EIT Waves: A Changing Understanding over a Solar Cycle

We present here a review of observations and the current theories that attempt to explain coronal EIT waves. EIT waves were first observed by SOHO-EIT in 1996. Since then, careful analysis has shown that they are related to various other phenomena, such as: CMEs, coronal dimming regions, Moreton waves, and transverse coronal loop oscillations. Over the years, myriad theories have been proposed to explain EIT waves. Early attempts, while elegant, relied heavily on theories based on pre-coronal observations. More recent work, which tends to consider a larger data pool, has led to two competing theoretical camps: wave vs. non-wave models; in many cases, proposed hypotheses flatly contradict each other. Sifting through these seemingly-incongruous models requires a thorough understanding of the available data, as some observations make certain theories more difficult to justify. However, some questions still do not appear resolvable with current data and will likely require help from the next generation of coronal telescopes.     

Coronal Observations of CMEs

CMEs have been observed for over 30 years with a wide variety of instruments. It is now possible to derive detailed and quantitative information on CME morphology, velocity, acceleration and mass. Flares associated with CMEs are observed in X-rays, and several different radio signatures are also seen. Optical and UV spectra of CMEs both on the disk and at the limb provide velocities along the line of sight and diagnostics for temperature, density and composition. From the vast quantity of data we attempt to synthesize the current state of knowledge of the properties of CMEs, along with some specific observed characteristics that illuminate the physical processes occurring during CME eruption. These include the common three-part structures of CMEs, which is generally attributed to compressed material at the leading edge, a low-density magnetic bubble and dense prominence gas. Signatures of shock waves are seen, but the location of these shocks relative to the other structures and the occurrence rate at the heights where Solar Energetic Particles are produced remains controversial. The relationships among CMEs, Moreton waves, EIT waves, and EUV dimming are also cloudy. The close connection between CMEs and flares suggests that magnetic reconnection plays an important role in CME eruption and evolution. We discuss the evidence for reconnection in current sheets from white-light, X-ray, radio and UV observations. Finally, we summarize the requirements for future instrumentation that might answer the outstanding questions and the opportunities that new space-based and ground-based observatories will provide in the future.     

Global Properties of Solar Flares

This article broadly reviews our knowledge of solar flares. There is a particular focus on their global properties, as opposed to the microphysics such as that needed for magnetic reconnection or particle acceleration as such. Indeed solar flares will always remain in the domain of remote sensing, so we cannot observe the microscales directly and must understand the basic physics entirely via the global properties plus theoretical inference. The global observables include the general energetics—radiation in flares and mass loss in coronal mass ejections (CMEs)—and the formation of different kinds of ejection and global wave disturbance: the type II radio-burst exciter, the Moreton wave, the EIT “wave”, and the “sunquake” acoustic waves in the solar interior. Flare radiation and CME kinetic energy can have comparable magnitudes, of order 10³² erg each for an X-class event, with the bulk of the radiant energy in the visible-UV continuum. We argue that the impulsive phase of the flare dominates the energetics of all of these manifestations, and also point out that energy and momentum in this phase largely reside in the electromagnetic field, not in the observable plasma.     

Multi-Wavelength Observations of CMEs and Associated Phenomena

This chapter reviews how our knowledge of CMEs and CME-associated phenomena has been improved, since the launch of the SOHO mission, thanks to multi-wavelength analysis. The combination of data obtained from space-based experiments and ground based instruments allows us to follow the space-time development of an event from the bottom of the corona to large distances in the interplanetary medium. Since CMEs originate in the low solar corona, understanding the physical processes that generate them is strongly dependant on coordinated multi-wavelength observations. CMEs display a large diversity in morphology and kinematic properties, but there is presently no statistical evidence that those properties may serve to group them into different classes. When a CME takes place, the coronal magnetic field undergoes restructuring. Much of the current research is focused on understanding how the corona sustains the stresses that allow the magnetic energy to build up and how, later on, this magnetic energy is released during eruptive flares and CMEs. Multi-wavelength observations have confirmed that reconnection plays a key role during the development of CMEs. Frequently, CMEs display a rather simple shape, exhibiting a well known three-part structure (bright leading edge, dark cavity and bright knot). These types of events have led to the proposal of the ‘`standard model’' of the development of a CME, a model which predicts the formation of current sheets. A few recent coronal observations provide some evidence for such sheets. Other more complex events correspond to multiple eruptions taking place on a time scale much shorter than the cadence of coronagraph instruments. They are often associated with large-scale dimming and coronal waves. The exact nature of these waves and the physical link between these different manifestations are not yet elucidated. We also discuss what kind of shocks are produced during a flare or a CME. Several questions remain unanswered. What is the nature of the shocks in the corona (blast-wave or piston-driven?) How they are related to Moreton waves seen in Hα? How they are related to interplanetary shocks? The last section discusses the origin of energetic electrons detected in the corona and in the interplanetary medium. “Complex type III-like events,”which are detected at hectometric wavelengths, high in the corona, and are associated with CMEs, appear to originate from electrons that have been accelerated lower in the corona and not at the bow shock of CMEs. Similarly, impulsive energetic electrons observed in the interplanetary medium are not the exclusive result of electron acceleration at the bow shocks of CMEs; rather they have a coronal origin.     

