一种便携式高精度超声流量仪

研究一种超声波传播方向平行于液体流动方向的流量管和以此为基础的超声流量仪。针对流量系统的新型流量管结构推导两种流量算法并进行误差分析,其中一种算法可以减小由声速变化引起的误差,从而提高系统的测量稳定性,也为流量管的改进方向提供了思路。使用测显比曲线修正管道中流体流速分布不均匀的影响以提升测量准确性,试验证明,在测量范围内,系统测量的平均示值误差不超过0.2%。     

Statistical Relationships between Solar, Interplanetary, and Geomagnetospheric Disturbances, 1976–2000

Within the framework of the Space Weather program, 25-year data sets for solar X-ray observations, measurements of plasma and magnetic field parameters in the solar wind, and D _st index variations are analyzed to reveal the factors that have had the greatest influence on the development of magnetospheric storms. The correlation between solar flares and magnetic storms practically does not exceed a level of correlation for random processes. In particular, no relation was found between the importance of solar flares and the minimum of the D _st index for storms that could be connected with considered flares by their time delay. The coronal mass ejections (CME; data on these phenomena cover a small part of the interval) result in storms with D _st < –60 nT only in half of the cases. The most geoeffective interplanetary phenomena are the magnetic clouds (MC), which many believe to be interplanetary manifestations of CMEs, and compressions in the region of interaction of slow and fast streams in the solar wind (the so-called Corotating Interaction Region, CIR). They correspond to about two-thirds of all observed magnetic storms. For storms with –100 < D _st < –60 nT, the frequencies of storms from MC and CIR being approximately equal. For strong storms with D _st < – 100 nT, the fraction of storms from MC is considerably higher. The problems of reliable prediction of geomagnetic disturbances from observations of the Sun and conditions in interplanetary space are discussed.     

Numerical investigation on gas–particle flows in horizontal channel under the reduced gravity environments

A unified second-order-moment gas–particle two-phase turbulent model incorporated with kinetic theory of granular flows (USM-θ) is developed to study the particle dispersion behavior of dense gas–particle flows in horizontal channel with 6.96 μm wall roughness and with earth, lunar and microgravity environments, respectively. Anisotropy of gas and particle two-phase stresses and the interaction between two-phase stresses are fully considered by constructing two-phase Reynolds stress model and the transport equation of two-phase stress correlation. The flow behavior of particles in a horizontal channel of Kussin and Sommerfeld [12] experiments is numerically simulated. Results show that the reduced gravity conditions affect the particle concentration distribution, particle velocity and fluctuation velocity, particle temperature, axial–axial fluctuation velocity correlation of gas and particle and particle collision frequency. Under microgravity conditions, particle temperature and collision frequency are much less than those of earth and lunar gravity. Compared with earth gravity, anisotropic of two-phase flow and sedimentation are weaker.     

Statistical Approach to the Evaluation of the Mean Correlation Length and the Propagation Velocity of Middle-Scale Plasma Structures in the Earth's Foreshock

Based on simultaneous measurements of ion fluxes made onboard the closely separated satellites Interball-1and Magion-4, the propagation velocity of middle-scale plasma structures in the Earth's foreshock relative to the solar wind flow is estimated. The derived value of this velocity allows these structures to be identified as a fast magnetosonic wave propagating upstream of the solar wind inflowing the Earth's bow shock. An evaluation is also made of the correlation length of these disturbances in the plane perpendicular to the Sun–Earth line. This length is approximately equal to 2R _E.     

