圆柱状含液体介质的空间辐射器的传热效率

给出了求解典型圆柱状态含液体介质的空间辐射器传热效率的解析计算公式,降低了辐射器传热效率计算的复杂度,通过与数值计算结果的比对分析,认为用流体入口温度代替辐射器平均温度的假设在工程上是能够接受的,其引起的偏差小于5%。     

Detailed magnetic structure and stochastic threshold

Non-linear evolution of reconnection is too slow to explain-by itself-fast phenomena such as internal disruptions in tokamaks or flares in the solar atmosphere. It has been proposed that the change in topology could lead to field line stochastization, and hence to highly increased transport. An important objection to this idea is that the increase of transport coefficients should smoothly follow the amplitude of the perturbation, while the observations show a catastrophic transition. We have shown 1) that the shape of the structures (and not only their size or amplitude) evolve during non-linear evolution 2) that the stochastic threshold can be strongly influenced by the detailed shape. Therefore, sharp transitions can appear during the evolution, due to the combination of these two effects. We will first consider an idealized situation, namely the two-waves problem in slab geometry, for which we will study the effect of the separatrix shape on the stochastic threshold. In the second part, we will present an application to the internal disruption in tokamaks, with anm=1 perturbation in a toroidal magnetic configuration. In the last part, we will discuss possible applications of the studies on shape effects to the behaviour of trapped particles in structures of the solar atmosphere.     

基于软件锁相环的电机速度控制系统

随着电力电子、微电子技术和控制技术的发展，一些场合对电机调速系统性能的要求越来越高，而锁相调速控制在稳速精度方面有其独特的优势。文章在改进的数字锁相环基础上，提出了软件锁相环电机速度控制系统，利用高性能微处理器实现了软件锁相环。     

微分变压器用于宽频数字信号隔离

用微分变压器取代积分变压器实现数字信号隔离，不仅有利于箭上设备小型化，还可提高隔离性能，改善电磁兼容（ＥＭＣ）性。文中分析了积分变压器隔离电路的缺点和局限性。展宽频域下限的一种有效途径是使用微分变压器，它的工作条件易于满足，可小型化，且频率下限低至毫赫级。文中给出了计算公式和电路。为了恢复变形的波形，给出了迟滞整形电路，本方案优点是增强了抗干扰能力，提高测量精度，延长传输距离。     

Solar cycle effect on temporal and spatial variation of topside ion density measured by SROSS C2 and ROCSAT 1 over the Indian longitude sector

We investigated the diurnal, seasonal and latitudinal variations of ion density Ni over the Indian low and equatorial topside ionosphere within 17.5°S to 17.5°N magnetic latitudes by combining the data from SROSS C2 and ROCSAT 1 for the 9 year period from 1995 to 2003 during solar cycle 23. The diurnal maximum density is found in the local noon or in the afternoon hours and the minimum occurs in the pre sunrise hours. The density is higher during the equinoxes as compared to that in the June and December solstice. The local time spread of the daytime maximum ion density increases with increase in solar activity. A north south asymmetry with higher ion density over northern hemisphere in the June solstice and over southern hemisphere in December solstice has been observed in moderate and high solar activity years. The crest to crest distance increases with increase in solar flux. Ion density bears a nonlinear relationship with F_10.7 cm solar flux and EUV flux in general. The density increases linearly with solar flux up to ∼150 sfu (1 sfu = 10⁻²²Wm⁻²Hz⁻¹) and EUV flux up to ∼50 units (10⁹ photons cm⁻² s⁻¹). But beyond this the density saturates. Inverse saturation and linear relationship have been observed in some season or latitude also. Inter-comparison of the three solar activity indices F_10.7 cm flux, EUV flux and F_10.7P (= (F_10.7 + F_10.7A)/2, where F_10.7A is the 81 day running average value of F_10.7) shows that the ion density correlates better with F_10.7P and F_10.7 cm fluxes. The annual average daytime total ion density from 1995 to 2003 follows a hysteresis loop as the solar cycle reverses. The ion density at 500 km over the Indian longitude sector as obtained by the international reference ionosphere is in general lower than the measured densities during moderate and high solar activity years. In low solar activity years the model densities are equal or higher than measured densities. The IRI EIA peaks are symmetric (±10°) in equinox while densities are higher at 10°N in June solstice and at 10°S in the December solstice. The model density follows F_10.7 linearly up to about F_10.7 > ∼150 sfu and then saturates.     

