170 km to the East. Investigation of the features of the disturbed region of the lower ionosphere based on its diagnostics by the methods of the vertical sounding and oblique backscattering is the main goal of this paper. Ionosphere disturbance was fulfilled by the effect of the powerful radio wave of the ordinary or extraordinary polarization emitted by transmitters of the Sura facility with effective radiated power ERP = 50–120 MW at the frequency of 4.3, 4.7 and 5.6 MHz. Pumping waves were emitted with period from 30 s to 15 min. The disturbed region of the ionosphere in Vasil’sursk was probed by the vertical sounding technique using the partial reflexion radar at the frequency of 2.95 and 4.7 MHz. For the oblique sounding of the disturbed region the modified ionosonde Cyclon-M, operating at ten frequencies from 2.01 to 6.51 MHz was used at the Observatory site. On many heating sessions simultaneous variations of the probing partial reflection signals in Vasil’sursk and backscattered signals in Observatory were observed at the height at 40–100 km below the reflection height of the pumping wave. These observations were correlated with the pumping periods of the Sura facility. Possible mechanisms of the appearance of the disturbance in the lower ionosphere and its effect on the probing radio waves are discussed.     

The low and middle latitude semi-annual anomaly in NmF2 near noon: A statistical study

Hourly values of the F2-layer peak density, NmF2, measured by 99 ionosonde stations near noon from 1957 to 2010 at low and middle geomagnetic latitudes of the northern and southern geographic hemispheres are used in a statistical study of the F2-region semi-annual anomaly. The equinox/winter and equinox/summer geomagnetically quiet NmF2 ratios, X and Y, taken near noon over each ionosonde for approximately the same winter, equinox, and summer solar activity conditions are analyzed. The conditional probabilities of occurrences of X and Y in intervals of X and Y, the most frequent values of X and Y, the mean expected values of X and Y, and the conditional probability to observe the F2-region semi-annual anomaly are calculated and studied for the fist time for low, moderate, and high solar activity conditions. These statistical parameters are averaged over 5° geomagnetic latitude interval in the northern and southern geographic hemispheres, and the trends in these averaged statistical characteristics of the NmF2 semi-annual anomaly are calculated and studied for the fist time. It is shown that the median approach can produce the incorrect conclusions about the absence of the NmF2 semi-annual anomaly.     

Equatorial vertical E × B drift velocities inferred from ionosonde measurements over Ouagadougou and the IRI-2007 vertical ion drift model

F-region vertical plasma drift velocities were deduced from the hourly hmF2 values acquired from ionogram data over a near dip equatorial station Ouagadougou (12.4°N, 358.5°E, dip angle 5.9°N) in Africa. Our results are compared against the global empirical model of Scherliess and Fejer (1999) incorporated in the IRI model (IRI-2007) for 1600 to 0800 LT from 1 year of data during sunspot maximum year of 1989 (yearly average solar flux intensity, F10.7 = 192) corresponding to the peak phase of solar cycle 22, under magnetically quiet conditions. The drifts are entirely downward between 2000 and 0500 LT bin for both techniques and the root mean square error (RMSE) between the modeled and the ionosonde vertical plasma drifts during these periods is 3.80, 4.37, and 4.74 m/s for June solstice, December solstice and equinox, respectively. Ouagadougou average vertical drifts show evening prereversal enhancement (PRE) velocity peaks (V_ZP) of about 16, 14, and 17 m/s in June solstice, December solstice, and equinox, respectively, at 1900–2000 LT; whereas global empirical model average drifts indicate V_ZP of approximately 33 m/s (June solstice), 29 m/s (December solstice), and 50 m/s (equinox) at 1800 LT. We find very weak and positive correlation (+0.10376) between modeled V_ZP versus F10.7, while ionosonde V_ZP against F10.7 gives worst and opposite correlation (−0.05799). The results also show that modeled V_ZP–Ap indicates good and positive correlation (+0.64289), but ionosonde V_ZP–Ap exhibits poor and negative correlation (−0.22477).     

