洛仑兹力控制高超声速进气道边界层分离的数值模拟

采用空间HUE格式、时间LU-SGS推进、sst-kw湍流模型、多块结构网格程序,对磁流体动力学(Magnetohydrodynamic:MHD)控制高超声速二维进气道边界层分离进行了数值研究.研究发现,不施加控制时,数值模拟得到的壁面静压和实验结果符合良好,进气道喉道处分离区占据喉道高度的1/3左右.通过施加MHD控制,消除了进气道内部的边界层分离,总压恢复系数从0.502提高到0.56,喉道处流场畸变系数减小了18.6%.     

振荡燃烧过程的同步测量方法

振动燃烧是由非稳定燃烧放热和压力脉动互相耦合产生的系统振荡过程。振荡燃烧的研究方法之一是对自激振荡燃烧相互耦合过程进行研究,得到系统的闭环特性。另外还可以对燃烧系统施加特定的扰动以得到燃烧系统的开环特性。为了研究振荡燃烧的动态过程,需要实现不同物理量的同步测量。相同步方法能够实现压力脉动与燃烧放热率脉动的同步测量,确定二者间的周期变化关系。通过对两个不同振荡类型的实验台进行相同步测量,分析振荡燃烧过程中压力脉动与放热率脉动的相位关系,并讨论了相同步方法的误差,提出了不同实现方案。这些结果将有助于我们提高火焰测量的相同步技术的准确性。     

一种求解细线瞬态散射的稳定算法

利用时间步进方法(MOT)求解脉冲电场照射下细线的电流响应分布,分析其后期稳定性。提出一种新的电流系数平均法,不仅可以改善前面时间步的电流值,而且能对当前时间步的电流值进行判断,并采取措施预防振荡,有效消除迭代计算的累积误差,改善后期不稳定性问题。数值仿真表明,新方法消除了引起后期振荡的高频分量,获得了稳定的电流响应分布。     

一种具有电压支撑功能的改进无功注入策略

电压跌落是输配电系统面临的最严重的问题之一。随着分布式光伏电源在电力系统中的渗透率越来越高,国内外最新标准要求光伏逆变器必须具备低电压穿越能力。为了消除有功功率振荡,在传统的正/负序控制基础上提出了一种改进的有功/无功注入策略;针对现有电压支撑方法缺乏电压抬升范围控制,将三相电压幅值作为控制目标,详细推导了适用于不同电压跌落情况下的数学模型,得出为保证各相电压均保持在安全运行范围之内所需注入无功功率参考值。仿真结果验证了所提策略的正确性和有效性。     

A swept fin-induced flow field with different height mounting gaps

In order to apply the air fin successfully and ensure the maneuverability of hypersonic vehicle, a key problem to be studied urgently is the heat flux brought by the fin mounting gap. The appearance of mounting gap and fin shaft can induce many complex flow structures which need more attentions to be investigated. Under Ma 6, Nano-tracer-based Planar Laser Scattering (NPLS) and Temperature Sensitive Paints (TSP) were applied to visualize and measure transient flow structures and heat flux distribution of a swept fin-induced flow field with different height mounting gaps. Complementarily, Reynolds-averaged N-S equations were solved with k-ω SST turbulent model. The heat flux distribution results of numerical simulation and TSP observed the change of high heat flux region with different mounting gap, both in position and magnitude. The streamlines based on Computational Fluid Dynamics (CFD) and flow visualization results obtained by NPLS revealed the cause of high heat flux region. The high heat flux region in this flow field is mainly related to the reattachment of vortex and flow stagnation. The increase of gap height can lead to stronger gap overflow and shaft-induced horseshoe vortex, which are source of the high heat flux around the fin. The case with the highest mounting gap (4 mm) en-counters the most severe aerodynamic heating, both on the surface of fin and plate. Thus, under the premise of ensuring the flexibility of the fin, the gap should be set as small as possible.     

