Ionospheric total electron content response to annular solar eclipse on June 21, 2020

The effects of physical events on the ionosphere structure is an important field of study, especially for navigation and radio communication. The paper presents the spatio-temporal ionospheric TEC response to the recent annular solar eclipse on June 21, 2020, which spans across two continents, Africa and Asia, and 14 countries. This eclipse took place on the same day as the June Solstice. The Global Navigation Satellite System (GNSS) based TEC data of the Global Ionosphere Maps (GIMs), 9 International GNSS Service (IGS) stations and FORMOSAT-7/COSMIC-2 (F7/C2) were utilized to analyze TEC response during the eclipse. The phases of the TEC time series were determined by taking the difference of the observed TEC values on eclipse day from the previous 5-day median TEC values. The results showed clear depletions in the TEC time series on June 21. These decreases were between 1 and 9 TECU (15–60%) depending on the location of IGS stations. The depletions are relatively higher at the stations close to the path of annular eclipse than those farther away. Furthermore, a reduction of about ?10 TECU in the form of an equatorial plasma bubble (EPB) was observed in GIMs at ~20° away from the equator towards northpole, between 08:00–11:00 UT where its maximum phase is located in southeast Japan. Additionally, an overall depletion of ~10% was observed in F7/C2 derived TEC at an altitude of 240 km (hmF2) in all regions affected by the solar eclipse, whereas, significant TEC fluctuations between the altitudes of 100 km ? 140 km were analyzed using the Savitzky-Golay smoothing filter. To prove TEC depletions are not caused by space weather, the variation of the sunspot number (SSN), solar wind (V_SW), disturbance storm-time (Dst), and Kp indices were investigated from 16th to 22nd June. The quiet space weather before and during the solar eclipse proved that the observed depletions in the TEC time series and profiles were caused by the annular solar eclipse.     

水下高速射流气泡变化过程数值研究

为研究水下高速射流气泡变化规律,采用VOF(Volume of Fluids)模型分别对水下等温高速气体射流和热高速气体射流动态流场进行了气水耦合数值求解。其中热射流考虑了汽化因素对气泡内气流场的影响,数值模拟了气泡的形成、发展、断裂及融合过程,揭示了气泡中压力和马赫数等参数的变化规律,得出了水下点火初期的流场特征。研究发现:在相同入口压力下,热射流产生气泡的空间尺度比等温射流产生的气泡空间尺度要小;气泡发展过程中会出现颈缩,也可能断裂,断裂与否取决于气泡颈缩处内外压差,气泡的颈缩与断裂是产生压力脉动的重要因素,并决定了压力峰的位置和大小,气泡断裂位置越靠近喷管出口,压力峰值越大,该压力峰值会影响火箭发动机尾流场特性。     

微重力下高热流时池内双组分核态沸腾

本文基于Helmholtz不稳定性原理建立了微重力下双组分高热流时核态沸腾的双层汽泡结构模型。由于浮力很小,这种结构能维持到CHF状态。通过对该结构的深入分析,导得了汽柱面积占总面积的百分比及液体层初始厚度的表达式,在此基础上发展了CHF模型。分析结果同实验结果及地面条件下的结果作了比较,对异同之处作出了合理的解释。      

LISM structure — Fragmented superbubble shell?

Small scale structure in local interstellar matter (LISM) is considered. Overall morphology of the local cloud complex is inferred from Ca II absorption lines and observations of H I in white dwarf stars. Clouds with column densities ranging from 2–100 × 10¹⁷ cm^–2 are found within 20 pc of the Sun. Cold (50 K) dense (10⁵ cm^–3) small (5–10 au) clouds could be embedded and currently undetected in the upwind gas. The Sun appears to be embedded in a filament of gas with thickness 0.7 pc, and cross-wise column density 2 × 10¹⁷ cm^–2. The local magnetic field direction is parallel to the filament, suggesting that the physical process causing the filamentation is MHD related. Enhanced abundances of refractory elements and LISM kinematics indicate outflowing gas from the Scorpius-Centaurus Association. The local flow vector and Sco data are consistent with a 4,000,000 year old superbubble shell at –22 km s^–1, which is a shock front passing through preshock gas at –12 km s^–1, and yielding cooled postshock gas at –26 km s^–1in the upwind direction. A preshock magnetic field strength of 1.6 G, and postshock field strength of 5.2 G embedded in the superbubble shell, are consistent with the data.Abbreviations LISM Local ISM - SIC Surrounding Interstellar Cloud - LIC Local Interstellar Cloud     

