Signature of coronal holes and streamers in the interplanetary space

The properties of different solar wind streams depend on the large scale structure of the coronal magnetic field. We present average values and distributions of bulk parameters (density, velocity, temperature, mass flux, momentum, and kinetic and thermal energy, ratio of thermal and magnetic pressure, as well as the helium abundance) as observed on board the Prognoz 7 satellite in different types of the solar wind streams. Maximum mass flux is recorded in the streams emanating from the coronal streamers while maximum thermal and kinetic energy fluxes are observed in the streams from the coronal holes. The momentum fluxes are equal in both types of streams. The maximum ratio of thermal and magnetic pressure is observed in heliospheric current sheet. The helium abundance in streams from coronal holes is higher than in streams from streamers, and its dependences on density and mass flux are different in different types of the streams. Also, the dynamics of -particle velocity and temperature relative to protons in streams from coronal holes and streamers is discussed.     

Modeling the coronal magnetic field in a polar hole

The coronal magnetic field in the northern polar coronal hole in 1986 is predicted on the basis of the photospheric magnetic field observations and the horizontal current-current sheet coronal model (Zhao and Hoeksema, 1993). The predicted magnetic field intensity is stronger near the center of the hole than near the edge. The calculated expansion factor for the entire hole does not match the expansion factor of any flux tube in the hole, suggesting that it would not be appropriate to use the expansion factor for entire hole to represent the divergence of the flux tube in analyzing the acceleration and heating of the plasma in coronal holes.     

Modeling coronal streamers and their eruption

Numerical solutions of the time-dependent MHD equations are used to generate ambient coronal streamer structures in a corona characteristic of that near solar minimum. The streamers are then disrupted by slow photospheric shear motion at the base of magnetic field lines within the closed field region, which is currently believed to be responsible for producing at least some CMEs. In contrast to several other simulations of this phenomena, the polytropic index is maintained at a value of 5/3 through the addition of coronal heating. Observations are used as a guide in determining the thermodynamic structure and plasma beta in the ambient corona. For a shear speed of 2.5 km/sec, the streamer configuration evolves slowly for about 65 hours before erupting outward with the formation of a CME. The bright CME leading edge travels outward at a speed of about 240 km/sec, and the sheared field lines follow at a somewhat slower speed. A closed magnetic field region is ejected as the magnetic field lines that were opened by the CME reconnect and reform the streamer.     

Observations of the solar wind from coronal holes

The solar wind emanating from coronal holes (CH) constitutes a quasi-stationary flow whose properties change only slowly with the evolution of the hole itself. Some of the properties of the wind from coronal holes depend on whether the source is a large polar coronal hole or a small near-equatorial hole. The speed of polar CH flows is usually between 700 and 800 km/s, whereas the speed from the small equatorial CH flows is generally lower and can be <400 km/s. At 1 AU, the average particle and energy fluxes from polar CH are 2.5×10⁸ cm^–2 sec^–1 and 2.0 erg cm^–2 s^–1. This particle flux is significantly less than the 4×10⁸ cm^–2 sec^–1 observed in the slow, interstream wind, but the energy fluxes are approximately the same. Both the particle and energy fluxes from small equatorial holes are somewhat smaller than the fluxes from the large polar coronal holes.Many of the properties of the wind from coronal holes can be explained, at least qualitatively, as being the result of the effect of the large flux of outward-propagating Alfvén waves observed in CH flows. The different ion species have roughly equal thermal speeds which are also close to the Alfvén speed. The velocity of heavy ions exceeds the proton velocity by the Alfvén speed, as if the heavy ions were surfing on the waves carried by the proton fluid.The elemental composition of the CH wind is less fractionated, having a smaller enhancement of elements with low first-ionization potentials than the interstream wind, the wind from coronal mass ejections, or solar energetic particles. There is also evidence of fine-structure in the ratio of the gas and magnetic pressures which maps back to a scale size of roughly 1° at the Sun, similar to some of the fine structures in coronal holes such as plumes, macrospicules, and the supergranulation.     

Broadening of Fe X (6374 Å) profiles above the limb in a coronal hole

Profiles of the visible Fe X (6374 Å) coronal emission line as a function of height above the limb were obtained out to 1.16 solar radii in a coronal hole using the NSO/Sacramento Peak Observatory Coronagraph, Universal Spectrograph and a CCD camera. These are the first coronal line profiles obtained as a function of height in a coronal hole from the ground. Analysis of the line widths suggests a large component of nonthermal broadening which increases with height ranging from 40 to 60 km/s, depending upon the assumed temperature or thermal component of the profile.     

