Propagation and interaction of interplanetary transient disturbances. Numerical simulations

We study the heliocentric evolution of ICME-like disturbances and their associated transient forward shocks (TFSs) propagating in the interplanetary (IP) medium comparing the solutions of a hydrodynamic (HD) and magnetohydrodynamic (MHD) models using the ZEUS-3D code [Stone, J.M., Norman, M.L., 1992. Zeus-2d: a radiation magnetohydrodynamics code for astrophysical flows in two space dimensions. i – the hydrodynamic algorithms and tests. Astrophysical Journal Supplement Series 80, 753–790]. The simulations show that when a fast ICME and its associated IP shock propagate in the inner heliosphere they have an initial phase of about quasi-constant propagation speed (small deceleration) followed, after a critical distance (deflection point), by an exponential deceleration. By combining white light coronograph and interplanetary scintillation (IPS) measurements of ICMEs propagating within 1 AU [Manoharan, P.K., 2005. Evolution of coronal mass ejections in the inner heliosphere: a study using white-light and scintillation images. Solar Physics 235 (1–2), 345–368], such a critical distance and deceleration has already been inferred observationally. In addition, we also address the interaction between two ICME-like disturbances: a fast ICME 2 overtaking a previously launched slower ICME 1. After interaction, the leading ICME 1 accelerates and the tracking ICME 2 decelerates and both ICMEs tend to arrive at 1 AU having similar speeds. The 2-D HD and MHD models show similar qualitative results for the evolution and interaction of these disturbances in the IP medium.     

The evolution of mirror type magnetic fluctuations in the magnetosheath based on multipoint observations

Two orbits were selected in January–February 2006 when the separation between the Cluster spacecraft was large and mirror type magnetic field fluctuations were observed by all spacecraft in different regions of the terrestrial magnetosheath. Minimum variance analysis was applied to find the mirror type fluctuations, and the amplitude of the fluctuations was determined individually. Mirror mode structures are moving along the streamlines frozen in the plasma. A model was developed for the calculation of plasma flowtime from the bow shock to the observation point. The growth rate of the field strength perturbations was estimated by comparing the amplitudes of fluctuations observed simultaneously at distant locations (∼10,000 km) based on the assumption that δB ∼ exp(γt). The obtained growth rate values were about an order of magnitude smaller than those provided by linear models and they decreased in the inner regions of the magnetosheath, indicating some saturation in the growth of the waves when proceeding towards the magnetopause. The results of these two case studies suggest that mirror type fluctuations originate from the compression region downstream of the quasi-perpendicular bow shock, and the growth of the fluctuations cannot be described by linear approximations.     

Alfvénic Electron Acceleration in Aurora Occurs in Global Alfvén Resonosphere Region

Auroral emission caused by electron precipitation (Hardy et al., 1987, J. Geophys. Res. 92, 12275–12294) is powered by magnetospheric driving processes. It is not yet fully understood how the energy transfer mechanisms are responsible for the electron precipitation. It has been proposed (Hasegawa, 1976, J. Geophys. Res. 81, 5083–5090) that Alfvén waves coming from the magnetosphere play some role in powering the aurora (Wygant et al., 2000, J. Geophys. Res. 105, 18675–18692, Keiling et al., 2003, Science 299, 383–386). Alfvén-wave-induced electron acceleration is shown to be confined in a rather narrow radial distance range of 4–5 R _E (Earth radii) and its importance, relative to other electron acceleration mechanisms, depends strongly on the magnetic disturbance level so that it represents 10% of all electron precipitation power during quiet conditions and increased to 40% during disturbed conditions. Our observations suggest that an electron Landau resonance mechanism operating in the “Alfvén resonosphere” is responsible for the energy transfer.     

喷嘴位置对脉冲爆轰发动机性能影响的试验研究

为了研究喷嘴位置对脉冲爆轰发动机性能的影响,设计加工了直径为80mm的汽油/空气两相脉冲爆轰发动机（PDE）,在PDE文氏管内不同位置安装喷嘴,进行了冷态雾化和热态燃烧转爆轰试验,分析了马尔文激光粒度仪测得的液滴尺寸分布和动态压力传感器测得的信号。试验结果表明：喷嘴的安装位置对脉冲爆轰发动机的性能具有显著影响;喷嘴安装在文氏管喉部时爆轰管内雾化混合效果最好,爆轰波峰值压力最大为3．5 MPa,工作频率最高为30Hz;喷嘴安装在文氏管入口时爆轰管内雾化混合效果最差,爆轰波峰值压力最小为0．9MPa,工作频率最低为15 Hz;在试验范围内,改善雾化混合效果有利于提高脉冲爆轰发动机的工作频率。研究结果对脉冲爆轰发动机的设计具有参考价值。     

