蒸发管蒸发及雾化特性

为了研究某型发动机中的Γ型蒸发管的蒸发性能,在进口空气为常压条件下进行实验研究.实验采用燃气加热,模拟实际蒸发管工作环境.实验研究气油比、进口空气温度以及蒸发管管壁温度的变化对蒸发管燃油蒸发率及出口索太尔平均直径SMD(Sauter mean diameter)的影响.实验结果表明:气油比(AFR)、蒸发管空气进口温度及蒸发管壁温对蒸发率及SMD都有着很大的影响,气油比的增大和空气进口温度的增大以及蒸发管壁温的提高都会导致燃油蒸发率的增大和出口SMD直径的减小,而三者中壁温的作用最为显著.      

低速单级轴流压气机自引气扩稳实验

在一台低速单级轴流压气机上采用自引气-喷气方式进行了实验研究,实验中分析比较了不同的引气方式对压气机失速裕度改善(SMI)以及对压气机效率的影响,同时对不同自引气方式的扩稳机理进行了探讨.实验结果表明:自引气方式能够有效的改善压气机失速裕度,并且能够略微提高压气机效率.与传统的外部引气相比,节省了外部引气所需要的外部空气压缩系统;为自引气在实际压气机稳定性控制中的应用提供参考.      

辅助动力装置环形回流燃烧室数值研究

利用Fluent软件计算辅助动力装置(auxiliary power unit,简称APU)环形回流燃烧室三维两相喷雾燃烧流场,研究不同进口温度和油气比对两相喷雾燃烧流场的影响,采用标准 k-ε 模型模拟湍流黏性,离散相模型(DPM)追踪油珠运动轨迹,燃烧模型采用非预混平衡化学反应模型.计算结果表明:随着进口温度和油气比的增加,燃烧室出口温度相应增加,但温度分布规律基本保持不变;计算结果与试验测量结果比较吻合,说明采用的数学模型和计算方法可用于预估实际APU回流燃烧室三维两相喷雾燃烧流场.      

基于PIV技术的纵列式双旋翼尾迹特性实验研究

将现有单旋翼实验台进行改装,以适合于纵列式双旋翼的实验研究。基于PIV技术,针对悬停和前飞状态下的纵列式双旋翼时的桨尖涡特性进行了测量。通过改变前后旋翼的水平和轴向间距,调整两旋翼之间的重叠区域,研究了不同气动布局纵列式双旋翼干扰状态下的尾迹结构,并与单旋翼进行了对比。结果表明:悬停状态,随两旋翼纵向间距的增加,桨尖涡的轴向位移也逐渐增大,但桨尖涡径向位移并不是随纵向间距的改变而规律变化,在纵向间距为1.8R附近时最小;而双旋翼轴向间距的变化对桨尖涡的径向和轴向位移均有影响,但变化都不是很大。     

基于升力面自由尾迹的直升机旋翼悬停性能参数影响研究

 最大悬停效率(FM_max)作为衡量旋翼悬停性能的常用指标,反映了旋翼能达到的最大悬停效率,但不能反映旋翼在一定桨叶载荷范围内保持高悬停效率的能力,本文给出了旋翼悬停保持能力的定义.为更准确地反映桨叶涡量分布,建立了基于升力面理论的桨叶气动模型;考虑有弯度翼型的影响,将涡量布置于翼型中弧线,随后基于自由尾迹模型、耦合刚性桨叶挥舞运动方程、翼型动态失速模型以及二阶精度时间步进格式建立了升力面自由尾迹方法.通过计算模型旋翼在不同桨尖马赫数下的悬停效率,并与试验数据对比,验证了方法的准确性.相比于升力线自由尾迹方法,建立的升力面自由尾迹分析方法能显著提高旋翼悬停效率计算精度.最后分析旋翼关键设计参数对悬停性能的影响,得到设计参数影响旋翼悬停保持能力的新规律.     

双三角翼俯仰振荡运动的流场特性数值模拟

 建立了适用于双三角翼大迎角非定常分离流场模拟的数值方法,研究双三角翼俯仰振荡时的动态流场特性,给出动态流场结构和气动力性能随迎角的变化规律,重点考察了减缩频率、转轴位置、平均迎角和振幅等参数对动态流场迟滞效应和气动力曲线迟滞环的影响。研究结果表明:俯仰振荡到相同大迎角时上仰和下俯的流场存在明显差异;减缩频率对气动力迟滞效应的影响相对大于转轴位置;平均迎角的变化导致双三角翼背风区流场结构呈现不同流态,而振幅的大小决定这些流态的数目,事实上俯仰运动时如果跨越的流态数目越多则流场结构的动态响应滞后现象就越显著。通过数值分析,有利于提高对双三角翼在俯仰振荡运动条件下的非定常特性和流场滞后效应等非线性现象的认识。     

一种Ku频段全向高增益天线设计

提出了一种工作于Ku频段的宽频带、高增益和H面全向的新型共面波导（CPW）的中心导体和左右地板交叉连接耦合馈电天线结构设计。csTMws。软件仿真结果表明,该结构在具有较小尺寸的同时,能够有效展宽工作频带和提高增益,并保持天线的全向性。利用CSTMWS。软件对天线表面电流的仿真,解释了天线具有宽带和全向高增益辐射的原因：终端加载的三角形单极天线引起CPW中心带条的电流为行驻波电流,使天线获得了较宽的阻抗带宽;10个天线辐射单元的表面电流近似等幅同相,使天线获得了全向高增益的性能。研制出了工作在Ku频段的CPW交叉连接耦合馈电天线并进行了测试。天线印刷于厚度为0．5mm的FR-4环氧树脂板上,其反射系数低于-10dB时的频带为12．4～13．5GHz,相对带宽达8．5％,H面全向最大增益为6．6dBi,表明测试结果与仿真结果吻合较好。整个天线的尺寸仅为81mm×6．1mm,可应用于Ku频段的通信系统中。     

