气流速度振荡场中幂律液膜不稳定性分析

采用线性稳定性分析研究了处于气流速度振荡场中幂律液膜时间模式的不稳定性。振荡的气流速度导致动量方程为含有时间周期系数的希尔方程，采用Floquet理论进行求解。详细研究了不同振荡幅值和振荡频率下表观雷诺数、幂律指数及无量纲速度因子对各不稳定区间的影响。结果表明：振荡幅值的增加或振荡频率的减小会使液膜不稳定区域的个数增加，且Kelvin-Helmholtz（K-H）不稳定区域的最大增长率、主导波数和截止波数随振荡幅值和振荡频率的增加而增加；表观雷诺数、幂律指数和无量纲速度因子的增加增强了K-H不稳定区域内的不稳定性，使参数不稳定区域内的增长率先减小后增加；振荡幅值的变化不改变最大增长率发生转折时对应的流变参数，而当振荡频率较小时，幂律指数和无量纲速度因子的增加却使最大增长率单调增加。     

Topological and statistical properties of nonlinear force-free fields

We use our semi-analytic solution of the nonlinear force-free field equation to construct three-dimensional magnetic fields that are applicable to the solar corona and study their statistical properties for estimating the degree of braiding exhibited by these fields. We present a new formula for calculating the winding number and compare it with the formula for the crossing number. The comparison is shown for a toy model of two helices and for realistic cases of nonlinear force-free fields; conceptually the formulae are nearly the same but the resulting distributions calculated for a given topology can be different. We also calculate linkages, which are useful topological quantities that are independent measures of the contribution of magnetic braiding to the total free energy and relative helicity of the field. Finally, we derive new analytical bounds for the free energy and relative helicity for the field configurations in terms of the linking number. These bounds will be of utility in estimating the braided energy available for nano-flares or for eruptions.     

Excitation of flare-induced waves in coronal loops and the effects of radiative cooling

EUV imaging observations from several space missions (SOHO/EIT, TRACE, and SDO/AIA) have revealed a presence of propagating intensity disturbances in solar coronal loops. These disturbances are typically interpreted as slow magnetoacoustic waves. However, recent spectroscopic observations with Hinode/EIS of active region loops revealed that the propagating intensity disturbances are associated with intermittent plasma upflows (or jets) at the footpoints which are presumably generated by magnetic reconnection. For this reason, whether these disturbances are waves or periodic flows is still being studied. This study is aimed at understanding the physical properties of observed disturbances by investigating the excitation of waves by hot plasma injections from below and the evolution of flows and wave propagation along the loop. We expand our previous studies based on isothermal 3D MHD models of an active region to a more realistic model that includes full energy equation accounting for the effects of radiative losses. Computations are initialized with an equilibrium state of a model active region using potential (dipole) magnetic field, gravitationally stratified density and temperature obtained from the polytropic equation of state. We model an impulsive injection of hot plasma into the steady plasma outflow along the loops of different temperatures, warm (～1 MK) and hot (～6 MK). The simulations show that hot jets launched at the coronal base excite slow magnetoacoustic waves that propagate to high altitudes along the loops, while the injected hot flows decelerate rapidly with heights. Our results support that propagating disturbances observed in EUV are mainly the wave features. We also find that the effect of radiative cooling on the damping of slow-mode waves in 1–6 MK coronal loops is small, in agreement with the previous conclusion based on 1D MHD models.     

Stability and waves of transonic laboratory and space plasmas

The properties of magnetohydrodynamic waves and instabilities of laboratory and space plasmas are determined by the overall magnetic confinement geometry and by the detailed distributions of the density, pressure, magnetic field, and background velocity of the plasma. Consequently, measurement of the spectrum of MHD waves (MHD spectroscopy) gives direct information on the internal state of the plasma, provided a theoretical model is available to solve the forward as well as the inverse spectral problems. This terminology entails a program, viz. to improve the accuracy of our knowledge of plasmas, both in the laboratory and in space. Here, helioseismology (which could be considered as one of the forms of MHD spectroscopy) may serve as a luminous example. The required study of magnetohydrodynamic waves and instabilities of both laboratory and space plasmas has been conducted for many years starting from the assumption of static equilibrium. Recently, there is a outburst of interest for plasma states where this assumption is violated. In fusion research, this interest is due to the importance of neutral beam heating and pumped divertor action for the extraction of heat and exhaust needed in future tokamak reactors. Both result in rotation of the plasma with speeds that do not permit the assumption of static equilibrium anymore. In astrophysics, observations in the full range of electromagnetic radiation has revealed the primary importance of plasma flows in such diverse situations as coronal flux tubes, stellar winds, rotating accretion disks, and jets emitted from radio galaxies. These flows have speeds which substantially influence the background stationary equilibrium state, if such a state exists at all. Consequently, it is important to study both the stationary states of magnetized plasmas with flow and the waves and instabilities they exhibit. We will present new results along these lines, extending from the discovery of gaps in the continuous spectrum and low-frequency Alfvén waves driven by rotation to the nonlinear flow patterns that occur when the background speed traverses the full range from sub-slow to super-fast. This revised version was published online in August 2006 with corrections to the Cover Date.     

