微气泡发射沸腾形成机理

为了探究具有超高换热性能的微气泡发射沸腾现象的形成机理,采用FLUENT软件对加热面上单个气膜周围的速度场进行数值模拟,并与实验结果进行对比.实验结果表明,对于水,微气泡发射沸腾现象发生时,加热壁面上会出现气膜破裂的过程,并且过冷度和壁面过热度的升高会加剧这一过程.对于酒精,微气泡发射沸腾现象很难发生.计算结果表明,在过冷条件下气膜周围存在marangoni对流,对于水而言,过冷度和壁面过热度的升高会增强气膜周围的marangoni对流过程,而在酒精气膜周围 marangoni对流相对较弱.因此由气膜周围强烈的marangoni对流过程引起的气液界面上的扰动可能造成气膜破裂,这可能是微气泡发射沸腾现象形成的原因之一.      

Study of mid-latitude ionospheric convection during quiet and disturbed periods using the SuperDARN Hokkaido radar

Westward ionospheric convective flows around midnight are frequently observed at mid-latitudes. They can be generated by so-called disturbance dynamo mechanisms working mainly in the mid-latitudes. To understand the influence of disturbance dynamo effects in the mid-latitudes, we studied the latitudinal distribution of westward flows in association with several kinds of geomagnetic disturbances using the SuperDARN Hokkaido radar. This radar creates high temporal resolution (1 s to 2 min), two-dimensional observations measuring the line-of-sight velocities of ionospheric plasma irregularities, which can be regarded as line-of-sight velocities of ionospheric convection in the mid-latitude region from 40° to 50°. This region could not be monitored using preexisting SuperDARN radars. In this study, we used ionospheric echo data obtained by the SuperDARN Hokkaido radar over 5 years (December 2006 to November 2011). We identified westward flows around midnight at about 40° to 55° geomagnetic latitude. Additionally, the data showed that the westward flow around midnight intensified under high geomagnetic activity (high Kp). This suggests that the disturbance dynamo could affect the mid-latitude ionospheric convection. We performed Superposed Epoch Analysis (SEA) to study the influences from the geomagnetic disturbances on mid-latitude ionospheric convection. We found no obvious influence during major storms (minimum Dst below −60 nT). SEA was also used to study the temporal and latitudinal dependence on the influences from substorms. From analysis of 36 events of AL-defined substorms, we saw that the influence of substorms lasted from 5 to 20 h after the onset between 44° and 53° geomagnetic latitude. The westward flow at mid-latitude grew to a maximum at 12 h after the geomagnetic substorm onset. This is consistent with the results of past numerical simulation studies of the disturbance dynamo effects.     

临近空间飞艇内部自然对流换热计算研究

综合考虑太阳辐射、长波辐射、对流换热等热环境因素对临近空间飞艇热特性的影响,建立飞艇热特性的数学模型,编写程序并计算得到蒙皮表面温度分布。以此作为热边界条件,采用Fluent软件模拟其内部自然对流的流动状态和温度分布,对不同季节不同时刻飞艇内部自然对流换热系数进行了计算分析,并对四个自然对流经验公式进行了评价分析。结果表明,Eckert-Jackson和Bayley公式更适用于计算浮空器内部自然对流换热,与数值模拟结果相比,平均绝对误差（MAD）分别为22.6%和24.1%。     

强迫振动下超声速混合层的掺混特性

利用实验研究与数值仿真相结合的方法,对强迫振动下对流马赫数为0.22的超声速混合层的掺混特性进行了分析,采用动量混合、雷诺应力以及标量混合指标对超声速混合层的掺混效率进行评估.研究结果表明:强迫振动对超声速混合层的掺混特性有重要影响.与无振动下相比,强迫振动使混合层的失稳位置提前,卷起的展向涡尺度变大,加快上下两层流动的混合.同时,强迫振动下,动量混合和标量混合更加充分.振动频率为4500Hz时,雷诺应力峰值提高约48%,薄平板后缘下游160mm处,动量厚度增长120%.      

