2004年4月1日磁通量传输事件特性的研究——通量管内电流密度、粒子运动与管轴方向的对比分析

本文利用Cluster四颗卫星上磁通门磁力计(FGM)的同时观测,采用旋度器方法(Curlometer),计算和分析了2004年4月1日12:24到12:54UT期间Cluster卫星观测的多个磁通量传输事件(FTEs)的特性。结果表明:磁通量管内电流密度较大,可达到约10-7A/m2。应用最小方向微分法(MDD),发现这些FTE事件具有准二维结构,即为圆柱形结构,其通量管轴线方向与管内电流方向及粒子运动方向基本平行。     

两种应变软化介质组成的边坡失稳研究

对一个平面滑动型边坡,考虑滑面介质由两种应变软化介质材料组成,对应变软化介质存在损伤软化与水致软化两种软化方式。用指数分布描述滑带介质的剪应力与应变关系,建立了边坡系统的尖点突变模型。通过分析发现,边坡失稳与刚度比和边坡的几何/力学参数有极大关联性,这里考虑刚度比是含水率的函数,随着含水率的增加,刚度比不断发生变化。在一定条件下,由于含水率的增加和刚度比的增大,导致边坡失稳的危险性增大,这是降雨情况下边坡容易失稳的根本原因。     

事故和灾害预测中的突变模型

简要介绍了事故与灾害的特征、发展过程的形式及产生的主要原因,指出事故和灾害预测中的难点,依据突变论的思想提出了预测事故和灾害的最佳模型——突变模型,并建立了安全决策尖点突变模型、事故与灾害原因分析尖点突变模型和事故与灾害预测分析尖点突变模型,以1998年的洪水灾害为实例,阐述了模型的应用。     

Propagation and source of Pc5 frequency range pulsation at cusp latitude

1　ＩｎｔｒｏｄｕｃｔｉｏｎＴｈｅｐｏｌａｒｒｅｇｉｏｎｉｓａｎｉｍｐｏｒｔａｎｔａｒｅａｆｏｒｅｎｅｒｇｅｔｉｃｃｏｕｐｌｉｎｇｂｅｔｗｅｅｎｓｏｌａｒｗｉｎｄａｎｄｅａｒｔｈ’ｓｍａｇｎｅｔｏｓｐｈｅｒｅ .Ｔｈｅｃｕｓｐｉｓｔｈｅｄｉｒｅｃｔｐａｔｈｆｏｒｓｏｌａｒｗｉｎｄｐｅｎｅｔｒａｔｉｎｇｉｎｔｏｔｈｅｍａｇｎｅｔｏｓｐｈｅｒｅｏｒｅｖｅｎｉｎｔｏｔｈｅｉｏｎｏｓｐｈｅｒｅａｎｄｉｔａｌｓｏｉｓａｃｏｎｖｅｒｇｅｎｔｒｅｇｉｏｎｆｏｒａｌｏｔｏｆｍａｇｎｅｔｏｓｐｈｅｒｉｃｂｏｕｎｄａ…     

The stability of the pristine magnetopause

A MHD theory of combined Kelvin-Helmholtz (KH) and Rayleigh-Taylor (RT) instabilities for a transition layer with two different scale lengths (Δ and δ for the variation of velocity/magnetic fields and density, respectively) is presented. The study is motivated by reports of magnetopauses with no low latitude boundary layer, in which a sharp density drop over a distance δ?Δ is observed (“pristine” magnetopauses (J. Geophys. Res. 101 (1996) 49). The theory ignores compressibility effects and applies to subsonic regions of the dayside magnetopause. The RT effect is included to account for temporary periods of acceleration of the magnetopause, caused by sudden changes of the solar wind dynamic pressure. For small wavelengths λ, such that δ?λ?Δ, a WKB solution shows that the velocity gradient operates, together with magnetic tensions, to attenuate or even stabilize the Rayleigh-Taylor instability within a certain wavelength range. An exact dispersion relation for flute modes, valid for all λ, in the form of a fourth order polynomial for the complex frequency ω, is obtained from a model with a constant velocity gradient, dV/dy within Δ, and with δ→0. Flute modes are possible because of the existence of bands of very small magnetic shear on the dayside magnetopause (J. Geophys. Res. 103 (1998) 6703). The exact solution allows for a study of the change of the action of the velocity gradient with λ from the long-λ range where dV/dy is KH destabilizing to the short-λ range where dV/dy produces a stabilizing effect. Both, the WKB approximation and the well known tangential discontinuity model (Δ→0) are recovered as limiting cases of the exact solution. Properties of the KH and RT instabilities, for different density ratios on either side of the magnetopause, are described. For flute modes, at very small λ the RT instability grows faster and becomes the dominant effect. However, it is shown that the growth rate remains bounded at a finite value as λ→0, when a theory with a finite δ model is considered. To study configurations with finite, arbitrary, δ/Δ ratios, the MHD perturbation equations are solved numerically, using hyperbolic tangent functions for both the density and velocity transitions across the magnetopause. To examine the influence of different δ/Δ ratios on the growth rates of KH and RT, calculations are performed for different δ/Δ, with and without acceleration, and for two different density ratios. It is found that the general features exhibited by the constant dV/dy model, are confirmed by these numerical solutions. The stability of pristine magnetopauses, and the possibility of observing some theoretical predictions during magnetopause crossings in ongoing missions, are discussed.     

