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.     

Interplanetary Physics Research in China:2006—2008

This brief report summarized the latest advances of the interplanetary physics research in China during the period of 2006—2007,made independently by Chinese space physicists and through international collaboration.The report covers all aspects of the interplanetary physics,including theoretical studies,numerical simulation and data analysis.     

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.     

Particle Acceleration Mechanisms

In this paper we review the possible mechanisms for production of non-thermal electrons which are responsible for the observed non-thermal radiation in clusters of galaxies. Our primary focus is on non-thermal Bremsstrahlung and inverse Compton scattering, that produce hard X-ray emission. We first give a brief review of acceleration mechanisms and point out that in most astrophysical situations, and in particular for the intracluster medium, shocks, turbulence and plasma waves play a crucial role. We also outline how the effects of the turbulence can be accounted for. Using a generic model for turbulence and acceleration, we then consider two scenarios for production of non-thermal radiation. The first is motivated by the possibility that hard X-ray emission is due to non-thermal Bremsstrahlung by nonrelativistic particles and attempts to produce non-thermal tails by accelerating the electrons from the background plasma with an initial Maxwellian distribution. For acceleration rates smaller than the Coulomb energy loss rate, the effect of energising the plasma is to primarily heat the plasma with little sign of a distinct non-thermal tail. Such tails are discernible only for acceleration rates comparable or larger than the Coulomb loss rate. However, these tails are accompanied by significant heating and they are present for a short time of <10⁶ years, which is also the time that the tail will be thermalised. A longer period of acceleration at such rates will result in a runaway situation with most particles being accelerated to very high energies. These more exact treatments confirm the difficulty with this model, first pointed out by Petrosian (Astrophys. J. 557:560, 2001). Such non-thermal tails, even if possible, can only explain the hard X-ray but not the radio emission which needs GeV or higher energy electrons. For these and for production of hard X-rays by the inverse Compton model, we need the second scenario where there is injection and subsequent acceleration of relativistic electrons. It is shown that a steady state situation, for example arising from secondary electrons produced from cosmic ray proton scattering by background protons, will most likely lead to flatter than required electron spectra or it requires a short escape time of the electrons from the cluster. An episodic injection of relativistic electrons, presumably from galaxies or AGN, and/or episodic generation of turbulence and shocks by mergers can result in an electron spectrum consistent with observations but for only a short period of less than one billion years.     

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.     

平方阻尼在非线性缓冲系统中的作用

本文讨论平方阻尼(以参数a表征)在图(1)所示的缓冲系统中的作用,结果表明:平方阻尼对于降低相对位移峰值d_m总有良好的效果,但不一定降低加速度峰值a_m。在一定速度冲击V下,系统的平方阻尼有两种最佳值,使a_m最小的a_(am)和使缓冲效率γ最高的a_(cm),而平方阻尼最佳条件依赖于系统的缓冲弹簧的刚度变化类型: (1)线性弹簧情况:a_(am)=a_(cm),最佳条件为系统在首程中均匀减速; (2)渐硬弹簧情况:a_(am)=a_(cm),最佳条件为系统在首程中初始和终末加速度相等即; aV~2=ω_0~2q(dm) (3)渐软弹簧情况:a_(cm)>a_(am)。 本文的基础是所谓“首程显峰”,假定即系统在速度冲击V下的响应峰值d_m和a_m出现在第一行程中。当平方阻尼值不太小,缓冲弹簧刚度特性接近反对称时,该假定成立。     

冲压发动机燃烧引起激波运动过程一维分析

分析了冲压发动机喷油燃烧引起内流道内正激波运动的机理,采用一维激波捕捉方法,建立了燃油喷入对正激波运动位置影响的一维仿真模型。通过仿真发现:喷入燃油并逐步增大燃油-空气当量比时,正激波逐步向上游运动;燃油-空气当量比越大,正激波越接近进气道喉道;当燃油-空气当量比增大到一定程度时,正激波距离进气道喉道最近,但并未越过喉道;进一步增大燃油-空气当量比,正激波开始向下游回退进一步分析发现:冲压发动机流道及燃烧组织匹配设计直接影响到正激波在流道内的运动位置,需要在设计中格外重视。燃油-空气当量比与激波位置的关系分析可为冲压发动机设计提供一定的理论参考。     

用热流探针测量激波速度

激波速度测量是激波管和激波风洞运行状态的一个重要参数,压电传感器或光学方法测速系统成本高,而传统电离探针在激波马赫数较低、波后温度达不到空气电离程度的情况下无法满足实验要求。提出了一种使用同轴热电偶作为测速探针来测激波速度的方法,弥补了电离探针在激波马赫数较低时的不足。介绍了同轴热电偶探针测速原理,并设计了测量激波速度的系统电路。通过信号放大电路锁定激波冲激信号,触发脉冲信号发生电路,实现了一种单通道、多测点的激波风洞测速系统。分别开展以温度与热流为触发信号的风洞实验,结果表明只有使用热流信号才能满足激波测速的时间要求。     

超声速条件下多体干扰与分离试验研究

采用根据国外公开文献设计的类CAV模型,在0．6m×0．6m 跨/超声速风洞中开展了多体干扰与分离网格测力试验研究,初步获得了典型多体飞行器分离过程中的气动特性变化规律。试验结果表明,载荷模型气动特性受分离位置变化影响非常明显。载荷模型沿轴向分离时,气动力（矩）逐步接近自由流中气动力（矩）值,载荷模型法向位置改变会引发其气动力（矩）值发生更为剧烈的变化。引发这种现象的原因有两个：一是尾迹和头激波的发展改变了不同轴向位置处载荷模型的表面流态,从而影响了其气动特性;二是母机模型底部流动具有明显的非对称膨胀特征,不同法向位置处流速大小和方向差异明显,导致载荷模型气动特性随法向位置变化更为剧烈。     

冲击射流的彩虹纹影实验研究

超声速冲击射流在短距、垂直起降飞行器（S/VTOL）以及火箭发射等方面应用广泛,但是伴随着流场与噪声等诸多方面的问题。要研究这一类问题,必先研究这一类超声速流动的波系结构。文章利用彩虹纹影测量系统,对不同距离不同压比的冲击射流进行实验研究,得到了清晰的彩虹纹影实验结果,细致地呈现了冲击射流的波系结构。基于实验结果,对三种不同结构的冲击射流的波系结构进行了详细分析。发现喷嘴与挡板距离较大时,形成的射流结构与自由射流相似,壁面附近的射流区域不明显。随着距离减小,冲击射流出现壁面冲击区附近射流比较剧烈的现象。距离进一步减小时,出现滞止泡等结构,滞止泡的形状与压比相关。此外,实验表明冲击射流形成的马赫盘大小、形状与来流压比相关。