S/WAVES: The Radio and Plasma Wave Investigation on the STEREO Mission

This paper introduces and describes the radio and plasma wave investigation on the STEREO Mission: STEREO/WAVES or S/WAVES. The S/WAVES instrument includes a suite of state-of-the-art experiments that provide comprehensive measurements of the three components of the fluctuating electric field from a fraction of a hertz up to 16 MHz, plus a single frequency channel near 30 MHz. The instrument has a direction finding or goniopolarimetry capability to perform 3D localization and tracking of radio emissions associated with streams of energetic electrons and shock waves associated with Coronal Mass Ejections (CMEs). The scientific objectives include: (i) remote observation and measurement of radio waves excited by energetic particles throughout the 3D heliosphere that are associated with the CMEs and with solar flare phenomena, and (ii) in-situ measurement of the properties of CMEs and interplanetary shocks, such as their electron density and temperature and the associated plasma waves near 1 Astronomical Unit (AU). Two companion papers provide details on specific aspects of the S/WAVES instrument, namely the electric antenna system (Bale et al., Space Sci. Rev., 2007) and the direction finding technique (Cecconi et al., Space Sci. Rev., 2007).     

A Comparison of Ground Level Event e/p and Fe/O Ratios with Associated Solar Flare and CME Characteristics

Solar energetic particle (SEP) events reaching rigidities >1 GV are observed at 1?AU as ground-level events (GLEs). They are considered to be extreme cases of gradual SEP events, produced by shocks driven by wide and fast CMEs that are usually associated with long-duration (>1 hour) soft X-ray (SXR) flares. However, some large gradual SEP events, including GLEs, are associated with flares of short-duration (<1 hour) timescales comparable to those of flares seen with impulsive, low-energy SEP events with enhanced charge states, heavy-element abundances, and e/p ratios. The association of some GLEs with short-duration SXR events challenges us to understand the GLE event-to-event variation with SXR durations and whether it truly reflects the nature of the particle acceleration processes or simply the characteristics of the solar regions from which large, fast CMEs arise. We examine statistically the associated flare, active region (AR), and CME characteristics of ～40?GLEs observed since 1976 to determine how the GLE e/p and Fe/O ratios, each measured in two energy ranges, depend on those characteristics. The abundance ratios trend weakly to lower, more coronal, and less scattered values with increasing flare timescales, thermal and nonthermal peak fluxes, and measures of source AR sizes. These results and the wide range of solar longitude connections for GLEs with high abundance ratios argue against a significant role for flare effects in the GLEs. We suggest that GLE SEPs are accelerated predominately in CME-driven shocks and that a coupling of flare size and timescales with CME properties could explain the SEP abundance correlations with flare properties.     

Modelling of Solar Wind, CME Initiation and CME Propagation

Simulations of coronal mass ejections (CMEs) evolving in the interplanetary (IP) space from the Sun up to 1 AU are performed in the framework of ideal magnetohydrodynamics (MHD) by the means of a finite-volume, explicit solver. The aim is to quantify the effect of the background solar wind and of the CME initiation parameters, such as the initial magnetic polarity, on the evolution and on the geo-effectiveness of CMEs. First, three different solar wind models are reconstructed using the same numerical grid and the same numerical scheme. Then, different CME initiation models are considered: Magnetic foot point shearing and magnetic flux emergence. For the fast CME evolution studies, a very simple CME model is considered: A high-density and high-pressure magnetized plasma blob is superposed on a background steady state solar wind model with an initial velocity and launch direction. The simulations show that the initial magnetic polarity substantially affects the IP evolution of the CMEs influencing the propagation velocity, the shape, the trajectory (and thus, the geo-effectiveness).     