Evolution of magnetic fields and cosmic ray acceleration in supernova remnants

Observations show that the magnetic field in young supernova remnants (SNRs) is significantly stronger than can be expected from the compression of the circumstellar medium (CSM) by a factor of four expected for strong blast waves. Additionally, the polarization is mainly radial, which is also contrary to expectation from compression of the CSM magnetic field. Cosmic rays (CRs) may help to explain these two observed features. They can increase the compression ratio to factors well over those of regular strong shocks by adding a relativistic plasma component to the pressure, and by draining the shock of energy when CRs escape from the region. The higher compression ratio will also allow for the contact discontinuity, which is subject to the Rayleigh–Taylor (R–T) instability, to reach much further out to the forward shock. This could create a preferred radial polarization of the magnetic field. With an Adaptive Mesh Refinement MHD code (AMRVAC), we simulate the evolution of SNRs with three different configurations of the initial CSM magnetic field, and look at two different equations of state in order to look at the possible influence of a CR plasma component. The spectrum of CRs can be simulated using test particles, of which we also show some preliminary results that agree well with available analytical solutions.     

A statistical analysis of low frequency geomagnetic field pulsations at two Antarctic geomagnetic observatories in the polar cap region

The aim of this study is to investigate the characteristics of low frequency (∼0.5–5 mHz) geomagnetic field fluctuations as recorded at two Antarctic stations within the polar cap: the Italian observatory Mario Zucchelli Station (TNB) and the French–Italian observatory Dome C (DMC) in order to investigate the spatial extension and propagation characteristics of the phenomena observed at very high latitude. The stations have approximately the same geographic latitude, but a very different corrected geomagnetic latitude, being DMC close to the geomagnetic pole and TNB closer to the auroral oval.     

太阳风速度的源表面二维结构

以IPS观测数据为基础，在考虑了加速剖面对太阳风源位置和速度大小的影响下，探讨了1984年1745-1755Carrington周太阳风速度在源表面上的二维分布.结果显示：观测和理论结果均显示出此期间北半球太阳风速度明显高于南半球，特别是经度0一30°，300-360°N的高速流均有不同程度的从极区向南侵的现象.低速带与磁中性线有一定程度的类似即均为单峰结构.但理论和观测给出的低速带的峰值位置与磁中性线的峰值位置略有差异，而且磁中性线的报幅大于观测和理论的结果.     

EXPERIMENTAL AND NUMERICAL INVESTIGATIONS OF BOTH FLOW INDUCED CAVITY OSCILLATION AND ITS SUPPRESSION BY ACOUSTIC EXCITATION

ＥＸＰＥＲＩＭＥＮＴＡＬＡＮＤＮＵＭＥＲＩＣＡＬＩＮＶＥＳＴＩＧＡＴＩＯＮＳＯＦＢＯＴＨＦＬＯＷＩＮＤＵＣＥＤＣＡＶＩＴＹＯＳＣＩＬＬＡＴＩＯＮＡＮＤＩＴＳＳＵＰＰＲＥＳＳＩＯＮＢＹＡＣＯＵＳＴＩＣＥＸＣＩＴＡＴＩＯＮＬｕｏＢａｉｈｕａ；ＨｕＺｈａｎ...     

较小尺度磁螺旋线管相互作用的数值研究

在子午面内,偶极子场和六极子场适当叠加得到势磁场,势磁场与太阳风长时间相瓦作用得到特殊的冕流背景结构.在这种背景结构下,两个较小尺度的磁螺旋线管模型能够连续浮入到计算域,在计算域内相互作用,触发了日冕物质抛射(CME).在数值模拟这一过程时,较小尺度的磁螺旋线管模型具有同心圆形磁场结构,模型中心等离子压强与边界压强之比m=2,模型的半径分别取为a=0.07 R.和a=0.1 Rs(Rs为太阳半径).在这两种情况下,得到了两种典型的计算结果.当a=0.07 Rs时,两个磁螺旋线管模型相瓦作用,在7 Rs内融合成一个磁螺旋线管模型,向外传播;当a=0.1 Rs时,两个磁螺旋线管模型相互作用,作为一个整体向外传播,在计算域内没有融合到一起,基本上保持各自的磁场结构.      

适用于超声速流场计算的有限体积紧致算法

结合紧致格式与有限体积法两者的优点,提出了一种基于有限体积的紧致算法.采用特征处理的通量限制方法抑制紧致格式在间断附近的非物理振荡,将该算法应用于航天领域超声速流场的数值模拟.通过计算典型算例,并与其他格式计算结果进行对比,证明了该算法能够无振荡捕捉各种间断,且对波系结构的刻画最为锐利,并能够精细分辨小尺度流场结构,计算结果与精确解最为接近.