High Velocity Outflows in AGNs Observed with Gratings

Several Active Galactic Nuclei (AGNs) have been reported to harbor fast outflows exceeding 10,000 km?s^?1, which are detected mostly in their low-resolution CCD X-ray spectra. Only few, however, were detected with high-resolution grating spectrometers. Most of the grating detected outflows have been observed multiple times. In these cases, the absorption spectrum changes are indicating that variability is common among these high-velocity winds. In this paper we revisit the grating observations of PG?1211+143, and PDS?456, and report preliminary results on 4C?74.26. We discuss the spectral variability of the first two sources and its implications to the outflows.     

涡轮集气腔出流流量分配和温度特性研究

采用模型实验和数值方法,针对特定的涡轮集气腔结构进行了出流特性研究。首先,在实验室条件下,进行全尺寸基准涡轮集气腔的模型实验研究并验证数值模拟方法;其次,在接近发动机真实气-热参数条件下进行系列的数值模拟,分析进出口压比、腔室高度、出流孔孔径和出流孔轴向位置等对出流孔流量分配和温度分布的影响。研究表明,除了集气腔出流流量分配的不均匀性之外,气流与热壁面之间的对流换热也导致明显的出流温度不均匀性;改变出流孔轴向位置距离、增加集气腔腔室高度是在不影响集气腔通流能力下改善出流均匀性的有效技术措施,当出流孔轴向偏置距离或集气腔腔室高度达到一定值后,其对改善出流流量分配均匀性的作用趋于微弱,但对于改善出流温度分布均匀性依然有较好的作用。     

Numerical Simulations of Stellar Winds

We discuss steady-state transonic outflows obtained by direct numerical solution of the hydrodynamic and magnetohydrodynamic equations. We make use of the Versatile Advection Code, a software package for solving systems of (hyperbolic) partial differential equations. We model thermally and magneto-centrifugally driven stellar outflows as generalizations of the well-known Parker and Weber-Davis wind solutions. To obtain steady-state solutions efficiently, we exploit fully implicit time stepping. Wind solutions containing both a 'wind' and a 'dead' zone are presented. We emphasize the boundary conditions imposed at the stellar surface. For axisymmetric wind solutions, we use the knowledge of the flux functions to verify the numerical solutions. This revised version was published online in June 2006 with corrections to the Cover Date.     

Driving mechanisms for the solar wind

In this review, we consider the central physical aspects pertinent to the acceleration of the solar wind. Special importance is placed on the high-speed streams since the properties of these structures seem to strain the various theoretical explanations the most. Heavy emphasis is also given to the observations — particularly as to what constraints they place on the theories. We also discuss certain sporadic events such as spicules, macrospicules, X-ray bright points, and outflows seen in the EUV associated with the explosive events, jets, and coronal bullets which could be of relevance to this problem.Three theoretical concepts pertaining to the solar wind acceleration process are examined — purely thermal acceleration with and without extended heating, acceleration due to Alfvén wave pressure, and diamagnetic acceleration. Emphasis is given to how well these theories meet the constraints imposed by the observations. Diamagnetism is argued to be a powerful ingredient in solar wind theory, both in the light of observed sporatic outflows seen in the chromosphere and transition region and also because of its effectiveness in increasing the flow speed and producing strong acceleration near the Sun in line with coronal hole observations.     

An Overview of Jets and Outflows in Stellar Mass Black Holes

In this article, we will briefly review the current empirical understanding of the relation between accretion state and outflows in accreting stellar mass black holes. The focus will be on the empirical connections between X-ray states and relativistic (‘radio’) jets, although we are now also able to draw accretion disc winds into the picture in a systematic way. We will furthermore consider the latest attempts to measure/order jet power, and to compare it to other (potentially) measurable quantities, most importantly black hole spin.     

几何参数影响改进型压电合成射流驱动器实验

通过实验的方法研究了开孔尺寸与腔体体积对改进型压电合成射流驱动器出口处射流强度的影响,由热线风速仪测得的瞬时速度,得到了各驱动器试件单位周期内最大速度与时均速度的频响曲线,并引入腔体体积与开孔面积的比值作为无量纲参数,使得能够将驱动器几何尺寸参数对其射流的影响统一起来.结果显示:在低 频谐振频率处,单位周期内最大速度值与时均速度值单调下降;而在高频谐振频率处,时均速度单调下降,单位周期内最大速度值存在极值点;驱动器的几何参数主要对高频区的谐振频率有重要影响.      