返回舱再入过程密封舱气体泄漏计算研究

为分析返回舱再入过程中密封舱漏孔内外压差,并对漏孔变流量充气过程进行研究,采用离散化分析方法将返回舱再入过程分成若干个阶段,针对容积为14 m~3的密封舱和面积为10 cm~2的漏孔,计算并获得了密封舱内外压差、漏孔质量流率、漏孔流速等参数在50~5 km范围内随高度下降的变化规律。结果表明:在高度5 km开伞时刻,漏孔质量流率达到最大值0.134 kg/s,舱内外压差趋近于最大值,约20 172 Pa;返回舱下降过程中漏孔流速在148.4~181.5 m/s之间,处于亚声速区;漏孔气体流速与漏孔面积大小无关,仅与漏孔内外压力及漏孔进口空气密度有关。以上研究结果可为密封舱结构强度设计、伞舱弹伞设计提供参考。     

Directional Solidification Using a Baffle in Microgravity

Numerical simulations were performed to optimize the conditions and parameters for directional solidification of Te-doped GaSb in reduced gravity ranging from 10⁻³ to 10⁻⁵g₀. Our key goal was to quantify the velocity and concentration fields with and without a baffle present in the melt. The effect of the distance of the baffle from the solid–liquid interface was investigated. When the baffle is placed 0.5 cm from the solid–liquid interface, acceleration of 10⁻³g₀ does not cause significant interference with segregation. Furthermore, the flow between the baffle and the interface (low Reynolds number “creeping” flow) does not depend on fluid properties (viscosity).     

Thermocapillary simulation of single bubble dynamics in zero gravity

The lack of significant buoyancy effects in zero gravity conditions poses an issue with fluid transfer in a stagnant liquid. In this paper bubble movement in a stagnant liquid is analysed and presented numerically using a computational fluid dynamics (CFD) approach. The governing continuum conservation equations for two phase flow are solved using the commercial software package Ansys-Fluent v.13 and the Volume of Fluid (VOF) method is used to track the liquid/gas interface in 2D and 3D domains. The simulation results are in reasonable agreement with the earlier experimental observations, the VOF algorithm is found to be a valuable tool for studying the phenomena of gas–liquid interaction. The flow is driven via Marangoni influence induced by the temperature difference which in turn drives the bubble from the cold to the hot region. A range of thermal Reynolds (Re_T) and Marangoni numbers (Ma_T) are selected for the numerical simulations, specifically Re_T=13–658 and Ma_T=214–10,721 respectively. The results indicate that the inherent velocity of bubbles decreases with an increase of the Marangoni number, a result that is line with the results of previous space experiments (Kang et al., 2008) [1]. An expression for predicting the scaled velocity of bubble has been derived based on the data obtained in the present numerical study. Some three-dimensional simulations are also performed to compare and examine the results with two-dimensional simulations.     

Two-phase flow effect on hybrid rocket combustion

This study numerically explores the aerodynamic and combustion processes in a hybrid rocket combustor, under a two-phase turbulent flow environment, considering the evaporation, combustion and drag of droplet and droplet ignition criterion. The predictions of temperature, reaction mode, reactant mass fraction, velocity, oxidizer consumption, fuel regression and droplet number distribution enhance understanding of the two-phase combustion aerodynamics inside the combustor. A parametric study of the inlet spray pattern, including spray cone angle, spray injection velocity and droplet size, is performed to improve the operation of reactant mixing and higher fuel regression rate. Analytical results indicate that both the oxidizer consumption and the fuel regression increase with increasing spray cone angle and spray injection velocity in the practical range of operation. However, for stoichiometric operation, the superior spray cone angle is within 20–60°, and spray injection velocity within 20–40 m/s, under a volume-mean droplet radius of 50 μm. The power dependence of solid-fuel regression on total mass flux is found to decrease with rising of droplet mean size.     

Bursts of geomagnetic pulsations in the frequency range 0.2-5 Hz excited by large changes of the solar wind pressure

We present the results of studying the magnetospheres’s response to sharp changes of the solar wind flow (pressure) based on observations of variations of the ions flux of the solar wind onboard the Inreball-1 satellite and of geomagnetic pulsations (the data of two mid-latitude observatories and one auroral observatory are used). It is demonstrated that, when changes of flow runs into the magnetosphere, in some cases short (duration ~ < 5 min) bursts of geomagnetic pulsations are excited in the frequency range Δf~ 0.2–5 Hz. The bursts of two types are observed: noise bursts without frequency changes and wide-band ones with changing frequency during the burst. A comparison is made of various properties of these bursts generated by pressure changes at constant velocity of the solar wind and by pressure changes on the fronts of interplanetary shock waves at different directions of the vertical component of the interplanetary magnetic field.     