楔形体入波浪水面数值模拟

数值模拟分析楔形体入波浪水面流体力学现象和运动姿态变化历程，为水上飞机在波浪水面起降提供技术和理论支持。基于有限体积法求解非定常雷诺平均Navier-Stokes（URANS）方程和SST k-ω湍流模型，结合整体动网格法的速度入口造波方法、阻尼消波法和流体体积（VOF）液面捕捉技术构造数值波浪水池，耦合三/六自由度模型，实现楔形体入线性规则波和不规则波的数值模拟。在楔形体入静水面算例验证的基础上，详细研究二维楔形体在线性规则波波峰、波谷、平衡位置-上行速度和下行速度处入水过程的受力特性和运动姿态变化。结果表明：速度入口造波方法的波浪数值解与理论解析解较吻合，偏差为1%；在二维楔形体入规则波过程中，楔形体所受垂向力和垂向速度变化趋势相同，对横向位移影响较小，其数值变化少于0.01；在平衡位置入水过程中，模型的滚转角和横向速度变化明显，其数值变化约为波峰、波谷位置处的8倍和10倍。分析原因：平衡位置处波浪内流速度变化较快，模型所受波浪力冲量较大，且楔形体两侧斜边与波浪的相互作用力也参与到模型的运动中。数值模拟二维楔形体在线性不规则波5个随机时间点入水及三维楔形体在波峰、平衡位置-上行速度处入水过程，其变化规律及形成原因与入规则波相似。     

Large-scale Bright Fronts in the Solar Corona: A?Review of?��EIT waves��

??EIT waves?? are large-scale coronal bright fronts (CBFs) that were first observed in 195 Å images obtained using the Extreme-ultraviolet Imaging Telescope (EIT) onboard the Solar and Heliospheric Observatory (SOHO). Commonly called ??EIT waves??, CBFs typically appear as diffuse fronts that propagate pseudo-radially across the solar disk at velocities of 100?C700 km?s^?1 with front widths of 50?C100 Mm. As their speed is greater than the quiet coronal sound speed (c _s ??200 km?s^?1) and comparable to the local Alfvén speed (v _A ??1000 km?s^?1), they were initially interpreted as fast-mode magnetoacoustic waves ( $v_{f}=(c_{s}^{2} + v_{A}^{2})^{1/2}$ ). Their propagation is now known to be modified by regions where the magnetosonic sound speed varies, such as active regions and coronal holes, but there is also evidence for stationary CBFs at coronal hole boundaries. The latter has led to the suggestion that they may be a manifestation of a processes such as Joule heating or magnetic reconnection, rather than a wave-related phenomena. While the general morphological and kinematic properties of CBFs and their association with coronal mass ejections have now been well described, there are many questions regarding their excitation and propagation. In particular, the theoretical interpretation of these enigmatic events as magnetohydrodynamic waves or due to changes in magnetic topology remains the topic of much debate.     

Influence of shock wave impinging region on supersonic film cooling

Shock waves can significantly affect the film cooling for supersonic flow and shock waves may have different influence when impinging in different regions. The present study numerically compared the results of shock wave impinging in three different regions and analyzed the effect of impinging region. The shock wave generators were located at x/s = 5, 25, 45 with 4°, 7° and 10° shock wave incidence. The mainstream Mach number was 3.2 and the coolant Mach number was 1.2 or 1.5. The numerical results illustrated that the shock wave impinged in the further upstream region led to a larger high-pressure region and a larger vortex in the boundary layer. Moreover, placing the shock wave generator upstream resulted in the lower mass fraction of coolant in the downstream region. The velocity in the upstream part of the cooling layer was lower than the midstream and downstream part, which resulted in the less ability to resist the shock wave impingement. Therefore, the upstream impingement deteriorated the cooling performance to a greater extent. The study also manifested that the stronger shock wave had a larger effect on supersonic film cooling. Increasing the coolant inlet Mach number can increase the blowing ratio and reduce the mixing, which was of benefit to improve cooling effect.     

局部抽吸对边界层流动稳定性的影响和控制研究

在边界层壁面上,设计局部抽吸结构,采用直接数值模拟的方法,获得稳定的三维基本流.在此基础上,研究稳定及最不稳定的二维扰动T-S波的时、空演化机制;进一步探讨了局部抽吸的形式、强度大小及分布结构对二维T-S波的非线性演化影响及其对增长率的贡献大小.结果表明,局部抽吸结构诱导产生的三维基本流是扰动波得以快速增长的一个关键性因素,这是由于平均流剖面的改变及展向速度的出现,增强了流体运动中的不稳定性、扩大了中性曲线的不稳定区域范围.在最不稳定的二维扰动T-S波的非线性演化过程中,由于非线性作用的不断增强,逐渐激发产生出三维扰动波及高次谐波,其三维扰动波的流向波数和频率与二维扰动波的流向波数和频率相同;同时展向速度的大小对二维扰动波的增长、流动的失稳、流向涡的形成等方面都起着激励的作用.随着时、空的不断发展和非线性作用的迅速加强,正、负相间的流向涡逐渐形成,强度逐渐增大,流向涡的影响区域也在不断扩大,涡的形状逐渐拉伸变长,并出现强的剪切层,流动开始失稳等其它机制;这些结论与文献[4、5]的结果相吻合.     