Ring Currents and Internal Plasma Sources

The discovery of terrestrial O⁺ and other heavy ions in magnetospheric hot plasmas, combined with the association of energetic ionospheric outflows with geomagnetic activity, led to the conclusion that increasing geomagnetic activity is responsible for filling the magnetosphere with ionospheric plasma. Recently it has been discovered that a major source of ionospheric heavy ion plasma outflow is responsive to the earliest impact of coronal mass ejecta upon the dayside ionosphere. Thus a large increase in ionospheric outflows begins promptly during the initial phase of geomagnetic storms, and is already present during the main phase development of such storms. We hypothesize that enhancement of the internal source of plasma actually supports the transition from substorm enhancements of aurora to storm-time ring current development in the inner magnetosphere. Other planets known to have ring current-like plasmas also have substantial internal sources of plasma, notably Jupiter and Saturn. One planet having a small magnetosphere, but very little internal source of plasma, is Mercury. Observations suggest that Mercury has substorms, but are ambiguous with regard to the possibility of magnetic storms of the planet. The Messenger mission to Mercury should provide an interesting test of our hypothesis. Mercury should support at most a modest ring current if its internal plasma source is as small as is currently believed. If substantiated, this hypothesis would support a general conclusion that the magnetospheric inflationary response is a characteristic of magnetospheres with substantial internal plasma sources. We quantitatively define this hypothesis and pose it as a problem in comparative magnetospheres.     

Metal Enrichment Processes

There are many processes that can transport gas from the galaxies to their environment and enrich the environment in this way with metals. These metal enrichment processes have a large influence on the evolution of both the galaxies and their environment. Various processes can contribute to the gas transfer: ram-pressure stripping, galactic winds, AGN outflows, galaxy-galaxy interactions and others. We review their observational evidence, corresponding simulations, their efficiencies, and their time scales as far as they are known to date. It seems that all processes can contribute to the enrichment. There is not a single process that always dominates the enrichment, because the efficiencies of the processes vary strongly with galaxy and environmental properties.     

预旋进气转-静盘腔中的流动和传热数值研究

采用计算流体动力学(CFD)软件CFX5.7对预旋进气旋转盘腔中的流动和传热过程进行了全三维数值模拟.对4种工况进行了计算,计算结果与试验结果吻合较好,验证了所采用方法的计算精度,并分析了旋转雷诺数、无量纲切向速度、预旋比对流场结构、传热的影响.      

THEMIS ESA First Science Results and Performance Issues

Early observations by the THEMIS ESA plasma instrument have revealed new details of the dayside magnetosphere. As an introduction to THEMIS plasma data, this paper presents observations of plasmaspheric plumes, ionospheric ion outflows, field line resonances, structure at the low latitude boundary layer, flux transfer events at the magnetopause, and wave and particle interactions at the bow shock. These observations demonstrate the capabilities of the plasma sensors and the synergy of its measurements with the other THEMIS experiments. In addition, the paper includes discussions of various performance issues with the ESA instrument such as sources of sensor background, measurement limitations, and data formatting problems. These initial results demonstrate successful achievement of all measurement objectives for the plasma instrument.     

有预旋进气转静盘腔中的流动和换热特性数值研究

运用RNG湍流模型对有静盘外缘预旋进气和轴向中心进气、转盘外缘轴向出气和外围屏径向出气的转-静盘腔中流动和传热过程进行了数值研究。在盘腔结构中,静止内隔片和旋转内隔片将盘腔分为内转-静盘腔室和外预旋腔室。由于盘腔流动结构具有周向周期性,取盘腔的1/30作为计算域。研究发现:旋转雷诺数Re_θ、预旋喷嘴进气无量纲流动速度C_w,_p、静盘中心轴向进气的无量纲流动速度C_w,_d和预旋比β_p都不同程度地影响盘腔内流动和换热。预旋和隔片的协同作用可以很好地起到阻止热燃气入侵转-静盘腔和提供低静温冷却气体流入涡轮叶片冷却通道。      