The coronal context of transition region explosive events

Transition region explosive events are observed throughout the quiet Sun and represent an interesting local heating phenomenon. The coronal counterparts of these events, if they exist, were not observed in a sounding rocket campaign dedicated to this objective. The coronal instrument complement on the SOHO spacecraft provides an opportunity to extend this search for the coronal counterparts of the transition region explosive events, as well as to explore the correspondence of explosive events with large scale coronal structures, such as with coronal dark lanes.     

Manifestation of magnetic reconnection in coronal streamer current sheets

We investigate the possibility of observing the effects of magnetic reconnection inside a current sheet forming in a coronal streamer in the extended corona. In particular we study the possibility to observe with the UVCS of SOHO the excitation of the tearing instability in the current sheet.     

3D nonlinear wave heating of coronal loops

The heating of solar coronal loops by the resonant absorption or phase-mixing of incident wave energy is investigated in the framework of 3D nonlinear magnetohydrodynamics (MHD) by means of numerical simulations.     

射流式旋涡发生器对涡轮流动分离控制

通过数值计算,研究了稳态小孔射流式旋涡发生器VGJs(Vortex Generator Jets)对低雷诺数涡轮流动分离的控制。通过对VGJs射流孔径、孔间距的几何参数研究,分析了射流对分离流动的控制机理。在此基础上,提出并详细研究了多种不同孔径射流孔组合排列结构对分离流动的控制效果与作用机理。研究结果表明,射流孔组合排列结构,以大孔射流为主,采用小孔小流量射流对大孔射流控制的分离流场进行"弥补"与调节,可实现总压损失进一步降低22%,射流流量减小25%。     

二维超燃冲压发动机磁控进气道的数值模拟

针对飞行马赫数大于设计马赫数的情况,采用二维磁流体动力学方程对磁控进气道进行了数值模拟研究。数值模拟结果表明磁流体装置的电磁作用可以使非设计马赫数下进气道激波满足SOL(shock on lip)条件,并使出口处的流动变得均匀。分析了磁流体作用位置、宽度和深度等关键控制参数对该类进气道性能的影响,计算结果表明,磁流体作用区域越靠近飞行器前缘,而且在纵向越深,则进气道出口处的流动越均匀,但流率会有所下降;若磁流体作用区域较宽,则需较小的磁场就能使非设计马赫数下进气道的激波结构满足SOL条件。     

Effect of inlet rotating swirl on endwall film cooling for two representative hole arrangements

The swirl generator is widely used in lean-burn combustor to guarantee flame stability and reduce NO_x emissions. Thus, the non-uniformities induced by the swirler would affect and damage film-cooling effectiveness on the turbine components, even blow-off coolant coverage, to some certain extent. The arrangement of film-cooling holes was normally designed to be perpendicular to the axial direction and in standard straight row. In this work we experimentally studied the effects of inlet swirl and mass flow ratio on traditional film cooling holes arrangement and a new arrangement pattern whose holes are located along the isobars. Results indicated that the swirl perturbation would damage film coverage. The film-cooling effect of endwall on which the holes are along the isobars, is invariably more promising than that of endwall on which hole arrangement is perpendicular to axial with the same mass flow of coolant, whether the inlet conditions is uniform or not.     

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.     

航空发动机高压旋转涡轮盘腔流动与换热

在同模型实验参数范围内，且数值解和实验解基本吻合的前提下，对发动机原型参数进行数值模拟，求解了旋转系下流体流动与换热微分方程组，通过对气体域和固体域进行共扼计算，并将动量方程与能量方程福合求解。结果表明利用低参数下实验数据支持的数值计算程序对真实参数的模拟是合理的，对于复杂的非线性现象，数值外推法比传统实验外推更加准确。     

三维等离子体MHD气动热环境数值模拟

电磁流动控制技术是一个多学科交叉融合的重要研究方向,在高超声速飞行器气动特性优化、气动热环境减缓、边界层转捩和等离子体分布等流动控制方面显示出广阔的应用前景。考虑高超声速飞行器绕流流场中发生的离解、复合、电离和置换等化学反应,气体分子振动能激发以及化学非平衡效应,耦合电磁场作用并基于低磁雷诺数假设,通过数值模拟求解三维非平衡Navier-Stokes流场控制方程和Maxwell电磁场控制方程,建立磁场与三维等离子体流场耦合数值模拟方法及程序,采用典型算例进行考核。在此基础上,开展不同条件下磁场对再入三维等离子体流场以及气动热环境影响分析。研究表明:建立的高超声速飞行器的等离子体流场与磁场耦合计算方法及程序,其数值模拟结果与文献符合,外加磁场使飞行器头部弓形激波外推,磁场强度越强,激波面外推距离越大;不同磁场强度环境下,流场中温度峰值大小略有变化,变化幅度较小;磁场对绝大部分区域的热流有减缓作用,作用的大小与飞行高度、马赫数以及磁场的配置紧密相关;当前的计算条件下,飞行的高度越高,磁场的作用越明显。     

