The large-scale structure of the heliospheric current sheet during the Ulysses epoch

Space Science Reviews - Ulysses is traversing the Sun's polar regions for the first time a year or two before solar minimum. If the heliospheric magnetic field behaves as we expect, the...     

Doppler scintillation measurements of the heliospheric current sheet and coronal streamers close to the Sun

Prominent enhancements in Doppler scintillation lasting a fraction of a day (solar source several degrees wide) and overlying the neutral line represent the signature of the heliospheric current sheet and the apparent interplanetary manifestation of coronal streamers near the Sun. This first detection of coronal streamers in radio scintillation measurements provides the link betweenin situ measurements of the spatial wavenumber spectrum of electron density fluctuations beyond 0.3 AU and earlier measurements deduced from radio scintillation and scattering observations inside 0.3 AU. Significant differences between the density spectra of fast streams and slow solar wind associated with the heliospheric current sheet near the Sun reinforce the emerging picture that high- and low-speed flows are organized by the large-scale solar magnetic field, and that while the contrast between solar wind properties of the two flows is highest near the Sun, it undergoes substantial erosion in the ecliptic plane as the solar wind expands.     

Self-organization in a current sheet model

Self-organization is a possible solution to the seemingly contradicting observation of the repeatable and coherent substorm phenomena with underlying complex behavior in the plasma sheet. Self-organization, through spatio-temporal chaos, emerges naturally in a plasma physics model with sporadic dissipation. This revised version was published online in August 2006 with corrections to the Cover Date.     

Motion of the heliospheric termination shock at high heliographic latitude

We expect the mean distance of the heliospheric termination shock to be greater (smaller) at polar latitudes than at equatorial latitudes, depending on whether the mean dynamic pressure of the solar wind is greater or smaller at high latitudes. The heliospheric termination shock is expected to move in response to variation in upstream solar wind conditions, so that at any particular instant the termination shock will resemble a distorted asymmetric balloon with some parts moving inward and others moving outward. If the shock is a gasdynamic or magnetohydrodynamic shock the results of the analysis depend only very weakly on the nature of the upstream disturbance; typical speeds of the disturbed shock are 100 to 200 km/s. In the absence of a significant latitude gradient of the typical magnitude of solar wind disturbances typical motions of the disturbed shock at polar latitudes would be about twice as fast, due to the higher speed of the high-latitude wind. If the dynamics of the termination shock are dominated by acceleration of the aromalous component of the cosmic rays, the motion of the shock in response to a given disturbance is substantially slower than in the gasdynamic case. Conceivably, particle acceleration might be a less important effect at higher latitudes, and we envision the possibility of a termination shock that is dominated by particle acceleration at lower latitudes and is an MHD shock at high latitudes. In this event high latitude solar wind disturbances would produce substantially larger inward and outward motions of the shock in the polar regions.     

Ulysses observations of latitude gradients in the heliospheric magnetic field: Radial component and variances

The radial component of the magnetic field at Ulysses, over latitudes from –10° to –45° and distances from 5.3 to 3.8 AU, compares very well with corresponding measurements being made by IMP-8 in the ecliptic at 1AU. There is little, if any, evidence of a latitude gradient. Variances in the field, normalized to the square of the field magnitude, show little change with latitude in variations in the magnitude but a large increase in the transverse field variations. The latter are shown to be caused by the presence of large amplitude, long period Alfvénic fluctuations. This identification is based on the close relation between the magnetic field and velocity perturbations including the effect of anisotropy in the solar wind pressure. The waves are propagating outward from the Sun, as in the ecliptic, but variance analysis indicates that the direction of propagation is radial rather than field-aligned. A significant long-period component of 10 hours is present.     

Modelling of the magnetic field of magnetospheric ring current as a function of interplanetary medium parameters