Inter-hemispheric comparisons of geospace environment in the polar regions—A proposed cooperative research program between China and Norway

1　ＩｎｔｒｏｄｕｃｔｉｏｎＧｅｏｓｐａｃｅｄｅａｌｓｗｉｔｈｔｈｅＥａｒｔｈ’ｓｍｉｄｄｌｅａｎｄｕｐｐｅｒａｔｍｏｓｐｈｅｒｅ ,ｔｈｅｒｍｏｓｐｈｅｒｅ/ｉｏｎｏ ｓｐｈｅｒｅａｎｄｍａｇｎｅｔｏｓｐｈｅｒｅ .Ｔｈｉｓ“ｇｅｏｓｐａｃｅｅｎｖｉｒｏｎｍｅｎｔ”ｉｓｏｆｇｒｅａｔｓｃｉｅｎｔｉｆｉｃａｎｄｐｒａｃｔｉ ｃａｌｉｎｔｅｒｅｓｔ,ｐａｒｔｉｃｕｌａｒｌｙａｓｉｔｉｓｏｆｔｅｎｓｕｂｊｅｃｔｔｏｄｉｓｔｕｒｂａｎｃｅｓ.Ａｂｌａｓｔｗａｖｅｆｒｏｍｔｈｅｓｕｎｃａｎｃｏｍｐｒｅｓｓｔｈｅｍ…     

磁层顶高纬边界层的瞬时重联过程

用二维可压缩的ＭＨＤ模型模拟研究了北半球背阳面磁层顶区的瞬时重联过程．结果表明，当行星际磁场（ＩＭＦ）具有南向Ｂｚ分量和背太阳向Ｂｘ分量时，ＩＭＦ与地磁场联接，磁层顶向外扩张，在等离子体幔区可形成流体旋涡，磁力线被扭曲，但不易形成磁涡旋；当ＩＭＦ具有北向Ｂｚ分量时，不论Ｂｘ分量是背向太阳或指向太阳，都可发生瞬时重联，而且当ＩＭＦＢｘ分量与地磁场Ｂｘ分量反向时，在等离子体幔区更易形成磁涡旋．这两种情况，在磁层顶边界层区都能产生多层的电流片．     

The shearing instability of ion flow at the high-latitude tail of magnetopause boundary layer

Shearing instability of ion flow in an inhomogeneous plasma background in the magnetopause boundary layer at the high-latitude magnetotail is studied in this paper. By considering tail-aligned currents, we find that the instability excitation strongly depends on the disturbed wavelength. A quasi-critical wave number for instability is obtained. For relatively long perturbations, the instability tends to be excited at the inner edge of the boundary layer. The stable surface waves at the magnetopause and the K-H instability at the inner edge of the boundary layer can exist at the same time. This may contribute to the continuous transfer of momentum toward the magnetosphere.     

Multiple Flux Rope Events at the High-Latitude Magnetopause: Cluster/Rapid Observation on 26 January, 2001

Cluster measurements of the cusp and high latitude magnetopause boundary on 26 January, 2001 confirm that the cusp is a dynamic region full of energetic charged particles and turbulence. An energetic ion layer at high-latitudes beyond and adjacent to the duskside magnetopause exists when the Interplanetary Magnetic Field (IMF) has a southward orientation. Multiple energetic ion flux bursts were observed in the energetic ion layer. Each energetic ion flux burst was closely related to a magnetic flux rope. The axes of the flux ropes lie in the direction pointing duskward/tailward and somewhat upward. An intense axis-aligned current flows inside the ropes, with the current density reaching ∼10⁻⁸ A/m². The main components of the energetic ions are protons, helium and CNO ions, which originate from the magnetosphere, flowing out into the magnetosheath along the axis of the flux ropes. The velocity of the magnetosheath thermal plasma relative to the deHoffman-Teller (DHT) frame is found to be basically along the axis of the flux ropes also, but towards the magnetosphere. These flux ropes seem to be produced somewhere away via magnetic reconnection and move at similar DHT velocities passing over the spacecraft. These observations further confirm that the high-latitude magnetopause boundary region plays an important role in the solar wind-magnetopause coupling.     

Coupling the Solar-Wind/IMF to the Ionosphere Through the High Latitude CUSPS

Magnetic merging is a primary means for coupling energy from the solar wind into the magnetosphere–ionosphere system. The location and nature of the process remain as open questions. By correlating measurements from diverse locations and using large-scale MHD models to put the measurements in context, it is possible to constrain our interpretations of the global and meso-scale dynamics of magnetic merging. Recent evidence demonstrates that merging often occurs at high latitudes in the vicinity of the cusps. The location is in part controlled by the clock angle in the interplanetary magnetic field (IMF) Y–Z plane. In fact, B_Y bifurcates the cusp relative to source regions. The newly opened field lines may couple to the ionosphere at MLT locations of as much as 3 hr away from local noon. On the other side of noon the cusp may be connected to merging sites in the opposite hemisphere. In fact, the small convection cell is generally driven by opposite hemisphere merging. B_X controls the timing of the interaction and merging sites in each hemisphere, which may respond to planar features in the IMF at different times. Correlation times are variable and are controlled by the dynamics of the tilt of the interplanetary electric field phase plane. The orientation of the phase plane may change significantly on time scales of tens of minutes. Merging is temporally variable and may be occurring at multiple sites simultaneously. Accelerated electrons from the merging process excite optical signatures at the foot of the newly opened field lines. All-sky photometer observations of 557.7 nm emissions in the cusp region provide a “television picture” of the merging process and may be used to infer the temporal and spatial variability of merging, tied to variations in the IMF.