流动稳定性中小扰动波传播速度的数值研究

在保守系统中，小扰动波如线性水波及线性重力内波等均以其群速度传播，且群速度等于能流速度，在非保守系统中，波的传播速度还是个不十分清楚的问题。本文用数值计算的方法研究流动稳定性问题中小扰动波的传播速度，结果表明，波的传播速度并不等于能流速度，而与复群速度的实部近似相等。本文还用一简单的模型对此给予了解释。     

Love Waves in Layered Graded Composite Structures with Imperfectly Bonded Interface

Theoretical analysis and numerical calculations of Love wave propagation in layered graded composites with imperfectly bonded interface are described in this paper. On the basis of WKB method, the approximate analytic solutions for Love waves are obtained. By the interface shear spring model, the dispersion relations for Love waves in layered graded composite structures with rigid, slip, and imperfectly bonded interfaces are given, and the effects of the interface conditions on the phase velocities of Love waves in SiC/Al lay- ered graded composites are discussed. Numerical analysis shows that the phase velocity decreases when the defined flexibility parameter is greater. For the general imperfectly bonded interface, the phase velocity changes in the range of the velocities for the rigid and slip interface conditions.     

超声速膨胀角入射激波/湍流边界层干扰直接数值模拟

为了揭示膨胀效应对激波/湍流边界层干扰区内复杂流动现象的影响规律,采用直接数值模拟方法对来流马赫数2.9、30°激波角的入射激波与10°膨胀角湍流边界层相互作用问题进行了数值研究。系统地探讨了激波入射点分别位于膨胀角上游、膨胀角角点和膨胀角下游3种工况下膨胀角干扰区内若干基本流动现象,如分离泡、物面压力脉动及激波非定常运动、湍流边界层统计特性和相干结构动力学过程等。结果表明,激波入射点流向位置改变对分离区流向和法向尺度的影响显著,尤其是当激波入射点位于角点及其下游区域。研究发现,膨胀角干扰区内物面压力脉动强度急剧减小,分离区内压力波向下游传播速度将降低而在膨胀区内将升高,膨胀效应极大地抑制了分离激波的低频振荡运动。相较于入射激波与平板湍流边界层干扰,入射激波流向位置改变对膨胀角再附区速度剖面对数区及尾迹区影响显著,将导致其内层结构参数升高而外层降低,近壁区内将呈现远离一组元湍流状态的趋势。此外,流向速度脉动场本征正交分解分析指出,主模态空间结构集中在分离激波及剪切层根部附近而高阶模态以边界层内小尺度正负交替脉动结构为主。低阶重构流场结果表明,前者对应为分离泡低频膨胀/收缩过程而后者表征为分离泡高频脉动。     

爆震波点火器管路传播过程数值模拟

为了进一步研究液体火箭发动机爆震波点火器的工作过程，结合实际试验发动机用爆震波点火器的工作条件，在混合比为3，初始氢氧混气压力为0．1MPa情况下，采用常用的两步显式MacCormak差分格式和有限速率化学反应动力模型，对爆震波点火器管路中爆震波的传播过程进行了数值模拟，研究了爆震波形成后在一维管路中传播特性及性能参数。从数值模拟结果来看，稳定传播的爆震波温度可达3500K，压力达到2MPa，其传播速度可达3430m／s，从爆震波形成到其传播到2m距离的出口，用时不到0．6ms。并与试验结果进行了对比分析，数值模拟结果和试验结果符合很好，为爆震波点火器的工程设计提供了理论依据。     

In situ Wave Phenomena Associated with Magnetic Clouds and Other Ejecta

We present Ulysses Unified Radio and Plasma Wave (URAP) observations of ion-acoustic waves associated with magnetic clouds and ejecta. The peak intensities of these waves, which usually occur inside CMEs when T _e/T _i≫1, are not correlated with heliocentric distance or electron to ion temperature ratio inside the CMEs. This revised version was published online in August 2006 with corrections to the Cover Date.     

