共查询到20条相似文献，搜索用时 481 毫秒
1.
低纬Pc3脉动空间传播特性的研究 总被引：2，自引：1，他引：1
本文分析了从地球弓激波前的低纬磁流体波到低纬地面台站观测到Ｐｃ３脉动的整个传播过程,总结了国内外对低纬Ｐｃ３脉动传播特性在观测和理论上的主要研究成果,并对今后研究提出一些看法。 相似文献
2.
太阳风—磁层耦合过程会产生各种等离子体波,其中超低频波的频率最低(1 mHz～1 Hz)、波长最长(与内磁层磁力线长度相当)、能量密度最大.超低频波在磁层粒子加速、物质输运和能量转化中起着重要作用.以往的研究主要关注超低频波的全球性传播和分布特征以及这些波动与磁层能量粒子(辐射带电子和环电流离子)的相互作用过程.最近几... 相似文献
3.
太阳风的动量涨落将通过磁层边界在磁尾激发磁流体力学波。快磁声波携带扰动能量传到等离子体片中,发展为激波,或者通过激波的相互作用而耗散能量,使等离子体加热。等离子体片中的随机费米加速机制,使麦克斯韦分布尾巴部分的高能量粒子被加速到更高能。在宁静态时,加热、加速与耗散过程平衡。当太阳风的动量或者其涨落较大时,整个加热和加速过程加剧,更多的高能粒子产生,并从等离子体片中逃逸,形成高速的等离子体流注入近地轨道和极区,表现为磁层亚暴过程。利用这种机制,可以解释地球磁层亚暴的定性特征。 相似文献
4.
《中国科学:地球科学》2016,(7)
地球弓激波是超音速太阳风和地球磁层相互作用的产物,以往由于数据所限,人们发展的模型仅考虑了近地情况,而对于远地弓激波的位型,以及其他因素例如行星际磁场B_y对弓激波位型的影响,人们还不是很清楚.通过统计分析ARTEMIS卫星2011年1月至2015年1月期间的弓激波穿越事件,首先拟合修正了Chao弓激波模型(最常用的弓激波模型之一)中尾部张角a表达式的系数,得到适用于中远地(月球轨道处,地心距离-20R_EX-50R_E)弓激波的模型系数,然后研究了行星际磁场B_y分量对弓激波尾部张角a的影响.结果表明:(1)拟合的模型系数相对于原系数来说,在中远地与观测结果更吻合;(2)弓激波尾部张角a随行星际磁场B_y分量的增大而增大,且正的B_y对张角的影响比B_y为负的情况影响更大.研究结果为进一步建立包含行星际磁场B_y分量的弓激波模型提供了参考. 相似文献
5.
通过对太阳风-磁层-电离层系统的全球MHD模拟,研究地球弓激波相对日地连线的旋转非对称性．模拟限于太阳风速度沿日地连线、地球磁偶极矩和行星际磁场（IMF）与日地连线垂直的简单情况．模拟结果表明,即便对于IMF强度为零的情况,弓激波相对日地连线也不具备旋转对称性质：终端面（晨昏子午面）及其向阳侧的弓激波截线的东西宽度大于南北宽度（约9%~11％）,终端面尾侧的弓激波截线东西宽度小于南北宽度（约8％）．在存在IMF的情况下,弓激波的位形同时受到磁层顶的形状和快磁声波速度各向异性的影响．磁层顶向外扩张并沿IMF方向拉伸,且其扩张和拉伸程度随IMF由北转南而增强．在磁鞘中,垂直于磁场方向的快磁声波速度高于平行方向．因此,磁层顶拉伸方向与快磁声波速度最大方向垂直,它们对弓激波位置的效应恰好相反;弓激波的最终形状取决于何种效应占据主导地位．对于终端面尾侧,快磁声波速度的各向异性起主导作用,弓激波截线沿IMF垂直方向的宽度大于平行方向．对于终端面及其向阳侧,弓激波截线的形状与IMF取向有关：在准北向或晨昏向IMF情况下,弓激波截线沿IMF垂直方向的宽度仍大于平行方向;在准南向IMF情况下,弓激波截线沿IMF垂直方向的宽度小于平行方向的．鉴于弓激波形状同IMF取向之间的密切关系,我们提议以IMF为基准方向,提取弓激波截线的平行半宽度Rb∥和垂直半宽度Rb⊥作为尺度参数．这些尺度参数和通常引入的弓激波截线的东西半宽度yb和南北半宽度zb相比,更为合理地表征了弓激波的几何性质．模拟结果表明,在终端面上,yb/zb和Rb∥/Rb⊥在IMF各向同性取向下的统计平均值均低于1,与观测得到的结论一致. 相似文献
6.