Distribution of velocities of potentially hazardous objects

Velocities of potentially hazardous objects (asteroids and comets) approaching the Earth are studied. It is shown that for an overwhelming majority of objects the velocity of approach does not exceed 40 km/s. The acceptability of this estimate for design and manufacturing of instruments for detecting hazardous celestial bodies is discussed.     

Influence of Solar Wind Parameters on the Level of Geomagnetic Field Fluctuations

We investigated the dependence of the geomagnetic activity index K _p on the velocity and density of the solar wind and the intensity of the interplanetary magnetic field (IMF). A three-layer neural network was used to create the model. The degree of the influence of input parameters on K _p was determined by the value of the mean and root-mean square deviations of the model index values from the real indices. It was found that the largest contribution to the K _p index is provided by the Z component of the IMF, the velocity and density of the solar wind measured with a delay from 0 to 3 h relative to the studied value of K _p, and the previous value of the index itself. For the model with such a set of input parameters, the correlation coefficient between model and real series is ±0.89. The analysis of deviations from the real values of K _p showed that high indices are simulated worse than low indices. In order to solve this problem the data distribution was reduced to a uniform distribution over K _p, and this considerably decreased the standard deviations for large values of K _p.     

基于碱金属辅助电离的等离子鞘套模拟方法

为解决再入过程中通信黑障与探测异常问题，对等离子体鞘套地面模拟方法进行了研究。以RAM C-II 飞行试验为依据，计算了等离子体鞘套的参数范围。分析现有模拟设备，概括提出了高焓低速风洞的模拟方案，选取相适应的放电方式，并对流量功率进行了计算。针对高温环境对电磁设备造成损坏以及所需功率难以实现的问题，提出添加碱金属的解决方案，并进行了试验验证。试验结果表明，添加碱金属可以使电子密度提升约一个数量级。对方案效果进行评估，预期功率需求降至兆瓦量级。     

Acceleration of solar cosmic rays and the fine spectral structure of type II radio bursts

On the basis of data, obtained by means of the ground-based solar service RSTN (Radio Solar Telescope Network) and the geostationary satellite system GOES, the relationship between the solar cosmic rays (SCR) intensity I _p with the proton energy E _p > 1 MeV and parameters of meter-decameter type II radio bursts in the frequency range of 25–180 MHz is studied. The process of proton acceleration by shock waves was characterized by the frequency drift velocity of radio bursts V _mII and the relative difference between radio emission frequencies at the first two harmonics b. It is shown that the coefficient of correlation between I _p and b increases with E _p growing from 0.40 to 0.70, while a similar coefficient between I _p and V _mII does not exceed 0.30. Indications in favor of the two-stage SCR acceleration model are obtained.     

SIMULATION OF A THERMAL SOLAR POWER PLANT OPERATING ON MARS UNDER CLEAR SKY AND DUST STORM CONDITIONS

The power plant analyzed in this work consists of a selective solar collector–thermal engine combination. The paper focuses on solar power plant operation under various weather conditions during all seasons on Mars. Meteorological data measured at Viking Landers (VL) sites were used in computations. Two strategies to collect solar radiation were analyzed: a solar horizontal (H) collector and a solar collector whose tilt and orientation are continuously adjusted to keep the receiving surface perpendicular to Sun rays (P). Both a low and a high efficiency thermal engine were considered. All the computations were performed for a selective solar flat-plate collector similar in size to the Mars Pathfinder's Sojourner. Results show that generally the influence of latitude on performance is important. In some situations, the meteorological effects compensate the latitudinal effects and the output power is quite similar at both VL1 and VL2 sites. In case a low-efficiency engine is coupled to a horizontal collector, the solar efficiency does not exceed 0.13 at VL2 site. It is lower during summer and higher during winter dust storms. In case the low-efficiency engine is coupled to a P collector, the solar efficiency increases during summer. The solar efficiency is as high as 0.18 in case of a horizontal collector attached to a high-efficiency engine. If the high-efficiency thermal engine is connected to a P collector the solar efficiency increases significantly during summer and spring but does not exceed 0.18. The power provided by a system consisting of a horizontal collector and a low-efficiency engine does not exceed 7 W. Using a high engine coupled to a horizontal collector leads to a power output up to 13 W during spring, autumn and winter. The P collector is recommended mainly during summer and spring in combination with high-efficiency engines. In this case the solar efficiency could be as high as 25 W. The performance of PV cell power systems and properly designed dynamic solar power plants operating on Mars is comparable.     