二维平板水漂运动数值模拟

探索平板水漂运动的流体力学现象机理对飞行器着水问题的研究有重要的参考价值。基于有限体积法和k-ε RNG湍流模型求解非定常雷诺平均Navier-Stokes（URANS）方程,采用流体体积分数（VOF）模型与速度入口造波法构造数值波浪水池,并结合整体动网格方法,完成二维平板在静水面与波浪水面的水漂运动数值模拟。在与试验值和理论值对比的基础上,讨论初始姿态角、投掷角度与投掷速度对水漂运动的影响。进一步研究不同波浪参数和波浪位置对平板水漂的影响,并从能量角度展开分析。结果表明：20°姿态角平板能以最小的投掷速度实现水漂运动;运动中平板能量的相对损失率受初始投掷速度的影响较小,主要受投掷角和姿态角作用,随投掷角或姿态角的增加而增大。波浪情况下,在上行波位置触水的平板能够获得更大的接触面积,而更长的触水时间发生在波谷处;因此,这两个位置触水的平板在水漂运动过程中的相对能量损失大,其数值变化比波峰位置大5%左右;在上行波位置触水时,平板的速度衰减与相对能量损失随着波高的增加而增大,而波峰位置则有相反的变化趋势。     

激波边界层的相互作用对扰动波传播的影响

利用线性稳定性理论和直接数值模拟研究了带有入射斜激波的、来流马赫数Ma=4．5条件下的平板边界层的失稳特性。重点考察了在由于激波边界层相互干扰，平板边界层上形成分离区，又进而产生激波、膨胀波和旋涡等复杂流动现象的流场上游，引入小扰动的TS波后，扰动波传播通过带有这些复杂流动现象的流场时，扰动波的发展变化特点。通过对流场中扰动波（包括基本波和衍生波）演化特征的分析，研究分离和激波等复杂流动现象对平板边界层稳定性的影响特点。数值模拟发现，激波的出现不同于一般的压缩波，在亚声速区与超声速区对扰动波演化的影响是不同的，此外，分离对扰动有稳定作用。     

Relationship of coronal transients to interplanetary shocks: 3D aspects

More than 1000 coronal mass ejections (CMEs) caused by different types of coronal transients have been analyzed up to now, based on the images from white light coronagraphs on board the OSO 7, Skylab, P78-1, and SMM spacecraft. In many cases, the CME images lead us to the impression of loop-like, more planar structures, similar to those of prominence structures often seen in H pictures. There is increasing evidence, though, for a three-dimensional bubble- or cloud-like structure of CMEs. In several cases, CMEs directed toward the earth (or away from it) were identified, as their outer fronts emerged on all sides of the coronagraph's occulting disk, thus suggesting a bubble-like appearance.There now appears to be unanimity about the crucial role that magnetic reconnection plays during the transient process. Recently, direct evidence was found for the pinch-off of CMEs, both from optical observations and from in situ measurements of isolated magnetic clouds' following transient shock waves. However, the detailed sequence of events during the generation of a CME is still unclear.Interplanetary shock waves associated with the CMEs are usually restricted in latitudinal extent to about the angular width of the optically observed CMEs. They may be somewhat less restricted in longitudinal extent. A nearly 1 1 association between CMEs and shock waves measured in situ from spacecraft (Helios 1 and 2, IMP 7 and 8, ISEE 3, Pioneer Venus) can be established, provided the CME and the spacecraft were in the same longitudinal and latitudinal range and the CME speed exceeds 400 km s^–1. Around the past solar activity minimum all CMEs observed were centered at solar latitudes of less than 60°. Around solar maximum, a significant fraction of CMEs also originated from the polar regions. Thus, there is a good chance that the Ulysses spaceprobe will encounter many shocks caused by both low- and high-latitude CMEs, when it finally starts its journey over the Sun's poles.     

Numerical study of compression corner flowfield using Gao-Yong turbulence model

A numerical simulation of shock wave turbulent boundary layer interaction induced by a 24° compression corner based on Gao-Yong compressible turbulence model was presented.The convection terms and the diffusion terms were calculated using the second-order AUSM (advection upstream splitting method) scheme and the second-order central difference scheme,respectively.The Runge-Kutta time marching method was employed to solve the governing equations for steady state solutions.Significant flow separation-region which indicates highly non-isotropic turbulence structure has been found in the present work due to intensity interaction under the 24° compression corner.Comparisons between the calculated results and experimental data have been carried out,including surface pressure distribution,boundary-layer static pressure profiles and mean velocity profiles.The numerical results agree well with the experimental values,which indicate Gao-Yong compressible turbulence model is suitable for the prediction of shock wave turbulent boundary layer interaction in two-dimensional compression corner flows.