On the nature of coronal loops above the quiet sun network

The structure and dynamics of a box in a stellar corona can be modeled employing a 3D MHD model for different levels of magnetic activity. Depending on the magnetic flux through the surface the nature of the resulting coronal structures can be quite different. We investigate a model of an active region for two sunspots surrounded by magnetic field patches comparable in magnetic flux to the sunspots. The model results in emission from the model corona being concentrated in loop structures. In Gudiksen and Nordlund (2005) the loops seen in EUV and X-ray emission outline the magnetic field, following the general paradigm. However, in our model, where the magnetic field is far from a force-free state, the loops seen in X-ray emission do not follow the magnetic field lines. This result is of interest especially for loops as found in areas where the magnetic field emerging from active regions interacts with the surrounding network.     

Supersonic flow over a pitching delta wing using surface pressure measurements and numerical simulations

Experimental and numerical methods were applied to investigating high subsonic and supersonic flows over a 60° swept delta wing in fixed state and pitching oscillation.Static pressure coefficient distributions over the wing leeward surface and the hysteresis loops of pressure coefficient versus angle of attack at the sensor locations were obtained by wind tunnel tests.Similar results were obtained by numerical simulations which agreed well with the experiments.Flow structure around the wing was also demonstrated by the numerical simulation.Effects of Mach number and angle of attack on pressure distribution curves in static tests were investigated.Effects of various oscillation parameters including Mach number, mean angle of attack, pitching amplitude and frequency on hysteresis loops were investigated in dynamic tests and the associated physical mechanisms were discussed.Vortex breakdown phenomenon over the wing was identified at high angles of attack using the pressure coefficient curves and hysteresis loops, and its effects on the flow features were discussed.     

Statistical study of twist values of transequatorial loops and the relationship with flares

In this paper, the twist values of ‘S’-shape transequatorial loops (TLs) from 1991 to 2001 are calculated, GOES soft X-ray flares dataset of the active regions connected by these TLs are investigated. The result shows the twist value of the TLs has a weak relation with the flare flux. There is no clear correlation between the twist value and the distance between the footpoint of TLs and location of flare in the corresponding active regions.     

Experimental study of hysteresis and catastrophe in a cavity-based scramjet combustor

Hystereses and catastrophes were experimentally investigated in a cavity-based scramjet combustor. The inflow Mach number was 3.0. Fuel Equivalence Ratio(ER) was continuously regulated with multi-steps to explore influences of historical regulation directions on combustion states. Two divided hysteresis loops with catastrophes were observed. By 1-D flow estimations,the first loop occurred with shock-free/separated scramjet mode transitions, while the second kept in the separated scramjet mode. T...     

双模态冲压发动机中的模态转换研究综述

在以双模态冲压发动机为推进装置的高超声速飞行器的加速过程中,燃烧室内的释热量及其分布必须做出相应的调整,使得发动机从亚燃模态转换为超燃模态。在模态转换过程中,由于燃烧室下游边界条件突然从热力壅塞状态变为无壅塞状态,其壁面压力分布会发生明显改变。这将使作用在飞行器上的推力和动量发生突然变化,可能会导致飞行器失去控制。因此,如何实现不同燃烧模态的平稳转换,是燃烧室设计中的技术难点。本文详细介绍了双模态冲压发动机中不同燃烧模态的定义和判定准则、模态转换的实现方式、模态转换的机理,以及在模态转换时可能存在的激波反射结构转换迟滞和火焰结构转换迟滞现象。 