Solar cycle variation of “killer” electrons at geosynchronous orbit and electron flux correlation with the solar wind parameters and ULF waves intensity

To construct models for hazard prediction from radiation belt particles to satellite electronics, one should know temporal behavior of the particle fluxes. We analyzed 11-year variation in relativistic electron flux (E>2 MeV) at geosynchronous orbit using measurements made by GOES satellites during the 23rd sunspot cycle. As it is believed that electron flux enhancements are connected with the high-speed solar wind streams and ULF or/and VLF activity in the magnetosphere, we studied also solar cycle changes in rank order cross-correlation of the outer radiation belt electron flux with the solar wind speed and both interplanetary and on-ground wave intensity. Data from magnetometers and plasma sensors onboard the spacecraft ACE and WIND, as well as magnetic measurements at two mid-latitude diametrically opposite INTERMAGNET observatories were used. Results obtained show that average value of relativistic electron flux at the decay and minimum phases of solar activity is one order higher than the flux during maximum sunspot activity. Of all solar wind parameters, only solar wind speed variation has significant correlation with changes in relativistic electron flux, taking the lead over the latter by 2 days. Variations in ULF amplitude advance changes in electron flux by 3 days. Results of the above study may be of interest for model makers developing forecast algorithms.     

Variations of the solar acoustic high-degree mode frequencies over solar cycle 23

Using full-disk observations obtained with the Michelson Doppler Imager (MDI) on board the Solar and Heliospheric Observatory (SOHO) spacecraft, we present variations of the solar acoustic mode frequencies caused by the solar activity cycle. High-degree (100 < ? < 900) solar acoustic modes were analyzed using global helioseismology analysis techniques over most of solar cycle 23. We followed the methodology described in details in [Korzennik, S.G., Rabello-Soares, M.C., Schou, J. On the determination of Michelson Doppler Imager high-degree mode frequencies. ApJ 602, 481–515, 2004] to infer unbiased estimates of high-degree mode parameters ([see also Rabello-Soares, M.C., Korzennik, S.G., Schou, J. High-degree mode frequencies: changes with solar cycle. ESA SP-624, 2006]). We have removed most of the known instrumental and observational effects that affect specifically high-degree modes. We show that the high-degree changes are in good agreement with the medium-degree results, except for years when the instrument was highly defocused. We analyzed and discuss the effect of defocusing on high-degree estimation. Our results for high-degree modes confirm that the frequency shift scaled by the relative mode inertia is a function of frequency and it is independent of degree.     

Cosmic ray acceleration by supernova shocks

We analyse the results of recent measurements of nonthermal emission from individual supernova remnants (SNRs) and their correspondence to the nonlinear kinetic theory of cosmic ray (CR) acceleration in SNRs. It is shown that the theory fits these data in a satisfactory way and provides the strong evidences for the efficient CR production in SNRs accompanied by significant magnetic field amplification. Magnetic field amplification leads to considerable increase of CR maximum energy so that the spectrum of CRs accelerated in SNRs is consistent with the requirements for the formation of Galactic CR spectrum up to the energy ∼10¹⁷ eV.     

On the Velocity and Intensity Asymmetries of Solar P-Mode Lines

We show that to explain the opposite line asymmetries shown by the velocity and intensity spectra, it is necessary to solve the full non-adiabatic problem which is at least of the fourth order. This revised version was published online in June 2006 with corrections to the Cover Date.     

New evidence for strong non-thermal effects in Tycho’s supernova remnant

For the case of Tycho’s supernova remnant (SNR), we present the relation between the blast wave and contact discontinuity radii calculated within the nonlinear kinetic theory of cosmic ray (CR) acceleration in SNRs. It is demonstrated that these radii are confirmed by recently published Chandra measurements which show that the observed contact discontinuity radius is very close to the shock radius. Therefore a consistent explanation of these observations can be given in terms of efficient CR acceleration which makes the medium more compressible.