Solar Imprint on ICMEs, Their Magnetic Connectivity, and Heliospheric Evolution

Interplanetary outflows from coronal mass ejections (ICMEs) are structures shaped by their magnetic fields. Sometimes these fields are highly ordered and reflect properties of the solar magnetic field. Field lines emerging in CMEs are presumably connected to the Sun at both ends, but about half lose their connection at one end by the time they are observed in ICMEs. All must eventually lose one connection in order to prevent a build-up of flux in the heliosphere; but since little change is observed between 1 AU and 5 AU, this process may take months to years to complete. As ICMEs propagate out into the heliosphere, they kinematically elongate in angular extent, expand from higher pressure within, distort owing to inhomogeneous solar wind structure, and can compress the ambient solar wind, depending upon their relative speed. Their magnetic fields may reconnect with solar wind fields or those of other ICMEs with which they interact, creating complicated signatures in spacecraft data.     

Presolar Grains in Meteorites and Their Compositions

Small amounts of pre-solar “stardust” grains have survived in the matrices of primitive meteorites and interplanetary dust particles. These grains—formed directly in the outflows of or from the ejecta of stars—include thermally and chemically refractory carbon materials such as diamond, graphite and silicon carbide; as well as refractory oxides and nitrides. Pre-solar silicates, which have only recently been identified, are the most abundant type except for possibly diamond. The detailed study with modern analytical tools, of isotopic signatures in particular, provides highly accurate and detailed information with regard to stellar nucleosynthesis and grain formation in stellar atmospheres. Important stellar sources are Red Giant (RG) and Asymptotic Giant Branch (AGB) stars, with supernova contributions apparently small. The survival of those grains puts constraints on conditions they were exposed to in the interstellar medium and in the early solar system.     

Cosmic Ray Production in Supernovae

We give a brief review of the origin and acceleration of cosmic rays (CRs), emphasizing the production of CRs at different stages of supernova evolution by the first-order Fermi shock acceleration mechanism. We suggest that supernovae with trans-relativistic outflows, despite being rather rare, may accelerate CRs to energies above \(10^{18}\mbox{ eV}\) over the first year of their evolution. Supernovae in young compact clusters of massive stars, and interaction powered superluminous supernovae, may accelerate CRs well above the PeV regime. We discuss the acceleration of the bulk of the galactic CRs in isolated supernova remnants and re-acceleration of escaped CRs by the multiple shocks present in superbubbles produced by associations of OB stars. The effects of magnetic field amplification by CR driven instabilities, as well as superdiffusive CR transport, are discussed for nonthermal radiation produced by nonlinear shocks of all speeds including trans-relativistic ones.     

The Supermassive Black Hole—Galaxy Connection

The observed scaling relations imply that supermassive black holes (SMBH) and their host galaxies evolve together. Near-Eddington winds from the SMBH accretion discs explain many aspects of this connection. The wind Eddington factor \(\dot{m}\) should be in the range ～1–30. A factor \(\dot{m}\sim 1\) give black hole winds with velocities v～0.1c, observable in X-rays, just as seen in the most extreme ultrafast outflows (UFOs). Higher Eddington factors predict slower and less ionized winds, observable in the UV, as in BAL QSOs. In all cases the wind must shock against the host interstellar gas and it is plausible that these shocks should cool efficiently. There is detailed observational evidence for this in some UFOs. The wind sweeps up the interstellar gas into a thin shell and propels it outwards. For SMBH masses below a certain critical (M–σ) value, all these outflows eventually stall and fall back, as the Eddington thrust of the wind is too weak to drive the gas to large radii. But once the SMBH mass reaches the critical M–σ value the global character of the outflow changes completely. The wind shock is no longer efficiently cooled, and the resulting thermal expansion drives the interstellar gas far from the black hole, which is unlikely to grow significantly further. Simple estimates of the maximum stellar bulge mass M _b allowed by self-limited star formation show that the SMBH mass is typically about 10^?3 M _b at this point, in line with observation. The expansion-driven outflow reaches speeds v _out?1200 km?s^?1 and drives rates \(\dot{M}_{\mathrm{out}}\sim 4000~\mathrm {M}_{\odot }\,\mathrm{yr}^{-1}\) in cool (molecular) gas, giving a typical outflow mechanical energy L _mech?0.05L _Edd, where L _Edd is the Eddington luminosity of the central SMBH. This is again in line with observation. These massive outflows may be what makes galaxies become red and dead, and can have several other potentially observable effects. In particular they have the right properties to enrich the intergalactic gas with metals. Our current picture of SMBH-galaxy coevolution is still incomplete, as there is no predictive theory of how the hole accretes gas from its surroundings. Recent progress in understanding how large-scale discs of gas can partially cancel angular momentum and promote dynamical infall offers a possible way forward.     