Evolution of salt finger convection with steady wind shear

In oceanographics situations where salt fingers may be an important mechanism for the transport of heat and salt in the vertical direction, velocity shears may also be present. Salt finger convection is analogous to Bénard convection in that the kinetic energy of the motions is obtained from the potential energy stored in the unstable distribution of a stratifying component. On the basis of the thermal analogy it is of interest to discover whether salt fingers are converted into two-dimensional sheets by wind shear, and how the vertical fluxes of heat and salt are changed by wind shear. Salt finger convection under the effect of steady wind shear is theoretically examined in this paper. The evolution of instability developing in the presence of a vertical density gradient disturbance and the horizontal Couette flow is considered near the onset of salt fingers under a moderate rate of shear. We use velocity as the basic variable and solve the pressure Poisson equation in terms of the associated Green function. Growth competition between the longitudinal rolls (LR) and the transverse rolls (TR), whose axes are, respectively, in the direction parallel to and perpendicular to the Couette flow, is investigated by the weakly nonlinear analysis of coupled-mode equations. The results show that the TR mode is stable under a small wind shear and the LR mode is stable for a higher wind shear.     

双脉冲发动机点火过程三维数值模拟

以喷射棒式双脉冲发动机燃烧室、级间隔离装置和喷管一体化为研究对象,采用数值仿真技术对Ⅱ脉冲点火过程三维流场特性进行分析研究。计算结果表明,点火初期燃气压力波峰超前于火焰峰到达级间隔离装置,并以压强冲击波形式传播,Ⅱ脉冲燃烧室相对高压区位置不断发生改变;级间孔打开过程对药柱末端压强影响较大,但对Ⅱ脉冲燃烧室压强整体上升过程影响较小;级间孔打开后,燃气经级间孔加速后形成高度欠膨胀射流,并在Ⅰ脉冲燃烧室内形成非对称带状低压区;级间孔分布的非对称性,导致压强及温度在发动机燃烧室中呈现显著的三维分布特性;高温区出现在隔板附近,而在装药前端、装药末端及外围级间孔轴线附近出现低温区。     

Activation of the tail open part during the magnetospheric storm

In each polar cap (PC) we mark out “old PC” observed during quiet time before the event under consideration, and “new PC” that emerges during the substorm framing the old one and expanding the PC total area. Old and new PCs are the areas for the magnetosphere old and new tail lobes, respectively. The new lobe variable magnetic flux Ψ₁ is usually assumed to be active, i.e. it provides the electromagnetic energy flux (Poynting flux) ɛ′ transport from solar wind (SW) into the magnetosphere. The old lobe magnetic flux Ψ₂ is supposed to be passive, i.e. it remains constant during the disturbance and does not participate in the transporting process which would mean the old PC electric field absolute screening from the convection electric field created by the magnetopause reconnection. In fact, screening is observed, but far from absolute. We suggest a model of screening and determine its quantitative characteristics in the selected superstorm. The coefficient of a screening is the β = Ψ₂/Ψ₀₂, where Ψ₀₂ = const is open magnetic flux through the old PC measured prior to the substorm, and Ψ₂ is variable magnetic flux through the same area measured during the substorm. We consider three various regimes of disturbance. In each, the coefficient β decreased during the loading phase and increased at the unloading phase, but the rates and amplitudes of variations exhibited a strong dependence on the regime. We interpreted decrease in β as a result of involving the old PC magnetic flux Ψ₂, which was considered to be constant earlier, in the Poynting flux ɛ′ transport process from solar wind into the magnetosphere. Transport process weakening at the subsequent unloading phase creates increase in β. Estimates showed that coefficient β during each regime and the computed Poynting flux ɛ′ varied manifolds. In general, unlike the existing substorm conception, the new scenario describes an unknown earlier of tail lobe activation process during a substorm growth phase that effectively increases the accumulated tail energy for the expansion and recovery phases.     

