Coronal Heating: a Comparison of Ion-cyclotron and Gravity Damping Models

SOHO/UVCS data indicate that minor ions in the corona are heated more than hydrogen, and that coronal heating results in T_⊥ larger than T_‖. Analogous behavior has been known from in situ measurements in solar wind for many years. Here we compare and contrast two mechanisms which have been proposed to account for the above behavior: ion-cyclotron resonance and gravity damping. This revised version was published online in June 2006 with corrections to the Cover Date.     

Acoustic κ-density fluctuation waves in suprathermal κ function fluids

We describe a new wave mode similar to the acoustic wave in which both density and velocity fluctuate. Unlike the acoustic wave in which the underlying distribution is Maxwellian, this new wave mode occurs when the underlying distribution is a suprathermal κ-function and involves fluctuations in the power law index, κ. This wave mode always propagates faster than the acoustic wave with an equivalent effective temperature and becomes the acoustic wave in the Maxwellian limit as κ → ∞.     

分叉尾喷管气动性能实验研究

某涡轴发动机尾喷管由环形转接段和双管急弯收扩段组成，其形状呈“裤衩”形。在模拟涡轮出口旋流的条件下进行了喷管模型内流气动试验，采用双向总压探针测量喷管内大回流区，发现从３３°截面开始的大分离区对喷管性能有重大影响。在给定流量条件下，通过该流量的喷管进出口压比Ｐ＊５／Ｐ６远比无分离的理论值要高。试验证明导流板是减少喷管气流分离、提高扩压比、降低进口总压的有效措施。Ｐ＊５／Ｐ６可降低１．７％左右。     

Progress in the Study of Galaxies: Structures,Collective Phenomena and Methods

The review contains the important achievements in dynamics of the galactic disks. Among them there are I. New structures discovered recently: • giant vortices (including giant anticyclone in the Solar vicinity); • slow bar; • inner oscillating structure within spiral arms similar that of enveloped soliton; • chaotic streamlines in the velocity field of the gaseous disk of a real galaxy. II. New collective phenomina discovered recently: • new overreflection instability initiating ‘mini-spiral’ in the innermost central parsec of Galaxy; • large-scale convection caused by nonlinear interaction of density wave with disk gas; • non-kolmogorovian spectrum of weak turbulence corresponding to the observed one in the • Solar vicinity. III. New methods worked out recently: • reconstruction of full three-dimensional vector field of gas velocity from the observed line-of- • sight velocity field; • observational test for verification of the wave-nature of the spiral arms; • observational test to distinguish two types of vertical motions: warp and z-motions in the • density wave; • derivation of correct system of two-dimensional dynamical equations from the initial three- • dimensional one. This revised version was published online in June 2006 with corrections to the Cover Date.     

旋风式燃气过滤器的冷流实验和内流场模拟

为了考察某导弹系统燃气发生器的旋风式燃气过滤器的除尘特性，对其进行了冷流实验研究，对除尘效率进行了模拟测量，并应用多流体模型的IPSA算法对其内流场进行了三维两相的数值模拟。计算结果与实验结果较符合，计算得到的分离界限粒径为2μm--3μm。     

Propagation of interplanetary shocks into the Earth’s magnetosphere

This paper is devoted to the study of propagation of disturbances caused by interplanetary shocks (IPS) through the Earth’s magnetosphere. Using simultaneous observations of various fast forward shocks by different satellites in the solar wind, magnetosheath and magnetosphere from 1995 till 2002, we traced the interplanetary shocks into the Earth’s magnetosphere, we calculated the velocity of their propagation into the Earth’s magnetosphere and analyzed fronts of the disturbances. From the onset of disturbances at different satellites in the magnetosphere we obtained speed values ranging from 500 to 1300 km/s in the direction along the IP shock normal, that is in a general agreement with results of previous numerical MHD simulations. The paper discusses in detail a sequence of two events on November 9th, 2002. For the two cases we estimated the propagation speed of the IP shock caused disturbance between the dayside and nightside magnetosphere to be 590 km/s and 714–741 km/s, respectively. We partially attributed this increase to higher Alfven speed in the outer magnetosphere due to the compression of the magnetosphere as a consequence of the first event, and partially to the faster and stronger driving interplanetary shock. High-time resolution GOES magnetic field data revealed a complex structure of the compressional wave fronts at the dayside geosynchronous orbit during these events, with initial very steep parts (10 s). We discuss a few possible mechanisms of such steep front formation in the paper.     

磁重联区Alfven波及新生离子的加速

利用二维混合数值模拟研究了有速度驱动、低等离子体β值情况下的磁场重联过程，结果表明磁重联过程可以产生Alfven波，该Alfven波动对重新区中的新生离子作用，使得新生离子经历投掷角散射方程，具有球壳分布特征，部分新生离子得到加速，其获得的最大能量约为4（miVA0^2/2)，此加速过程所需的加速时间在100／Ωi量级，是一个极快的加速机制，加速粒子能谱为双幂律谱。     

大气重力波引起的突发钠层的模拟研究

应用钠原子和中性大气分子的质量连续性方程来模拟突发纳层（SSL），垂直风场采用接近实际大气重力波的正弦行波模式，结果较好地反映了SSL的形成过程。SSL的形成时刻在5－15min之间并可持续到30min之后，形成高度大约在90－100km之间，峰宽为0.5-2km之间，这些都与实际观测SSL的特点相符，同时还进一步地研究了当重力波参数（主要指垂直波长和周期）、风速以及常态钠层半宽度发生变化时SSL的变化趋势。     

Solar wind dependence of the Pc1 wave activity

There are a host of factors influencing the excitation of Pc1 geomagnetic pulsations, which are ULF waves in the frequency range between 0.2 and 5 Hz. We have studied carefully the dependence of the pearl-type Pc1 activity at Sodankylä, Finland (L = 5.1) on the plasma density N in front of the magnetosphere, the bulk velocity V of the solar wind, and the intensity B of the IMF. The result is as follows: high values of N and reduced values of V are favorable to appearance of Pc1, whereas the dependence of Pc1 activity on B is practically absent. We also show that the probability of Pc1 occurrence decreases with the interplanetary electric field, and increases with solar wind impact pressure and with the plasma to magnetic pressure ratio “beta”.     

透平内部非稳态流动试验研究进展

为探究透平内部流场的非稳态特性及其演变特征,通过归纳国内外透平内部流动的试验研究,回顾了轴流透平、向心透平采用的试验方法及取得的研究进展,分析总结了试验方案与研究中存在的问题。目前,轴流式透平与平面叶栅的试验数量较多,试验的压力温度较低;向心式透平试验研究还比较少,并且试验多处于高温高压环境;随着接触式测量设备性能的大幅提升,其目前在透平非稳态试验中得到广泛应用,例如气动探针已经能够满足1×106Hz的高频采集要求;上游尾迹以及叶顶泄漏涡扰动下轴流式透平叶表附面层的转捩机制,以及向心式透平盘腔泄漏流与主流流场的非定常掺混等问题还有待进一步研究。