外物损伤对民用飞机短舱内/外流气动特性的影响

根据民用飞机动力装置/机体适航验证研究需要,结合三维有限元碰撞冲击仿真,进行了外物损伤(FOD)条件下发动机短舱内/外流数值模拟分析,初步获得了外罩变形对短舱气动特性的影响。结果表明:结合三维有限元碰撞冲击仿真进行的民用飞机短舱气动特性数值模拟,可以较好地分析FOD对发动机短舱内/外流气动特性和安全性能的影响;在内流方面,外罩和唇口的变形导致了巡航状态和低速大流量等状态短舱内流品质降低,一定程度上影响了进气道流通能力并进一步降低了发动机效率;在外流方面,外物损伤变形导致的气流分离致使局部唇口的前缘吸力丧失,这使得FOD短舱的阻力系数始终比光滑短舱的大,但是当外罩流动均处于失速状态时,两者的阻力特性差异降低。通过对严重影响短舱气动特性或飞机安全性的FOD进行评估,表明该研究成果可以为短舱结构设计的优化和民用飞机安全性分析提供技术依据与建议。     

Protostellar Winds and Chondritic Meteorites

We discuss the interaction between the magnetosphere of a young star and its surrounding accretion disk. We consider how an X-wind can be driven magnetocentrifugally from the inner edge of the disk where accreting gas is diverted onto stellar field lines either to flow onto the Sun or to be flung outwards with the wind. The X-wind satisfies many observational tests concerning optical jets, Herbig-Haro objects, and molecular outflows. Connections may exist between primitive solar system materials and X-winds. Chondrules and calcium-aluminum-rich inclusions (CAIs) experienced short melting events uncharacteristic of the asteroid belt where meteorites originate. The inner edge of the solar nebula has the shortest orbital timescale available to the system, a few days. Protosolar flares introduce another timescale, tens of minutes to hours. CAIs may form when solids are lifted from shaded portions of the disk close to the Sun and are exposed to its intense light for a day or so before they are flung by the X-wind to much larger distances. Chondrules were melted, perhaps many times, by flares at larger distances from the Sun before being launched and annealed, but not remelted, in the X-wind. Aerodynamic sorting explains the narrow range of sizes with which CAIs and chondrules are found in chondritic meteorites. Flare-generated cosmic-rays may induce spallation reactions that produce some of the short-lived radioactivities associated with primitive solar system rocks. This revised version was published online in June 2006 with corrections to the Cover Date.     

高压涡轮工作叶片内部流场特性试验研究

为研究变工况特性下涡轮叶片内部通道流场特性，选取高压涡轮二级工作叶片内部通道作为研究对象，在5种不同的进口雷诺数（Re）工况下，利用TRPIV（时序PIV）技术对通道内的流场特性进行了试验研究。Re变化为32426～64700，模拟了飞行循环过程中的若干典型工况。在先进加工技术的辅助下，保留了真实叶型约束下的完整内冷三通道带肋结构，捕捉到一些不同于常规截面两通道模型等简化模型中的流动现象，包括：弯头区域不对称主流分离结构和非对称二次涡系。通过数据分析，明确了高、低雷诺数下流动特性的差异。在高Re工况条件下，弯头出口附近的冲击区域增大；对于第一通道内的二次流，在接近弯头位置处，横向速度分量会导致纵向涡对的强度被削弱，高Re工况下拥有更加剧烈的影响，极有可能削弱吸力面的换热强度。