激波聚焦诱导气液两相爆震燃烧的数值模拟

对以激波聚焦和增加障碍物方式诱导煤油-空气气液两相爆震燃烧的过程进行了数值模拟.采用欧拉-拉格朗日方法建立了脉冲爆震发动机(PDE)中气液两相流的喷射、雾化、掺混过程.研究发现环形爆震波在爆震管凹腔内经过反射、汇聚后能够引燃可燃混合物.而在障碍物处,激波的反射和再反射聚焦能够形成高温高压点(2700K,25MPa),产生局部爆炸,有助于形成稳定的脉冲爆震燃烧(波面速度为1900m/s,温度为2 950K),有效地缩短由缓燃向爆震转变(DDT)距离至0.45m.     

几种常用格式和湍流模型在高速流动中的适用性研究

针对高超声速飞行器中存在的强激波、激波/边界层干扰、分离、湍流等复杂流动现象,对比分析了当前计算流体力学中的主要空间离散格式及湍流模型,发现不同格式对强激波的分辨率基本相同,Roe和LDE(low diffusion E-CUSP(convective upwind split pressure))格式对摩擦因数和传热系数的模拟优于其他格式;S-A(Spalart-Allmaras)一方程湍流模型计算的摩擦因数比k-ωSST(shear stress transport)两方程湍流模型高10%左右,而后者预测的分离区约为前者的2倍,且分离点靠前.     

航空发动机盘件径轴向裂纹底波监控超声检测方法研究

针对某航空发动机盘件中的径轴向裂纹,采用不同焦距的5MHz、10MHz聚焦探头和平探头,分别在0°,1°,2°,3°的声束入射角度下进行检测试验,通过对入射角度以及探头类型、频率、焦距等参数的优化,建立了径轴向裂纹的底波监控超声检测方法。研究发现:与垂直入射相比,小角度纵波斜入射底波监控超声检测方法可提高超声波对裂纹的敏感程度;使用焦距为89mm的10MHz聚焦探头,并使声束以2°入射角斜入射可得到最佳检测效果,试验结果与数值模拟具有良好的一致性。     

温度对液体中超声速度的影响

本文导出了超声波速度同液体压缩系数及密度关系，研究了压缩系数及密度与温度的关系，进而研究了温度对声速及声时的影响，用实验测量了不同的液体成份下的声时同温度的关系，从而提出了进行液体成份分析所必需的参量，对用超声波分析液体成份提供了理论依据，对提高产品质量及实现工业在线检测有一定的实用价值。     

Propagation of non-linear ion-sound pulses in dusty plasma waveguides

There are a lot of objects in space associated with dusty plasma inclusions. Such inclusions may bear a prolonged shape and behave as waveguides for ion-sound waves. In the case of space plasmas, the dust particles can possess both negative charge, due to electron attachment, and positive one, due to photoionization. In this paper the propagation of linear and non-linear ion-sound wave pulses in the dusty plasma waveguides, possessing positive charge, is studied. It has been demonstrated that non-linear dynamics of baseband pulse propagation in plasma waveguide possesses essentially non-solitonic behavior. Namely, propagation of a long ion-sound pulse leads to an excitation of a shock-like wave but not a stable localized nonlinear pulse. Also, when a Korteveg–de Vries (KdV) soliton is incident onto the dusty plasma waveguide, some part of the soliton energy is captured by the waveguide and transformed into a multi-pulse structure. Additionally, an interaction of dusty plasma inclusions with KdV soliton can lead to the occurrence of transverse instabilities of the soliton and its eventual destruction.     

Height and time variability of planetary wave activity

The height–season and year-to-year regularities of parameters of first and second spatial harmonics determine the structure of the stratosphere and mesosphere circulation and its variability. In the period 1992–2002 at heights 0–55 km, the amplitudes and phases of the first and second spatial harmonics in the field of temperature, geopotential height, zonal and meridional wind were calculated by the method of harmonic decomposition. Dispersion (standard or mean square deviation) of their day-to-day and year-to-year variations was calculated by their wavelength constants. Height and season patterns of variability have been estimated. The difference in height–longitude variability for wave numbers m = 1 and 2 has been discovered. At the same time, the intensity of wave disturbances for m = 1 is less than for m = 2 excluding the polar areas, where a significant variability appears at the heights 0–55 km. There is also a tendency for the intensity of year-to-year variations to decrease in comparison with day-to-day variations. In cold and warm periods the amplitude of perturbation waves with m = 2 both for day-to-day and year-to-year variations is greater than for waves with m = 1. Transient height areas in the interval of 20–30 km are more distinct for day-to-day variations of polar area.