重力条件对喷雾冷却换热特性影响的研究

喷雾冷却是一种高效的高热流密度散热方式,在空间热控领域具有重要的应用前景。本文基于液膜动力学、气泡动力学和传热学的基本原理,建立了描述微重力条件下喷雾冷却传热特性的理论模型。利用模型模拟的方法,对以水作为工质的微重力条件下喷雾冷却系统的被冷却表面温度分布、冷却曲线等因素进行了分析,分析结果显示:在单相区,重力条件对喷雾冷却的换热特性和表面温度分布不均匀性的影响较小;在两相区,由于微重力条件下气泡难以脱离等因素的影响,使得喷雾冷却的换热能力明显弱于常重力条件下的换热能力,并且被冷却表面的温度不均匀性增大。     

氮气强制对流消除煤油温度分层及其液氮降温系统分析

为找到煤油贮罐降温后的温度分层原因，通过分析煤油贮罐不同深度的温度，结合管道布置走向，发现煤油降温流动过程中存在上部滞流区，导致煤油贮罐形成上部热煤油和下部冷煤油分层。采用鼓泡与泵回流两种方式进行对比试验，结果表明鼓泡能较好消除煤油贮罐在垂直方向上的温度不均，泵回流方式无明显效果。为准确预估降温后的煤油温度，采用不同调温方式进行多次试验，构建了煤油调温目标温度计算模型，作为煤油降温停止的判断准则。鼓泡方法和调温模型已成功应用于天舟一号发射任务，有效保障了煤油推进剂的温度品质。     

孤立气泡生长过程的短时微重力落塔实验研究

利用中国科学院国家微重力实验室北京落塔提供的3.6s微重力时间开展了短时微重力条件下的池沸腾实验研究, 分析了微重力条件下孤立的单个气泡生长过程特征. 实验中采用掺杂磷的N型光滑硅片作为加热面(加热片尺寸10mm×10mm×0.5mm), 以含气率0.0046 (气液摩尔分数比)的FC-72作为工质, 利用恒流源对加热片通电加热. 通过对实验观测到的单个气泡生长图像及相应传热数据分析可知, 经典传热机制控制的气泡生长模型可以描述其早期特征. 相关模型中经验参数的拟合结果在文献报道的数值范围内, 表明重力对气泡生长早期影响较小, 但较大的气泡尺寸可以提供更准确的数值结果.      

微重力池沸腾传热研究

对利用中国返回式卫星搭载开展的两次微重力池沸腾空间实验及地基常重力和落塔短时微重力实验的结果进行了评述. 研究发现微重力时丝状加热器沸腾传热会略有强化, 而平板加热器则在高热流条件下明显恶化. 微重力时, 气泡脱落前存在沿加热面的横向运动, 加剧了相邻气泡间的合并, 合并气泡会在其表面振荡作用下从加热面脱落. Marangoni 效应对于微重力气泡行为有重要影响.      

Relative ionizations in the nearest interstellar gas

We compare CLOUDY predictions for the equilibrium ionization in the interstellar cloud surrounding the solar system with pick-up ion data. The incident radiation field includes contributions from hot stars, the emission from the conductive cloud boundary and the diffuse FUV back-ground. To within the observational uncertainties, CLOUDY predictions for the ratios n(He)/n(O), n(N)/n(O), n(Ne)/n(O), and n(He)/n(Ne) are consistent with pick-up ion data, provided that O and N are filtered by 50% in the heliopause region and the outer heliosphere as predicted by others. Thus, the steady-state ionization model and assumed radiation field appear approximately valid. However, the youth and low intervening column density towards the Vela pulsar leave open the possibility that the parent supernova explosion 10,500 years ago, and 200 pc distant, may also have affected LISM ionization, although the mechanism is uncertain. Support for this last possibility is provided by the apparent signature of the Vela explosion in the terrestrial geological record.Abbreviations ISM Interstellar Medium - FUV Far Ultraviolet - EUV Extreme Ultraviolet - SNR SN remnant - SXRB SXR Background - LISM Local Interstellar Matter     

重力对单气泡生长特性的影响

采用VOF (Volume of Fluid)多相流模型, 通过用户自定义函数UDF (User Defined Function)实现相变过程中质量和能量的输运, 对微重力条件下尺寸为10mm × 10mm × 25mm的矩形通道的池沸腾现象进行数值模拟, 得到了微重力及常重力作用下单个气泡生长特性的差异. 模拟结果表明, 微重力条件下气泡周围的流线与温度场的分布有显著差异; 由于表面张力作用, 微重力下的气泡脱离特性与常重力下不同; 在微重力条件下, 气泡直径的变化比较复杂, 并与重力加速度的大小有关; Marangoni流对微重力下的流动影响很大, 使换热系数波动, 而且波动的幅度随重力加速度的减小而增大.