Day-to-day variability of equatorial anomaly in GPS-TEC during low solar activity period

The ionospheric total electron content (TEC) in the northern hemispheric equatorial ionization anomaly (EIA) crest region is investigated by using dual-frequency signals of the Global Positioning System (GPS) acquired from Rajkot (Geog. Lat. 22.29°N, Geog. Long. 70.74°E; Geom. Lat. 14.21°N, Geom. Long. 144.90°E), India. The day-to-day variability of EIA characteristics is examined during low solar activity period (F10.7∼83 sfu). It is found that the daily maximum TEC at EIA crest exhibits a day-to-day and strong semi-annual variability. The seasonal anomaly and equinoctial asymmetry in TEC at EIA is found non-existent and weaker, respectively. We found a moderate and positive correlation of daily magnitude of crest, Ic with daily F10.7 and EUV fluxes with a correlation coefficient of 0.43 and 0.33, respectively indicating an existence of a short-term relation between TEC at EIA and the solar radiation even during low solar activity period. The correlation of daily Ic with Dst index is also moderate (r = −0.35), whereas no correlation is found with the daily Kp index (r = 0.14) respectively. We found that the magnitude of EIA crest is moderately correlated with solar flux in all seasons except winter where it is weakly related (0.27). The magnitude of EIA crest is also found highly related with EEJ strength in spring (r = 0.69) and summer (r = 0.65) than autumn (0.5) and winter (r = 0.47), though EEJ is stronger in autumn than spring.     

Modelling of galactic Carbon in an asymmetrical heliosphere: Effects of asymmetrical modulation conditions

Observations of galactic cosmic rays (GCRs) from the two Voyager spacecraft inside the heliosheath indicate significant differences between them, suggesting that in addition to a possible global asymmetry in the north–south dimensions (meridional plane) of the heliosphere, it is also possible that different modulation (turbulence) conditions could exist between the two hemispheres of the heliosphere. We focus on illustrating the effects on GCR Carbon of asymmetrical modulation conditions combined with a heliosheath thickness that has a significant dependence on heliolatitude. To reflect different modulation conditions between the two heliospheric hemispheres in our numerical model, the enhancement of both polar and radial perpendicular diffusion off the ecliptic plane is assumed to differ from heliographic pole to pole. The computed radial GCR intensities at polar angles of 55° (approximating the Voyager 1 direction) and 125° (approximating the Voyager 2 direction) are compared at different energies and for both particle drift cycles. This is done in the context of illustrating how different values of the enhancement of both polar and radial perpendicular diffusion between the two hemispheres contribute to causing differences in radial intensities during solar minimum and moderate maximum conditions. We find that in the A > 0 cycle these differences between 55° and 125° change both quantitatively and qualitatively for the assumed asymmetrical modulation condition as reflected by polar diffusion, while in the A < 0 cycle, minute quantitative differences are obtained. However, when both polar and radial perpendicular diffusion have significant latitude dependences, major differences in radial intensities between the two polar angles are obtained in both polarity cycles. Furthermore, significant differences in radial intensity gradients obtained in the heliosheath at lower energies may suggest that the solar wind turbulence at and beyond the solar wind termination shock must have a larger latitudinal dependence.     

Magnetospheric disturbances associated with the 13 December 2006 solar flare and their ionospheric effects over North-East Asia

We present an observational study of magnetospheric and ionospheric disturbances during the December 2006 intense magnetic storm associated with the 4В/Х3.4 class solar flare. To perform the study we utilize the ground data from North–East Asian ionospheric and magnetic observatories (60–72°N, 88–152°E) and in situ measurements from LANL, GOES, Geotail and ACE satellites. The comparative analysis of ionospheric, magnetospheric and heliospheric disturbances shows that the interaction of the magnetosphere with heavily compressed solar wind and interplanetary magnetic field caused the initial phase of the magnetic storm. It was accompanied by the intense sporadic E and F2 layers and the total black-out in the nocturnal subauroral ionosphere. During the storm main phase, LANL-97A, LANL 1994_084, LANL 1989-046 and GOES_11 satellites registered a compression of the dayside magnetosphere up to their orbits. In the morning–noon sector the compression was accompanied by an absence of reflections from ionosphere over subauroral ionospheric station Zhigansk (66.8°N, 123.3°E), and a drastic decrease in the F2 layer critical frequency (foF2) up to 54% of the quite one over subauroral Yakutsk station (62°N, 129.7°E). At the end of the main phase, these stations registered a sharp foF2 increase in the afternoon sector. At Yakutsk the peak foF2 was 1.9 time higher than the undisturbed one. The mentioned ionospheric disturbances occurred simultaneously with changes in the temperature, density and temperature anisotropy of particles at geosynchronous orbit, registered by the LANL-97A satellite nearby the meridian of ionospheric and magnetic measurements. The whole complex of disturbances may be caused by radial displacement of the main magnetospheric domains (magnetopause, cusp/cleft, plasma sheet) with respect to the observation points, caused by changes in the solar wind dynamic pressure, the field of magnetospheric convection, and rotation of the Earth.