Multifunctional Martian habitat composite material synthesized from in situ resources

The two primary requirements for a Martian habitat structure include effective radiation shielding against the Galactic Cosmic Ray (GCR) environment and sufficient structural and thermal integrity. To significantly reduce the cost associated with transportation of such materials and structures from earth, it is imperative that such building materials should be synthesized primarily from Martian in situ resources. This paper illustrates the feasibility of such an approach. Experimental results are discussed to demonstrate the synthesis of polyethylene (PE) from a simulated Martian atmosphere and the fabrication of a composite material using simulated Martian regolith with PE as the binding material. The radiation shielding effectiveness of the proposed composites is analyzed using results from radiation transport codes and exposure of the samples to high-energy beams that serve as a terrestrial proxy for the GCR environment. Mechanical and ballistic impact resistance properties of the proposed composite as a function of composition, processing parameters, and thermal variations are also discussed to evaluate the multifunctionality of such in situ synthesized composite materials.     

大功率无线电波加热低电离层

等离子体对大功率电波的欧姆耗散会使电子温度升高,进而导致电子密度和其他等离子体参数改变,实现电离层的地面人工变态.本文基于大功率无线电波与低电离层相互作用的自洽模型,分析了不同入射条件下电离层参数的变化,主要结论如下:电离层D区是电波的主要吸收区,并且其吸收强度随入射频率的升高而降低,当入射频率为6 MHz（有效入射功率为200 MW）时电子温度的最大增幅约为520 K,电子密度最大增幅为7300 cm^-3左右;电子温度达到饱和所需时间小于电子密度的饱和时间,前者具有μs量级,后者具有ms量级;停止加热后,电子温度和密度迅速恢复到初始状态,恢复时间均小于各自的饱和时间,但量级相当;入射功率越高,电子温度和密度的增幅越大,并且饱和时间也越长,在相同入射条件下,夜晚的饱和时间要大于白天.     

电离层综合探测器数据采集处理单元设计研究

电离层综合探测器(CDI)是一种面向快速响应航天器平台、用于原位综合探测电离层等离子体及未完全电离中性气体的新概念空间环境探测仪器, 实现了对常规平板朗缪尔探针、阻滞势分析器和离子阱质量分析器的小型化、一体化设计与集成. 本文基于USB2.0接口和FPGA (Field-Programmable Gate Array)技术, 选用高集成度的COTS (Commercial-Off-The-Shelf)器件, 对CDI多通道数据采集处理单元的系统方案和硬件设计进行研究, 并对FPGA的逻辑资源利用情况和Fusion器件内部ADC采样以及FIFO (First Input First Output)读写时序进行了仿真和分析.      

火星及其环境

火星环境类似于地球,而探索其生命存在是重大的科学任务。在火星探测中,对火星及其环境的了解与研究是重要的任务目标,事关探测任务的成功实施。文章对国外火星探测已发布的成果进行收集和整理,其中包含大量的相关数据。这些知识和数据是火星探测任务设计的输入条件,可为我国火星探测计划的制定提供参考依据。     

火星土壤物理力学特性分析

火星土壤既是火星表面探测活动的主要探测对象,也是表面探测器设计中需考虑的重要因素之一。火壤的物理力学特性将直接影响着陆器着陆缓冲系统、火星车移动系统等的设计。此外,在着陆器和火星车等表面探测器的地面研制过程中,需要研制模拟火壤,形成模拟的火星表面环境,开展相关的着陆器着陆缓冲性能、火星车移动性能等验证试验。迄今为止,人类已经有多个探测器登陆火星,获取了大量的有关火壤的信息,也研制了多种模拟火壤。通过对已有火壤和模拟火壤的物理力学特性分析,梳理出火壤物理力学特性的参数范围,可为我国火星探测器的研制提供参考。