The models are examined which are proposed elsewhere for describing the magnetic field dynamics in ring-currentDR during magnetic storms on the basis of the magnetospheric energy balance equation. The equation parameters, the functions of injectionF and decay , are assumed to depend on interplanetary medium parameters (F and during the storm main phase) and on ring-current intensity ( during the recovery phase). The present-day models are shown to be able of describing theDR variations to within a good accuracy (the r.m.s. deviation 5 < < 15 nT, the correlation coefficient 0.85 <r < 1). The models describe a fraction of the geomagnetic field variation during a magnetic storm controlled by the geoeffective characteristic of interplanetary medium and, therefore responds directly to the variation of the latter. The fraction forms the basis of the geomagnetic field variations in low and middle latitudes. The shorter-term variations ofDR are affected by the injections into the inner magnetosphere during substorm intervals.During magnetic storms, the auroral electrojets shift to subauroral latitudes. When determining theAE indices, the data from the auroral-zone stations must be supplemented with the data from subauroral observatories. Otherwise, erratic conclusions may be obtained concerning the character of the relationships ofDR toAE or ofAE to interplanetary medium parameters. Considering this circumstance, the auroral electrojet intensity during the main phase is closely related to the energy flux supplied to the ring current. It is this fact that gives rise simultaneously to the intensification of auroral electrojets and to the large-scale decrease of magnetic field in low latitudes.The longitudinal asymmetry of magnetic field on the Earth's surface is closely associated with the geoeffective parameters of interplanetary medium, thereby making it possible to model-estimate the magnetic field variations during magnetic storms at given observatories. The inclusion of the field asymmetry due to the system of large-scale currents improves significantly the agreement between the predicted and model field variations at subauroral and midlatitude observatories. The first harmonic amplitude of field variation increases with decreasing latitude. This means that the long-period component of theD _st -variation asymmetry is due rather to the ring-current asymmetry, while the shorter-term fluctuations are produced by electrojets. The asymmetry correlates better with theAL indices (westward electrojet) than with theAU indices (eastward electrojet).The total ion energy in the inner magnetosphere during the storm main phase is sufficient for the magnetic field observed on the Earth's surface to be generated. The energy flux to the ring current is 15% of the -energy flux into the magnetosphere.     

Fourier Transform and Ambiguity Function of Piecewise Polynomial Functions

A general systematic procedure is described for computing the Fourier transform and the ambiguity function of waveforms that are piecewise polynomial. The procedure can be implemented by hand or programmed for execution by a digital computer. The main advantage of the technique is that integration is replaced by a finite summation. Examples include the computation of characteristic function, moments, and the ambiguity function of an amplitude modulated linear FM signal.     

金属板料成形性能的试验研究

本文针对4种防锈铝金属板料（LF2M、LF3M，LF6M，LF21M）的成形性能进行研究，通过试验的方法测定出其成形性能指标。     

燃油喷嘴内部流动和油膜破碎的数值模拟

本文采用VOF法对某航空发动机离心式喷嘴主油路的两相流进行模拟,得到了不同流量时喷嘴内部压力分布、速度分布及喷雾半锥角等参数;采用realizable k—ε模型和雷诺应力模型进行了模拟;将实验数据、经验公式和模拟得到的数据进行对比分析,模拟结果比较理想;捕获了喷嘴下游油膜的初级破碎。     

Use of Nonquadratic Regularization in Fourier Imaging

In many Fourier imaging applications, the presence of unaccounted for amplitude or phase errors in the Fourier domain data can lead to a degraded system impulse response and high sidelobes in the image domain. Historically, many methods for data-driven correction of these effects have been proposed, and numerical optimization of nonquadratic, p-norm image quality metrics has recently emerged as a robust solution. This paper presents a tutorial examination of the sources of image sidelobes in Fourier imaging applications, and studies the effectiveness of p-norm regularization algorithms under various experimental conditions. Several observations are made, including comments on robustness to noise and methods for tapered window design and energy-constrained sparse aperture imaging. Image examples are presented as experimental validation.     

Fourier Analysis of Commutated-Capacitor-Type Integrator Output Signal

It is shown that an operational amplifier with four commutated capacitors in the feedback path produces an output signal whose fundamental is equal in magnitude but 180 degrees out of phase with the input. The analysis is carried out by expressing the output signal in a Fourier series.     

板料机械性能指标与压制成形性能间的关系

本文通过一定的试验数据，对板料机械性能指标与压制成形性能间的关系进行了定性的分析。     

钛合金板材翻边成形的有限元数值模拟

在研究薄板冲压成形原理和模型描述的基础上,采用ANSYS有限元方法对钛合金板材翻边成形进行了系统的分析,完成对钛合金板材的室温和高温下的翻边成形过程的模拟,预测板材成形过程中的应变分布,并得出室温和高温下极限翻边系数,预测值与试验值相比较,拟合良好,同时应变分布规律符合试验结果,证明了有限元方法模拟钛合金热成形性的可行性和准确性。     

STARSEM current and future activity

The launch services industry is facing a tremendous evolution caused by the changes brought to the design of the satellites. The launch industry must cope with the ‘smaller, faster, better’ era. This context was the main reason for the creation of the European-Russian joint venture STARSEM, promoting exclusive marketing of SOYUZ launch services.     