航天器受迫绕飞构型设计与控制

针对航天器在轨服务任务对绕飞技术的要求,研究了航天器受迫绕飞构型设计和控制问题。基于C-W(Clohessy-Wiltshire)方程的解析解,提出了双水滴拼接绕飞构型,并将单脉冲或双脉冲受迫绕飞延展至多脉冲绕飞构型设计;推导了伴随航天器初始状态变量与绕飞构型形状参数的关系,得到了4种构型的解析表达式和脉冲控制策略。通过数值仿真算例验证了设计的4种绕飞构型能够实现伴随航天器的慢速绕飞和快速绕飞,比较了不同绕飞构型的燃料消耗和绕飞距离误差。数值结果表明,双水滴拼接绕飞构型总脉冲最小。研究成果完善了航天器受迫绕飞构型设计与控制的相关理论,为工程应用提供参考。     

飞行器大迎角下俯仰静、动导数的数值计算

 采用一种适用于非定常流动计算的逐次超松弛（SOR）时间推进方法耦合求解非定常Navier-Stokes方程和强迫运动方程,数值模拟了NACA0012翼型、弹道外形(HBS)和有翼导弹等飞行器在不同初始迎角下做强迫俯仰振荡的黏性动态流场,给出动态气动力及力矩系数的时间历程;采用积分法获得飞行器的静导数和动导数,将计算结果与实验结果及半经验理论预测方法进行比较并分析飞行器在大迎角下动态特性的非线性特征;计算结果与实验值相吻合,表明本文采用的非定常数值模拟方法在大迎角下能够较准确地模拟飞行器的动态特性,具有工程应用价值。     

微阵列射流冲击肋化表面传热特性

以去离子水为工质,对微阵列射流冲击光滑和肋化表面的传热特性进行了实验研究,并以光滑表面传热性能为基准,讨论了肋化表面强化因子(ε)变化规律.实验结果表明:①浸没和自由射流的传热系数均受无量纲射流距离(H/d)影响;提高射流Re数和减小无量纲孔间距(S/d)都能够增强换热.②浸没射流ε受H/d影响大,而自由射流ε基本不受H/d影响;两种射流方式的ε都随Re数增大,且渐趋于一个常数.③对流热阻在各种射流情况下均随流量不断下降,但下降趋势逐渐平缓,当流量大到一定时,热阻基本不再降低.      

恒热流斜板自然对流边界层的稳定性研究

对恒热流条件下的斜板自然对流边界层的稳定性进行了分析及数值模拟.研究发现在一定的倾角和Prandtl数范围内,三维波可存在两种不稳定模态,其临界频率分别接近于重力内波和二维T-S(Tol-mien-Schlichting)波的频率.更为特殊的是,在适当条件下该三维波模态可比二维T-S波更不稳定.这一看似违反Squire定理的结果是由于控制方程中的浮力项造成的.数值模拟初步验证了三维波的临界特性.由于稳定性总是同层流至湍流的转捩过程密切相关,计算结果可为高效换热翅片的设计提供理论依据.      

两层液体Bénard-Marangoni对流的界面张力效应

采用PIV技术对两层流体Benard—Marangoni对流进行了实验研究,得到了不同厚度比下的速度场,分析了界面张力在各种对流模式中的作用。和Rayleig—Benard对流的三种临界对流模式相比,由于界面张力对上下层浮力对流的不同作用效果,使得更复杂的临界对流模式在Benard—Marangoni对流体系中出现;在实验中首次观测到三层涡胞结构等现象。     

Dynamics of the convection in the inner magnetosphere by observations of the diffuse aurora,SAR arc and ionospheric drift

The first results of the comparison of subauroral luminosity dynamics in 557,7 and 630,0 nm emission with simultaneous measurements of the ionospheric drift in the F2 region with a digisonde DPS-4 at the Yakutsk meridian (CGMC: 55–60N, 200°E) at Kp = 2–6 are presented. It is shown from the analysis of individual events that during the magnetospheric convection intensification after the turn of the IMF B_z – component to the south the equatorward extension of diffuse aurora takes place. At the same time the westward ionospheric drift velocity increases both in the diffuse aurora region and much equatorward of it due to the occurrence of the northward polarization electric field. We suppose that the generation of polarization field can be associated with the development of the region 2 FAC during the intensification of magnetospheric convection. The comparison of ground-based observations with measurements of the plasma drift aboard the DMSP-F15 satellite has been carried out.