激光引致水诱导空气击穿所获无约束流场演化过程的实验研究

流场演化过程是揭示激光推进机理的重要研究内容之一。利用纹影系统和PCO-HSFC 高速相机,首次拍摄了自来水诱导CO₂激光击穿空气产生的激波向空气和水中的演化过程。阐述了产生两次气蚀空穴的原因：初始时刻产生的空穴为激波作用于水面所致,第二次空穴出现在相机被触发后约8 μs 时,是激光烧蚀水蒸气作用于水面所形成的低压区。实验结果表明：击穿后流场向激光入射方向（空气中）演化较快,激波初速度较大,约为6 km/s;流场向水中演化相对较缓,激波初速度约为3.33 km/s。两者都服从指数衰减,分别在约73.368 μs 和41.649 μs 时衰减到声速。研究结果对于把水作为工质应用于激光推进有一定意义。     

Polarization pattern of low and mid-frequency magnetic pulsations in the polar cap: A comprehensive analysis at Terra Nova Bay (Antarctica)

The polarization pattern of ULF pulsations (f ≈ 1–100 mHz) at Terra Nova Bay (Antarctica, CGM λ ∼ 80°) has been determined for the entire 2003, soon after the solar maximum. A comparison with the results of previous investigations, conducted at the same station close to the solar minimum (1994–96), allows to focus common elements and major differences among different frequency bands which persist through the entire solar cycle. Basically, between f ∼ 1.5 and 5 mHz, the day can be divided into four sectors with alternate polarizations. The local time and latitudinal dependence of the observed pattern can be tentatively interpreted in terms of a latitude of resonant field lines reaching λ ∼ 80° in the noon sector; on the other hand, resonance effects of lower latitude field lines can be clearly identified also far from the noon meridian when the station moves into the deep polar cap. Moreover, in the morning sector the resonance region would extend to lower latitudes than in the evening sector. The proposed profile of the resonant region can interpret also the results obtained at other cusp/auroral stations and appears consistent with that one inferred in the northern hemisphere at smaller latitudes. The resonance region progressively shifts toward lower latitude with increasing frequency; correspondingly, the four-sector pattern progressively disappears at TNB. Above f ∼ 20 mHz, the experimental observations might suggest an additional contribution from Sunward propagating waves, possibly via the magnetotail lobes.     

Ionospheric oscillations caused by geomagnetic Pi2 pulsations and their observations by multipoint continuous Doppler sounding; first results

In 2004, we started operating a continuous Doppler sounding system to investigate ionospheric signatures of infrasonic, short period acoustic gravity waves and geomagnetic pulsations. Since January 2007, four stable 3.59 MHz transmitters have been in operation in the western part of the Czech Republic. Multipoint measurements enable us to investigate horizontal propagation of waves and disturbances in the ionosphere and to estimate horizontal distances over which these waves (disturbances) are correlated.     

一种新的用于MHD方程逆风格式的Jacobian矩阵分裂方法

针对理想MHD方程,提出了一种新的基于MacCormack算法的雅可比矩阵分裂方法,克服了原有方法稳定性差的问题,并成功地应用于理想MHD方程的求解.控制方程在非结构混合网格上进行空间离散,其中对流项采用本文发展的逆风向量分裂格式,并引入了双曲型磁场散度清除技术,时间推进为显式5步龙格-库塔方法.对MHD激波管流动和带均匀磁场干扰的二维高超声速钝头体绕流流场进行了数值模拟,得到了与参考文献相吻合的数值结果,表明本文发展的数值分裂方法可以有效地捕捉MHD流场的流动特征,并且具有比MacCormack方法更高的稳定性和计算精度.     

The Expansion of Coronal Plumes in the Fast Solar Wind

Coronal plumes are believed to be essentially magnetic features: they are rooted in magnetic flux concentrations at the photosphere and are observed to extend nearly radially above coronal holes out to at least 15 solar radii, probably tracing the open field lines. The formation of plumes itself seems to be due to the presence of reconnecting magnetic field lines and this is probably the cause of the observed extremely low values of the Ne/Mg abundance ratio. In the inner corona, where the magnetic force is dominant, steady MHD models of coronal plumes deal essentially with quasi-potential magnetic fields but further out, where the gas pressure starts to be important, total pressure balance across the boundary of these dense structures must be considered. In this paper, the expansion of plumes into the fast polar wind is studied by using a thin flux tube model with two interacting components, plume and interplume. Preliminary results are compared with both remote sensing and solar wind in situ observations and the possible connection between coronal plumes with pressure-balance structures (PBS) and microstreams is discussed. This revised version was published online in June 2006 with corrections to the Cover Date.     

顶部间隙对超声速膨胀器流动特性的影响

隔板与机匣之间留有间隙,间隙的存在势必会对超声速膨胀器的内部流场和总体性能产生影响,为了获得超声速膨胀器内部间隙流动的流动细节,采用三维雷诺平均Navier-Stokes方程和标准k-ε湍流模型,就顶部间隙对超声速膨胀器流动特性的影响进行了数值研究。结果表明:膨胀流道出口斜激波导致吸力面压力高于压力面,隔板尾缘附近部分泄漏流体经间隙流回压力面侧;间隙的存在导致吸力面进口及中、后部近下端壁压力上升,而压力面前缘附近压力下降,对比同一隔板位置,间隙高度每增加1%喉部高度,超声速膨胀器隔板载荷系数最高下降2.6%;端壁损失和斜激波损失降低,但产生了泄漏损失,三维流道内总的流动损失增加,膨胀器效率降低,本文研究范围内效率最多下降8.8%;马蹄涡、泄漏涡及二者之间的相互作用是顶部区域的主要涡系结构;前缘附近气流经间隙流到吸力面侧和尾缘附近泄漏流体越过间隙重新流回压力面侧是间隙内气流的主要运动形式。     

近壁区Reynolds应力输运方程的理论模型

在湍流边界层的近壁区,采用对称共振三波的理论模型描述相干结构,根据理论模型对Reynolds应力输运方程逐项进行计算和分析,结果与直接数值模拟符合很好.这不仅在理论上有益于对湍流物理机制的了解,而且展现了一种可能性,即根据相干结构的理论知识来改造湍流模型,使之具有更清晰的物理内涵以提高近壁区的预估精度.     

两冕流间CME事件数值模拟的改进

通过偶极子场和六极子场适当叠加，改进猜解磁场，使猜解磁场在太阳南北极符号相反，然后采用理想磁流体力学方程组(MHD)，由猜解磁场与太阳风流动相互作用计算出稳态自洽解，得到定性上与观测比较接近的具有两个冕流的背景结构．在两个冕流间采用具有同心圆磁场位形的触发模型触发CME事件，研究CME的日冕传播特征．模拟结果表明，CME被约束在两冕流间传播，CME闭磁场位形和磁云横截面磁场位形相似，可以解释1AU处观测磁云的部分特征；在CME附近，存在压力和Lorentz力起主要作用的区域，这可以为分析1AU处CME事件的观测数据提供帮助．     

乘波构型飞行器磁流体进气道一体化概念设计

采用准一维的磁流体方程组对设计状态下内磁流体发生器进行参数设计,利用斜激波理论设计磁流体进气道一体化的外形.以该外形为基点,对安装五对电极的内磁流体发生器采用五方程模型进行三维数值模拟,并通过调节其磁作用数以满足准一维假设下设计的进气道外形.研究表明,磁流体进气道最小出口流动均匀参数可以作为判别内发生器最优磁作用数的准则,在该磁作用数下内磁流体发生器可以有效地提高进气道的性能.