本文首次利用完全相同两颗卫星（CLUSTER C1和C3）的数据对地球激波前兆区太阳风的减速和偏转特性进行了统计研究.结果表明,在激波前兆坐标系中,太阳风减小的速度随观测点到激波的距离DBS增大而减小,随行星际磁场与激波法向夹角θBN增大也减小,在ULF波动区深度DWS小于6Re(Re为地球半径)的范围内最为显著;伴随着太阳风减速的另外一个现象——太阳风的偏转,也存在相似的规律.其最大减速和最大偏转角度分别为10 km/s和3°.太阳风减速和偏转,以及随之变化的太阳风动压,可能会引起地球磁层顶位置和形状发生改变,同时也为激波前兆区弥散（diffuse）离子的起源及加热提供了一种可能的机制. 相似文献
7.
《中国科学:地球科学》2021,(7)
文章提出以月球科研站为平台,配置一台具有宽视场和高分辨观测能力的软X射线成像仪——月基软X射线成像仪(LSXI),以实现对地球磁层的全景成像. LSXI是一种宽视场的软X射线望远镜,可以对太阳风电荷交换过程(SWCX)产生的软X射线进行动态成像,通过软X射线图像获取地球磁层边际与结构特性.地球磁层全景观测对于理解太阳风-磁层相互作用的物理过程至关重要. LSXI将首次通过对弓激波、磁鞘区、磁层顶和极尖区等区域的同时连续观测,监测太阳风作用下的空间天气演化过程. 相似文献
8.
本文采用特征线方法和激波装配法,对磁流体中间激波在行星际空间的演化过程进行数值模拟。主要结论如下:（1） 2→4型中间激波通过向下游发出后向慢压缩波使下游态磁场减幅,通过向上游发出前向快压缩波使上游态磁场增幅,以致2→4型中间激波迅速经导灭激波向慢激波转化;所发出的前向快压缩波经非线性变陡形成快激波。（2）1→3型中间激波首先通过向下游发出前向慢稀疏波而很快变成1→3=4型临界中间激波,并瞬间转变为由前向快激波和前向2→4型中间激波构成的激波系统。其中,2→4型中间激波可在其前导快激波的下游传播较远的距离,有可能为 IAU 附近的飞船观测到,但最终导灭激波转变为慢激波。 相似文献
9.
本文运用磁场的最小方差分析法和磁场-电子密度的相关分析法分析了欧洲空间局Giotto飞船对P／Grigg-Skjellerup（简称G-S）彗星弓激波附近磁场和电子能流的部分观测数据．结果表明彗星附近存在大量的频率靠近新生水族离子回旋频率的波动,它们是由彗星新生水族离子环流激发的低频左旋电磁波．波在近似平行于磁场方向传播,斜传播角小于15°．电子数据和磁场数据相关分析表明即使在离彗星很远的地方仍然存在压缩波． 相似文献
10.
利用全球磁流体模拟的结果,本文研究了行星际磁场B_y对弓激波位型的影响.结果显示:随着行星际磁场B_y绝对值的增大,弓激波的日下点距离、旋转对称张角、南北非对称性以及旋转非对称性均随之增加.其中,B_y对弓激波日下点距离的影响可达5 RE左右.东向B_y和西向B_y对弓激波位型影响具有对称性,东向B_y和西向B_y大小相同时弓激波日下点距离、旋转对称张角以及旋转非对称性参数均相同,而南北非对称性参数大小相同正负相反.行星际磁场B_y占主导时弓激波尾部横截面在南北方向上拉伸,并且拉伸程度随着B_y绝对值的增大而增大,弓激波尾部横截面的拉伸现象与磁声波马赫数密切相关. 相似文献
11.