电导率模拟对高超声速MHD控制影响

高温气体电导率是高超声速电磁流动控制数值模拟最重要的参数之一。针对电导率模拟准确性及其对高超声速磁流体控制影响的问题,考虑高超声速飞行器流场中高温气体热化学非平衡效应,采用三维低磁雷诺数磁流体动力学（MHD）数值模拟方法及程序,结合国内外常见电导率处理方法开展典型状态高超声速MHD控制数值模拟,分析电导率模拟对高超声速磁流体流场分布、气动力/热特性的影响。研究表明：磁控热流减缓效果与电导率呈非线性关系,电导率较大时将出现电导率的磁控热饱和现象,其产生的原因可能与化学反应趋向于平衡态存在一定关系;采用定电导率方法,会人为放大磁场洛仑兹力的磁阻力效果,使阻力系数的预测值偏大;不同电导率模型计算得到的电导率分布差异很大,甚至存在数量级的差别,显著影响了磁流体的控制效果,这与电导率模型的适用范围、参数选取原则存在很大关联;对于含多种离解、电离组分的高温气体流动来说,采用基于多电离组分迁移碰撞的电导率模型（本文模型M8）,计算与试验一致性最好。     

磁控进气道二维性能计算

超燃冲压发动机进气道通常都是针对某一特定的马赫数进行设计的,当飞行马赫数不在设计马赫数时发动机性能急剧降低,磁控进气道的应用很有可能解决这一技术难题.对磁控进气道内的流动情况进行了二维数值模拟.飞行马赫数大于设计马赫数时采用磁控进气道可以调整激波位置使激波回到设计点,并减小燃烧室入口处的马赫数.分析了霍尔效应对磁控进气道性能的影响,结果表明分段电极可以有效减小霍尔效应的不利影响.      

双出口气膜孔冷却效率数值模拟

为了优化气膜冷却结构,通过数值模拟研究了一种新型气膜孔(由两个圆柱孔组成的双出口孔)的气膜冷却特性.利用Fluent软件对Navier-Stokes方程进行求解,湍流模型采用两方程Realizablek-ε模型和增强壁面函数处理.圆柱孔射流的冷却效率计算结果和实验数据吻合较好.双出口孔射流冷却效率计算结果表明,双出口孔射流有效地增加了冷气的径向覆盖范围,在吹风比为0.5时,次孔射流起到了减弱主孔出口对旋涡的作用;在吹风比为1.0和2.0时,次孔射流使主孔出口处的对旋涡消失.最高冷却效率对应的吹风比为1.0.双出口孔射流在提高冷却效率的同时,其加工难度较扩张形孔明显降低.      

High energy cosmic-ray nuclei results on Ulysses: 2. Effects of a recurrent high-speed stream from the southern polar coronal hole

Since June 1992 the Kiel Electron Telescope on board ULYSSES measures 26-day variations of the order of 6% in the fluxes of high energy H and He. In May 1993 ULYSSES entered into the unipolar region of the southern polar coronal hole, but continued to observe similar effects: increases in the MeV proton channels due to acceleration near the shocks of the corotating interaction region and decreases in the intensity of galactic nuclei associated with the same region. Amplitude variations are presented for different magnetic rigidities and the effects are discussed in view of corotating shock development in a 3-dimensional heliospheric structure.     

心形孔气膜冷却特性的数值模拟

为进一步提高航空发动机热端部件的冷却效率,提出了心形气膜冷却孔结构,利用数值模拟分析心形孔的流场特性和冷却特性,并通过与常规圆形孔计算结果的对比,揭示心形气膜孔强化冷却的物理机制.计算结果表明:与圆形孔相比,心形孔能有效抑制反向旋转涡对的生成,冷却气流的贴壁效果得到明显提高,同时心形孔的扩展出口结构使得冷却气流在展向上的分布更为均匀,展向平均气膜冷却效率得到显著提高;在吹风比为0.5~2.0内,心形孔的全局平均冷却效率相对于圆形孔分别提高了70.93%,246.94%,598.9%和879.07%;从热流比分布来看,心形孔在吹风比为1.5下的热流比值最低,表征在吹风比为1.5下心形孔对壁面的保护效果最好.