快速傅立叶变换的多机并行计算

快速傅立叶变换(FFT)运算速度相比离散傅立叶变换(DFT)提高了1至2个数量级,但当离散信号的有限序列太长时,FFT算法同样也无法满足实时系统的需要.本文提出一种基于共享存储的多处理机计算FFT的并行算法,并给出该算法的性能分析.计算机仿真实验表明,该FFT并行算法有效、高速,适合于实时处理系统.     

片光反射遮挡式超高速亚毫米粒子探测技术

为满足在超高速碰撞靶上开展航天器抗空间碎片防护性能试验,需要准确测量速度3～10km／s,以及更高速度的毫米级或亚毫米级粒子的飞行速度,在可以实现毫米级粒子探测的片光遮挡式粒子探测技术基础上发展了片光反射遮挡式粒子探测技术,通过采用提高粒子直径与激光光束宽度的比值,解决了探测粒子直径小于1mm时探测信号弱不能识别等关键技术,研制了试验装置并开展了验证试验,研究结果表明该技术在0．2～10km／s速度范围内可实现直径为0．1mm量级粒子的有效探测。     

Mechanics analysis of axisymmetric thin-walled part in warm sheet hydroforming

To obtain the influence of fluid pressure and temperature on warm hydroforming of5A06-O aluminum alloy sheet, the unified mechanics equilibrium equations, which take throughthickness normal stress and friction into account, were established in spherical coordinate system.The distribution of through-thickness normal stress in the thickness direction was determined. The relation between through-thickness normal stress and fluid pressure was also analyzed in different regions of cylindrical cup. Based on the method of subtracting one increasing function from another, the constitutive equation of 5A06-O applied to warm hydroforming was established and in a good agreement with uniaxial tensile data. Based on whether the thickness variation was taken into account, two mechanic models were established to do the comparative study. The results for the studied case show that the calculated stress values are pretty close according to the two models and consistent with results of finite element analysis; the thickness distribution in flange computed by the second model conforms to the experimental data. Finally, the influences of fluid pressure on the flange thickness and radial stress were analyzed.     

Role of ionospheric effects and plasma sheet dynamics in the formation of auroral arcs

At the ionospheric level, the substorm onset (expansion phase) is marked by the initial brightening and subsequent breakup of a pre-existing auroral arc. According to the field line resonance (FLR) wave model, the substorm-related auroral arc is caused by the field-aligned current carried by FLRs. The FLRs are standing shear Alfvén wave structures that are excited along the dipole/quasi-dipole lines of the geomagnetic field. The FLRs (that can cause auroral arc) thread from the Earthward edge of the plasma sheet and link the auroral arc to the plasma sheet region of 6–15 R _E. The region is associated with magnetic fluctuations that result from the nonlinear wave-wave interactions of the cross-field current-instability. The instability (excited at the substorm onset) disrupts the cross-tail current which is built up during the growth phase of the substorms and results in magnetic fluctuations. The diversion of the current to polar regions can lead to auroral arc intensification. The current FLR model is based on the amplitude equations that describe the nonlinear space-time evolution of FLRs in the presence of ponderomotive forces exerted by large amplitude FLRs (excited during substorms). The present work will modify the FLR wave model to include the effects arising from magnetic fluctuations that result from current disruption near the plasma sheet (6–15 R _E). The nonlinear evolution of FLRs is coupled with the dynamics of plasma sheet through a momentum exchange term (resulting from magnetic fluctuations due to current disruption) in the generalized Ohm's law. The resulting amplitude equations including the effects arising from magnetic fluctuations can be used to study the structure of the auroral arcs formed during substorms. We have also studied the role of feedback mechanism (in a dipole geometry of the geomagnetic field) in the formation of the discrete auroral arc observed on the nightside magnetosphere. The present nonlinear dispersive model (NDM) is extended to include effects arising from the low energy electrons originating from the plasma sheet boundary layer. These electrons increase the ionospheric conductivity in a localized patch and enhance the field-aligned current through a feedback mechanism. The feedback effects were studied numerically in a dipole geometry using the the NDM. The numerical studies yield the magnitude of the field-aligned current that is large enough to form a discrete auroral arc. Our studies provide theoretical support to the observational work of Newell et al. that the feedback instability plays a major role in the formation of the discrete auroral arcs observed on the nightside magnetosphere.     

基于傅立叶变换和模糊逻辑的APC/PIO探测方法

为了对飞机-驾驶员耦合(APC)或驾驶员诱发振荡(PIO)现象实现在线探测,提出了适于实时计算的滑动窗口傅立叶变换递推算法、相关特征的模糊隶属函数以及基于模糊逻辑的识别模型。各种情况飞行试验数据的计算和分析表明,该方法对探测APC/PIO是有效、可行的。最后提出了进一步研究的若干建议。