—?Seismic precursors to space shuttle re-entry shock fronts are detected at TXAR in Southwest Texas when the ground track of the orbiter vehicle passes within ～150–200?km of the observatory. These precursors have been termed “shuttle-quakes” because their seismograms superficially mimic the seismograms of small earthquakes from shallow sources. Analysis of the “shuttle-quake” seismograms, however, reveals one important difference. Unlike ordinary earthquakes, the propagation azimuths and horizontal phase velocities of the individual phases of the “shuttle-quakes” are functionally related. From a theoretical model developed to account for the origin of these precursors it is found that the seismic phases of “shuttle-quakes” are “bow” waves. A “bow” wave originates at the advancing tip of the shock front trace (i.e., intersection of the re-entry shock front with the surface of the earth) when the ground speed of the orbiter vehicle exceeds the horizontal phase velocity of a particular seismic phase. “Bow” waves are shown to differ in two important respects from the ordinary seismic phases. They vanish ahead of the advancing tip of the shock front trace and their propagation azimuths and horizontal phase velocities are functionally related. The ground speed of the orbiter vehicle exceeds the horizontal phase velocities of crustal seismic phase over much of the re-entry flight profile. As a result, P,S, and R g “bow” waves will be seen as precursors to the re-entry shock front at stations located within a few hundred km of its ground track. 相似文献
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13.
The present paper analyses electromagnetic turbulence in the frequency range 0.1-75 Hz, associated with the supercritical quasiperpendicular crossings of the Earth’s bow shock recorded by the Prognoz-8 and -10 satellites. The quasimonochromatic waves are identified in the shock transition region. Their frequencies, lying in the range 2–5 Hz upstream from the shock ramp, shift to a value less than 1 Hz in the downstream region. The amplitudes of these narrow emissions are great enough to provide the primary dissipation in the flow of the solar wind plasma. Electromagnetic oscillations with such properties are likely to be generated during non-linear evolution of the shock front, rather than by the instabilities driven by ion and electron drifts. Emissions with frequencies higher than 5 Hz have much smaller amplitudes and may be driven by lower hybrid-like instabilities. 相似文献
14.
Atsushi Kubokawa 《地球物理与天体物理流体动力学》2013,107(2):119-137
Although the study of topographic effects on the Rossby waves in a stratified ocean has a long history, the wave property over a periodic bottom topography whose lateral scale is comparable to the wavelength is still not clear. The present paper treats this problem in a two-layer ocean with one-dimensional periodic bottom topography by a simple numerical method, in which no restriction on the wavelength and/or the horizontal scale of the topography is required. The dispersion diagram is obtained for a wavenumber range of [?π/L b , π/L b ], where L b is the periodic length of the topography. When the topographic?β?is not negligible compared to the planetary β, the Rossby wave solutions around the wavenumbers which satisfy the resonant condition among the waves and topography disappear and separate into an infinite number of discrete modes. For convenience, each mode is numbered in order of frequency. As topographic height is increased, the high frequency barotropic Rossby wave (mode 1) becomes a topographic mode which can exist even on the f plane, and the highfrequency baroclinic mode (mode 2) becomes a surface intensified mode. Behaviors of low frequency modes are somewhat complicated. When the topographic amplitude is small, the low frequency baroclinic modes tend to be bottom trapped and the low frequency barotropic modes tend to be surface intensified. As topographic amplitude further increases, the relation between the mode number and vertical structure changes. This change can be attributed to the increase of the frequency of the topographic mode with the topographic amplitude. 相似文献
15.
给定地球轨道附近的行星际条件和地球弓激波的几何位形，本文分析向阳侧弓激波强度参数沿激波阵面的分布，以及行星际激波与弓激波的相互作用.对于弓激波阵面相对日地连线轴对称的情形，得到如下结论：（1）弓激波强度参数分布相对由行星际磁场和日地连线构成的基准面对称，各激波强度参数的最大值出现在基准面上.磁压比在垂直激波线一侧较大，而气压比在平行激波点一侧较大，导致总压比相对日地连线大致呈轴对称分布.（2）随着行星际磁场与日地连线夹角的增大，弓激波强度参数的最大值有所减小，且位置朝远离日下点方向偏移；但气压比和总压比的分布基本上不受影响.（3）行星际激波透过弓激波之后，切向磁场比更接近于1，但总磁场跳变幅度增大.（4）透过弓激波之后，行星际准垂直激波的总磁场比更接近于1，准平行激波的总磁场比则反之. 相似文献
16.