Analysis of Low-Frequency Microaccelerations onboard the Foton-11Satellite

The method and the results of investigating the low-frequency component of microaccelerations onboard the Foton-11satellite are presented. The investigation was based on the processing of data of the angular velocity measurements made by the German system QSAM, as well as the data of measurements of microaccelerations performed by the QSAM system and by the French accelerometer BETA. The processing was carried out in the following manner. A low-frequency (frequencies less than 0.01 Hz) component was selected from the data of measurements of each component of the angular velocity vector or of the microacceleration, and an approximation was constructed of the obtained vector function by a similar function that was calculated along the solutions to the differential equations of motion of the satellite with respect to its center of mass. The construction was carried out by the least squares method. The initial conditions of the satellite motion, its aerodynamic parameters, and constant biases in the measurement data were used as fitting parameters. The time intervals on which the approximation was constructed were from one to five hours long. The processing of the measurements performed with three different instruments produced sufficiently close results. It turned out to be that the rotational motion of the satellite during nearly the entire flight was close to the regular Eulerian precession of the axially symmetric rigid body. The angular velocity of the satellite with respect to its longitudinal axis was about 1 deg/s, while the projection of the angular velocity onto the plane perpendicular to this axis had an absolute value of about 0.2 deg/s. The magnitude of the quasistatic component of microaccelerations in the locations of the accelerometers QSAM and BETA did not exceed 5 × 10^–5–10^–4m/s²for the considered motion of the satellite.     

高超声速边界层转捩特性试验探究

通过在激波风洞中开展转捩试验,选取来流马赫数分别为6和8,单位雷诺数分别为4.1×10 6m -1 、2.6×10 7m -1 和4.4×10 7m -1 的来流条件,研究马赫数、单位雷诺数以及攻角变化对钝锥边界层和平板边界层转捩位置的影响。结果表明,攻角增大使钝锥迎风面和背风面边界层转捩位置均前移,使平板边界层转捩位置也前移;钝锥边界层在低马赫数时更容易转捩,平板边界层转捩受马赫数影响在攻角有差异时有所不同;单位雷诺数的增大促进转捩,但对于钝锥边界层而言,该参数增加到试验选定的上限时,转捩位置的变化并不明显;在转捩过程中平板边界层的脉动压力系数与热流具有相同的变化趋势。试验捕捉到了第二模态扰动。     

Manifestations of sudden commencement of a severe magnetic storm of November 20, 2003, in generation of an SC pulse, <Emphasis Type="Italic">P</Emphasis><Subscript>SC</Subscript> pulsations,and spatial modulation of the auroral brightness

The results of investigation of the geomagnetic and auroral response to the commencement of a severe magnetic storm of November 20, 2003, are presented. It is established that the onset of SC led to the brightening of the auroral arc in the dusk sector for 2–3 min with its extent to the east with a velocity of 10–20 km/s and to displacement poleward with a velocity of 1.0 km/s. Furtheron, the fast auroral expansions of short duration (5 min) to the pole up to 2–4°were observed, repeating every 5–10 min during 40 min, which led to the spatial modulation of the brightness of the glow and to generation of P_SC pulsations with similar periods of oscillations. The broadening of aurora poleward had a steplike character, with generation of new arcs poleward of previous ones 5 arcs per 1.5 min. The modulation of brightness of the glow and P_SC were observed against the background of intensification of a two-cell DP2 type current system and were accompanied by multiple turnings of the IMF B_z from south to north and back. It is assumed that the source of P_SC pulsations was a modulation of the intensity of the DP2 ionosphere currents as a result of variations of the magnetosphere convection level.Translated from Kosmicheskie Issledovaniya, Vol. 42, No. 6, 2004, pp. 608–615.Original Russian Text Copyright © 2004 by Baishev, Borisov, Velichko, Solovyev, Yumoto.