In this work we use ion and magnetic field data from the AMPTE-UKS mission to study the characteristics of low frequency (r p) waves observed upstream of the Earths bow shock. We test the application of various plasma-field correlations and magnetic ratios derived from linear Vlasov theory to identify the modes in this region. We evaluate (for a parameter space consistent with the ion foreshock) the Alfvén ratio, the parallel compressibility, the crosshelicity, the noncoplanar ratio, the magnetic compression and the polarization for the two kinetic instabilities that can be generated in the foreshock by the interaction of hot diffuse ions with the solar wind: the left-hand resonant and the right-hand resonant ion beam instabilities. Comparison of these quantities with the observed plasma-field correlations and various magnetic properties of the waves observed during 10 intervals on 30 October 1984, where the waves are associated with diffuse ions, allows us to identify regions with Alfvénic waves and regions where the predominant mode is the right-hand resonant instability. In all the cases the waves are transverse, propagating at angles 33° and are elliptically polarized. Our results suggest that while the observed Alfvén waves are generated locally by hot diffuse ions, the right-handed waves may result from the superposition of waves generated by two different types of beam distribution (i.e. cold beam and diffuse ions). Even when there was good agreement between the values of observed transport ratios and the values given by the theory, some discrepancies were found. This shows that the observed waves are different from the theoretical modes and that mode identification based only on polarization quantities does not give a complete picture of the waves characteristics and can lead to mode identification of waves whose polarization may agree with theoretical predictions even when other properties can diverge from those of the theoretical modes. 相似文献
17.
The origination of various plasma inhomogeneities in the magnetosheath in front of the Earth’s magnetosphere is analyzed within classical magnetohydrodynamics. The effect of directional discontinuities or tangential and rotational discontinuities of the solar wind on plasma is studied. The origination of inhomogeneities of the type of secondary MHD waves in the magnetosheath is shown; the former equalize plasma parameters when restoring the stationary state. The effect of a rotational discontinuity on the bow shock–Earth’s magnetosphere system is of special interest, with distinguishing of plasma inhomogeneities of the plateau type observed in the near-Earth space. 相似文献
18.
The ponderomotive force (PMF) is a ubiquitous nonlinear wave effect arising in plasma physics when applied wave fields or plasma parameters have significant spatial gradients. Some basic properties of the PMF are described as they relate to ULF hydromagnetic waves in the magnetosphere. Examples are given of recent results obtained using both analytical and numerical techniques for waves from the lowest frequencies (determined by the dimensions of the magnetosphere) up to the vicinity of the ion cyclotron frequency. These results include the possibilities that the PMF may transport plasma over large distances in the magnetosphere, and that the PMF may energize magnetospheric ions significantly. In particular the PMF may play a role in transporting and energizing O+ ions from the ionosphere into the body of the magnetosphere. The PMF can also generate nonlinear coupling between the slow magnetosonic mode and the other hydromagnetic modes. This should lead to limitation of density enhancements and, notably in the case of standing Alfvén waves, to spatial harmonic generation, secularly growing frequency shifts, and saturation of driven wave fields. Some implications of these results for the magnetosphere are discussed.Based on an invited review given in IAGA Symposium 3.07, Nonlinear and Kinetic Effects in ULF Waves, at the IUGG XXI General Assembly, Boulder, Colorado, July 2-14, 1995. 相似文献
19.
Geomagnetism and Aeronomy - The change in the properties of the solar wind flow as it crosses the bow shock wave front and moves in the Earth’s magnetosheath are discussed. Solar wind data... 相似文献
20.
L. S. Rakhmanova M. O. Riazantseva N. L. Borodkova O. V. Sapunova G. N. Zastenker 《Geomagnetism and Aeronomy》2017,57(6):664-671
Data from the BMSW spectrometer, which measures the ion flux value and sometimes plasma parameters with a time resolution of 31 ms, allow the study of the parameters of turbulence of the solar wind and magnetosheath plasma on kinetic scales. In this work, the frequency spectra of the ion flux fluctuations before and after recording the interplanetary shock front in the Earth’s magnetosheath are compared based on these data. It is shown that, in contrast to the solar wind, where the exponential decay of the spectrum often occurs after the shock front on the kinetic scales, no such phenomenon is observed in the magnetosheath: the spectrum on these scales can be approximated by a power function in all the cases considered. In half of these cases, the spectrum slope on the kinetic scales does not change during the interplanetary shock propagation. The results indicate a weak impact of interplanetary shock waves on the parameters of the plasma turbulence. In addition, it is shown that an interplanetary shock does not change the level of intermittency of the ion flux in the magnetosheath at both low and high level before the front. 相似文献